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<text><span class="style11"> </span><span class="style20">Space View</span><span class="style11"></span><span class="style10"> </span><span class="style11"> </span><span class="style10"> Copyright © 1995 by Pacific HiTech, Inc. </span><span class="style11"> </span><span class="style10"> August 1995</span><span class="style17">Introduction </span><span class="style10">The Macintosh Interface for Space View has been created so that you can easily view the "thumbnail" images on the CD-ROM and the accompanying textual information. The higher resolution images are located in the TIFF, JPEG, GIF and PICT folders and may be viewed and manipulated using graphics programs like Photoshop.Notes: You should have at least 4 MB of free memory and a 13" color monitor. In order for this interface program to run correctly, it must be located in the same folder as "pict_sml", which contains the images. </span><span class="style17">Screens, Buttons and Fields</span><span class="style10">The </span><span class="style18">Space View Menu</span><span class="style10"> screen has 12 icons representing the image categories. Clicking on an icon will take you to the first image in that group. Using the </span><span class="style18">arrow </span><span class="style10"> buttons you can browse the images in that and other groups. The </span><span class="style18">Slide Show </span><span class="style10"> button will cycle through all of the images one at a time. It can be stopped at any time by clicking with the mouse. The </span><span class="style18">Quit</span><span class="style10"> button will, naturally, allow you to quit the program.The </span><span class="style18">title </span><span class="style10"> at the top of each page has the name of the image file, which can be found in the PICT, JPEG, or MPEG folders on the CD. The field</span><span class="style18"> Internet Site</span><span class="style10"> is the place where the particular image was stored. The </span><span class="style18">Description</span><span class="style10"> and </span><span class="style18">Category </span><span class="style10"> fields should be self-explanatory. </span><span class="style17">Searching</span><span class="style10">The HyperCard Find function is available for searching on text in fields. It can be accessed by typing Command-F. Please refer to a HyperCard Manual for details on more advanced searching with this command.</span><span class="style17">Acknowledgements</span><span class="style10">We would like to thank all of the people on the Internet who have given us suggestions and have made this CD-ROM possible. In particular, we'd like to express appreciation to the scientists and laboratories who have produced the images and made them available to the public on the Internet.</span><span class="style17">Pacific HiTech Contact Information</span><span class="style10">Pacific HiTech, Inc3855 South 500 West, Suite MSalt Lake City, Utah 84115USATel. 801-261-1024, 800-765-8369Fax. 801-261-0310Email. orders@pht.com, info@pht.comWWW. http://www.pht.com/</span></text>
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<text><span class="style11"> </span><span class="style20">Space View</span><span class="style11"></span><span class="style10"> </span><span class="style11"> </span><span class="style10"> Copyright © 1995 by Pacific HiTech, Inc. </span><span class="style11"> </span><span class="style10"> August 1995</span><span class="style25">¡¬¡¬±z¡ ∂R¶π CD-ROM.≥o¨Oß⁄≠ñq∞ͪ⁄πq∏£∫Ù∏Ù(internet)¶U≠”Sites ¶¨∂∞¶U∫ÿπœÆ◊©M§Â¶r¿…°A∏¸§J§U®”,±q∑s¬kØ«¶w±∆,ªs¶®¶π•˙∫–≥n≈È.¶π•˙∫–≥n≈ȧ∫ßt¶≥¬sƒ˝¨…≠±,≈˝±z•i•H¬≤≥ʧŒß÷≥t™∫¶s®˙≥o®«πœ§˘,ß⁄≠Ãß∆±Ê¶π•˙∫–≥n≈ÈπÔ±z¶b¨Ï櫪‚∞ϧ◊®‰¶b§”™≈§J™˘§Ë≠±Ø‡¶≥©“¿∞ßU.ß⁄≠Ã≠n∑PøE®∫®«≈˝ß⁄≠Ãß𶮶π CD-ROM ™∫ß@™Ã≠Ã. §◊®‰≠n¡¬¡¬®∫®«±q®∆¶U∫ÿ≠pπ∫¨„®sß‚•L≠öb¨Ïæ«™∫µo≤{∏¸•X®Ï∞ͪ⁄πq∏£∫Ù∏Ù™∫ß@™Ã§Œ§—§Âæ«Æa≠ðD</span><span class="style38">¶≥√ˆß@™Ã</span><span class="style25">µ{¶°≥]≠p°G Koji Ashida, Cliff Millerπœ§˘¶¨∂∞©M§¿√˛°G Neil Daly, Koji Ashida¬Ωƒ∂§H≠˚°G ™Lج¶W(§§§Â) Michiko Bracken</span><span class="style41"> </span><span class="style25">(§È§Â) Gundi Reed (ºw§Â) Petra Hein (™k§Â) Professor Mauricio Mixco (¶ËØZ§˙§Â)</span><span class="style38">√ˆ©Û Pacific HiTech ¡pµ∏∏Í∞T</span><span class="style17"></span><span class="style10">Pacific HiTech, Inc3855 South 500 West, Suite MSalt Lake City, Utah 84115USATel. 801-261-1024, 800-765-8369Fax. 801-261-0310Email. orders@pht.com, info@pht.comWWW. http://www.pht.com/</span></text>
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<text><span class="style11"> </span><span class="style20">Space View</span><span class="style11"></span><span class="style10"> </span><span class="style11"> </span><span class="style10"> Copyright © 1995 by Pacific HiTech, Inc. </span><span class="style11"> </span><span class="style10"> August 1995Wir danken Ihnen für den Kauf dieser CD-ROM. Wir haben verschiedene Bilder undTextdateien vom Internet der ganzen Welt gesammelt und auf dieser Diskette organisiert.Inbegriffen ist ebenso ein Programm, welches die Bilder schnell und einfach zugänglichmacht. Wir hoffen, daß diese Diskette eine gute Einleitung zu der großartigenHerausforderung des WELTALLs ist.Wir möchten gerne den vielen Leuten danken, die diese CD-ROM möglich machten. Einbesonderer Dank geht zu denen, die an den verschiedenen Forschungsprojektengearbeitet haben und die ihre Entdeckungen den Internetstellen zur Verfügung gestellthaben, und natürlich danken wir auch den Astronomen.</span><span class="style17">Anerkennung:</span><span class="style10">Programmierung: Koji Ashida, Cliff MillerDatenvorbereitung: Neil Daly, Koji AshidaÜbersetzung: Gundi Reed (Deutsche) Petra Hein (Französisch) Professor Mauricio Mixco (Spanisch) Michiko Bracken (Japanische) Jeny Lo (Chinesisch)</span><span class="style17">Kontaktinformation für Pacific HiTech:</span><span class="style10">Pacific HiTech, Inc3855 South 500 West, Suite MSalt Lake City, Utah 84115USATel. 801-261-1024, 800-765-8369Fax. 801-261-0310Email. orders@pht.com, info@pht.comWWW. http://www.pht.com/</span></text>
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<text><span class="style11"> </span><span class="style20">Space View</span><span class="style11"></span><span class="style10"> </span><span class="style11"> </span><span class="style10"> Copyright © 1995 by Pacific HiTech, Inc. </span><span class="style11"> </span><span class="style10"> August 1995Merci d'avoir acheté ce CD-ROM. Nous y avons recueilli différentes sortes d'images et detextes venant d'emplacements de l'Internet du monde entier et les avons organisés sur cedisque. Nous y avons également inclu un "interface" qui vous permet un accès facile etrapide à ces images. Nous espérons que ce disque va être pour vous une bonneintroduction à ce grand monde scientifique qu'est l'espace.Nous aimerions remercier les nombreuses personnes qui ont rendu la création de ce CD-ROM possible. Nous souhaiterions remercier tout spécialement les personnes qui onttravaillé sur différents projets de recherche et qui mettent leurs découvertesscientifiques à portées d'emplacements d'Internet et aux astronomes.</span><span class="style17">Générique</span><span class="style10">Mise en Programme : Koji Ashida, Cliff MillerPréparation des données : Neil Daly, Koji AshidaTraducteur: Petra Hein ( Françés ) Professor Mauricio Mixco ( Español ) Jeny Lo ( Chinoán ) Gundi Reed ( Alemán ) Michiko Bracken ( Japonais )</span><span class="style17">Comment nous atteindre</span><span class="style10">Pacific HiTech, Inc3855 South 500 West, Suite MSalt Lake City, Utah 84115USATel. 801-261-1024, 800-765-8369Fax. 801-261-0310Email. orders@pht.com, info@pht.comWWW. http://www.pht.com/</span></text>
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<text><span class="style11"> </span><span class="style20">Space View</span><span class="style11"></span><span class="style10"> </span><span class="style11"> </span><span class="style10"> Copyright © 1995 by Pacific HiTech, Inc. </span><span class="style11"> </span><span class="style10"> August 1995su Disco Compacto del Espacio Se le agradece la adquisición de este Disco Compacto-ROM. Hemos copiado varios tipos de imágenes y de datos de texto transferidos de sitiosde la red Internet de todas partes del mundo y los hemos organizado en estedisco. Hemos introducido además un enlace (interface) que le permite acceso a estasimágenes fácil- y rápidamente. Esperamos que este disco sea una buena introducción ala gran frontera científica del ESPACIO.Nos complacemos en agradecer la colaboración de las muchas personas que hanasistido en la elaboración de este Disco Compacto-ROM. Les agradecemos en formaespecial a aquellas personas que hayan colaborado en varios proyectos de investigacióny que han facilitado sus descubrimientos científicos a sitios de la red Internet, y a losastrónomos.</span><span class="style17">Credits</span><span class="style10">Programming: Koji Ashida, Cliff MillerData Preparation: Neil Daly, Koji AshidaTraducción: Professor Mauricio Mixco (Español) Jeny Lo (Chinoán) Gundi Reed (Alemán) Petra Hein (Françés) Michiko Bracken ( Japonés)</span><span class="style17">Pacific HiTech, Inc</span><span class="style10">Pacific HiTech, Inc3855 South 500 West, Suite MSalt Lake City, Utah 84115USATel. 801-261-1024, 800-765-8369Fax. 801-261-0310Email. orders@pht.com, info@pht.comWWW. http://www.pht.com/</span></text>
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<text>High detail map of eclipse path across the Northeastern U.S. with major cities plotted (Kentucky, Tennessee, North Carolina, South Carolina, West Virginia, Iowa, Illinois,Ohio, Maine, New York, New Hampshire, etc.)</text>
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<text>Carte détaillée de l'orbite d'éclipse à travers le sud-ouest des U.S.A avec les importantes villes marquées.</text>
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<text>Mapa pormenorizado de la ruta del eclipse a través del suroeste de USA indicando las ciudades principales.</text>
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<text>Detaillierte Karte des Eklipsenweges über die nordöstliche U.S., wichtige Städte.</text>
<text>High detail map of eclipse path across the Northeastern U.S. with major cities plotted (Kentucky, Tennessee, North Carolina, South Carolina, West Virginia, Iowa, Illinois,Ohio, Maine, New York, New Hampshire, etc.)</text>
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<text>Carte détaillée de l'orbite d'éclipse à travers le sud-ouest des U.S.A avec les importantes villes marquées.</text>
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<text>Mapa pormenorizado de la ruta del eclipse a través del suroeste de USA indicando las ciudades principales.</text>
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<text>Detaillierte Karte des Eklipsenweges über die nordöstliche U.S., wichtige Städte.</text>
<text>High detail map of eclipse path across the Southwestern U.S. with major cities plotted (Texas, California, Nevada,Colorado, Arizona, New Mexico, Mexico, Oklahoma, Utah,Kansas, Wyoming, Nebraska, Arkansas, Louisiana, and Missouri)</text>
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<text>Carte détaillée de l'orbite d'éclipse à travers le sud-ouest des U.S.A avec les importantes villes marquées.</text>
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<text>Mapa pormenorizado de la ruta del eclipse a través del suroeste de USA indicando las ciudades principales.</text>
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<text>Detaillierte Karte des Eklipsenweges über die südwestlichen U.S., wichtige Städte.</text>
<text>High detail map of eclipse path across the Southwestern U.S. with major cities plotted (Texas, California, Nevada,Colorado, Arizona, New Mexico, Mexico, Oklahoma, Utah,Kansas, Wyoming, Nebraska, Arkansas, Louisiana, and Missouri)</text>
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<text>Carte détaillée de l'orbite d'éclipse à travers le sud-ouest des U.S.A avec les importantes villes marquées.</text>
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<text>Mapa pormenorizado de la ruta del eclipse a través del suroeste de USA indicando las ciudades principales.</text>
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<text>Detaillierte Karte des Eklipsenweges über die südwestlichen U.S., wichtige Städte.</text>
<text>From: Jay_R_Keller@cup.portal.com Organization: The Portal System (TM) ECLIPSE.GIF, part 1 of 4 This is a 1024 x 946 x 256 color scan of a slide I took while on the Eclipse Edge Expedition. The location was Sayulita, Mexico, where the southern edge of the path of totality first touched the mainland of Mexico. This is a short exposure, showing very little corona but a nice view of the prominences. This is a 1024 x 946 x 256 color scan of a slide I took on the Eclipse Edge Expedition, at Sayulita, Mexico (just north of Puerto Vallarta), on July 11, 1991 at 12:07 PM, just about at the end of totality.</text>
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<text>Balayage en couleurs d'une diapositive prise dans l'Eclipse Edge Expedition à Sayulita, Mexico.</text>
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<text>Escanción de colores de la diapositiva tomada en la Expedición Orilla del Eclipse en Sayulita, México.</text>
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<text>Farb-Scan eines Dias, von der Eclipse Edge Expedition in Sayulita, Mexiko.</text>
<text>Ultraviolet image of Jupiter taken by the Wide Field Camera of the Hubble Space Telescope. The image shows Jupiter's atmosphere at a wavelength of 2550 Angstroms after many impacts by fragments of comet Shoemaker-Levy 9. The most recent impactor is fragment R which is below the center of Jupiter (third dark spot from the right). This photo was taken 3:55 EDT on July 21, about 2.5 hours after R's impact. A large dark patch from the impact of fragment H is visible rising on the morning (left) side. Proceding to the right, other dark spots were caused by impacts of fragments Q1, R, D and G (now one large spot), and L, with L covering the largest area of any seen thus far. Small dark spots from B, N, and Q2 are visible with careful inspection of the image. The spots are very dark in the ultraviolet because a large quantity of dust is being deposited high in Jupiter's stratosphere, and the dust abosrbs sunlight. Scientists will be able to track winds in the stratosphere by watching the evolution of these Credit: Hubble Space Telescope Comet Team</text>
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<text>Image ultraviolette de Jupiter montrant l'atmosphère après de nombreuses collisions de comètes.</text>
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<text>Imagen ultravioleta de Júpiter que muestra la atmósfera después de muchos impactos del cometa.</text>
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<text>Ultraviolet-Bild von Jupiters Atmosphäre nach mehreren Kometenaufschlägen.</text>
<text>Image of Jupiter with the Hubble Space Telescope Planetary Camera. Eight impact sites are visible. From left to right are the E/F complex (barely visible on the edge of the planet), the star-shaped H site, the impact sites for tiny N, Q1, small Q2, and R, and on the far right limb the D/G complex. The D/G complex also shows extended haze at the edge of the planet. The features are rapidly evolving on timescales of days. The smallest features in this image are less than 200 kilometers across. This image is a color composite from three filters at 9530, 5550, and 4100 Angstroms. Credit: Hubble Space Telescope Comet Team</text>
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<text>Prise de vues de Jupiter par Hubble Telescope Planetary Camera montrant 8 emplacements de collisions.</text>
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<text>Foto de Júpiter de la Cámara Planetaria del Telescopio Hubble que muestra 8 sitios de impacto.</text>
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<text>Schuß auf Jupiter von Hubble Teleskop-Kamera, mit 8 Aufschlagstellen.</text>
<text>Hubble Space Telescope Views of Comet Fragment G Impact Zone This image shows two views of the impact zone on Jupiter of fragment G of Comet Shoemaker-Levy 9. The image on the left was made in green light with the Planetary Camera channel of the Wide Field Planetary Camera 2 (WFPC2). The image on the right is the same field taken through the WFPC2 methane filter. Data for the images were obtained in the early morning hours of July 18, 1994. The impact site is visible as a complex pattern of circles seen in the lower left of the partial planet image. The small dark feature to the left of the pattern of circles is the impact site of fragment D. The dark, sharp ring at the site of the fragment G impact is 80% of the size of the Earth. Comet Shoemaker-Levy 9 broke up into 21 fragments during a close passage by Jupiter in July of 1992. Fragment G was one of the brightest and likely the largest of the 21 fragments. The remaining fragments will continue to impact Jupiter through July 22, 1994. Scientists estimate that the combined energy from all of the impacts will approach the equivalent of 40 million megatons of TNT. Jupiter was approximately 477 million miles (767 million kilometers) from Earth when the image was taken. Credit: Dr. Heidi Hammel, Massachusetts Institute of Technology, NASA HST.</text>
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<text>Deux vues de la zone à collisions sur Jupiter de fragment G de Comet Shoemaker-Levy 9.</text>
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<text>Dos vistas de la zona de impacto en J├║piter del fragmento G del cometa de Shoemaker-Levy 9.</text>
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<text>2 Ansichten der Aufschlagzone von Fragment G des Shoemaker-Levy 9 auf Jupiter.</text>
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<text>®‚≠”¨yƒ˝ G ∏H§˘¶bºz¨P™∫ Shoemaker-Levey 9 ™∫§Ï¨P§W™∫º≤¿ª¶a∞œ.</text>
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<text>PHOTO RELEASE NO STScI-PRC94-33 FOR RELEASE: July 21, 1994 COLOR HUBBLE IMAGE OF LARGE COMET IMPACT ON JUPITER This image of the giant planet Jupiter, by NASA's Hubble Space Telescope, reveals the impact sites of fragments "D" and "G" from Comet Shoemaker-Levy 9. The large feature was created by the impact of fragment "G" on July 18, 1994 at 3:28 a.m. EDT. It entered Jupiter's atmosphere from the south at a 45-degree angle, and the resulting ejecta appears to have been thrown back along that direction. The smaller feature to the left of the fragment "G" impact site was created on July 17, 1994, at 7:45 a.m. EDT by the impact of fragment "D". This image was taken 1 hour and 45 minutes after fragment "G" impacted the planet. The "G" impact has concentric rings around it, with a central dark spot 1,550 miles (2,500 km) in diameter. This dark spot is surrounded by a thin dark ring 4,660 miles (7,500 km) in diameter. The dark thick outermost ring's inner edge has a diameter of 7,460 miles (12,000 km) -- about the size of the Earth. The picture is a combination of separate images taken thorugh several color filters to create this "true color" rendition of Jupiter's multi- colored clouds. The impact sites are located in Jupiter's southern hemisphere at a latitude of 44 degrees. Credit: H. Hammel, MIT and NASA</text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Vue de l'emplacement à collisions de fragments D et G de Comet Shoemaker-Levy 9.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>View of Impact sites of fragments D and G from Comet Shoemaker-Levy 9.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Die Aufschlagstellen der Fragmente D und G des Kometen Shoemaker-Levy 9.</text>
</content>
<content>
<layer>background</layer>
<id>32</id>
<text>¨yƒ˝±qºz¨P Shoemaker-Levey 9 ™∫ D ∏H§˘©M G ∏H§˘º≤¿ª¶Ï∏m .</text>
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<name>hst_gc2_card</name>
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card_118329.xml
<?xml version="1.0" encoding="utf-8" ?>
<!DOCTYPE card PUBLIC "-//Apple, Inc.//DTD card V 2.0//EN" "" >
<text>PHOTO RELEASE NO STScI-PRC94-33 FOR RELEASE: July 21, 1994 COLOR HUBBLE IMAGE OF LARGE COMET IMPACT ON JUPITER This image of the giant planet Jupiter, by NASA's Hubble Space Telescope, reveals the impact sites of fragments "D" and "G" from Comet Shoemaker-Levy 9. The large feature was created by the impact of fragment "G" on July 18, 1994 at 3:28 a.m. EDT. It entered Jupiter's atmosphere from the south at a 45-degree angle, and the resulting ejecta appears to have been thrown back along that direction. The smaller feature to the left of the fragment "G" impact site was created on July 17, 1994, at 7:45 a.m. EDT by the impact of fragment "D". This image was taken 1 hour and 45 minutes after fragment "G" impacted the planet. The "G" impact has concentric rings around it, with a central dark spot 1,550 miles (2,500 km) in diameter. This dark spot is surrounded by a thin dark ring 4,660 miles (7,500 km) in diameter. The dark thick outermost ring's inner edge has a diameter of 7,460 miles (12,000 km) -- about the size of the Earth. The picture is a combination of separate images taken thorugh several color filters to create this "true color" rendition of Jupiter's multi- colored clouds. The impact sites are located in Jupiter's southern hemisphere at a latitude of 44 degrees. Credit: H. Hammel, MIT and NASA</text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Vue de l'emplacement à collisions de fragments D et G de Comet Shoemaker-Levy 9.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Vista de sitios de impacto en J├║piter de fragmentos D y G del cometa de Shoemaker-Levy 9.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Die Aufschlagstellen der Fragmente D und G des Kometen Shoemaker-Levy 9.</text>
</content>
<content>
<layer>background</layer>
<id>32</id>
<text>¨yƒ˝±qºz¨P Shoemaker-Levey 9 ™∫ D ∏H§˘©M G ∏H§˘º≤¿ª¶Ï∏m .</text>
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card_118144.xml
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<text>Hubble Space Telescope View of Comet Fragment G Impact Zone This image shows the impact zone on Jupiter of fragment G of Comet Shoemaker-Levy 9. The image was made in green light with the Planetary Camera channel of the Wide Field Planetary Camera 2 (WFPC2). Data for the image were obtained in the early morning hours of July 18, 1994. The impact site is visible as a complex pattern of circles seen in the lower left of the partial planet image. The small dark feature to the left of the pattern of circles is the impact site of fragment D. The dark, sharp ring at the site of the fragment G impact is 80% of the size of the Earth. Comet Shoemaker-Levy 9 broke up into 21 fragments during a close passage by Jupiter in July of 1992. Fragment G was one of the brightest and likely the largest of the 21 fragments. Fragments A-H have impacted the planet. Remaining fragments will continue to impact Jupiter through July 22, 1994. Pre-encounter estimates of the energy of the combined impacts are highly uncertain, and range up to that of a million hydrogen bombs (a million megatons of TNT). Jupiter was approximately 477 million miles (767 million kilometers) from Earth when the image was taken. Credit: Dr. Heidi Hammel, Massachusetts Institute of Technology, NASA HST.</text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Vue de la zone à collisions sur Jupiter de fragment G de Comet Shoemaker-Levey 9.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Vista de zona de impacto en J├║piter del fragmento G del cometa de Shoemaker-Levy 9.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Aufschlagzone von Fragment G des Kometen Shoemaker-Levey 9 auf Jupiter.</text>
</content>
<content>
<layer>background</layer>
<id>32</id>
<text>¨yƒ˝ G ∏H§˘¶bºz¨P™∫ Shoemaker-Levey 9 ™∫§Ï¨P§W™∫º≤¿ª¶a∞œ.</text>
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<content>
<layer>background</layer>
<id>45</id>
<text>Jupiter</text>
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<name>hst_g555_card</name>
<script></script>
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card_117549.xml
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<!DOCTYPE card PUBLIC "-//Apple, Inc.//DTD card V 2.0//EN" "" >
<text> MAGELLAN PROJECT OFFICE P-38811 8/12/91 Two unusual volcanic domes are shown in this Magellan full- resolution mosaicked image. The image covers an area 180 by 240 kilometers (120 by 160 miles) centered at 18.1 degrees north latitude, 303.52 degrees east longitude, just east of Beta Regio. The dome in the south center of the image is about 45 kilometers (30 miles) across, with a 20 kilometer (13 mile) caldera, or volcanic collapse crater, in the center. The dome in the northwest corner of the image is about 30 kilometers (20 miles) across with a small (5 kilometer or 3 mile) summit crater; the very bright radar return from the western flank of this dome indicates that it has steep slopes. The flanks of these volcanoes display prominent gullies which may have been formed by slumping of surface material or thermal erosion by lava flows. Variation in the brightness within the surrounding plains show the extent of lava flows which originated at these volcanoes. Arcuate fractures surrounding the southern edifice indicate that there has been subsidence (down-warping) of the dome following eruptive activity. Jet Propulsion Laboratory California Institute of Technology National Aeronautics and Space Administration Pasadena, Calif. 91109 </text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Deux dômes volcaniques inhabituels sont montrés dans cette mosaïque Magellan à pleine résolution.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>En este mosaico de plena-resolución tomado desde Magallanes se ven dos bóvedas volcánicas poco comunes.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>2 ungew├╢hnliche Vulane sind in diesem detailliertem Magellan-Mosaik dargestellt.</text>
<text> MAGELLAN PROJECT OFFICE P-38811 8/12/91 Two unusual volcanic domes are shown in this Magellan full- resolution mosaicked image. The image covers an area 180 by 240 kilometers (120 by 160 miles) centered at 18.1 degrees north latitude, 303.52 degrees east longitude, just east of Beta Regio. The dome in the south center of the image is about 45 kilometers (30 miles) across, with a 20 kilometer (13 mile) caldera, or volcanic collapse crater, in the center. The dome in the northwest corner of the image is about 30 kilometers (20 miles) across with a small (5 kilometer or 3 mile) summit crater; the very bright radar return from the western flank of this dome indicates that it has steep slopes. The flanks of these volcanoes display prominent gullies which may have been formed by slumping of surface material or thermal erosion by lava flows. Variation in the brightness within the surrounding plains show the extent of lava flows which originated at these volcanoes. Arcuate fractures surrounding the southern edifice indicate that there has been subsidence (down-warping) of the dome following eruptive activity. Jet Propulsion Laboratory California Institute of Technology National Aeronautics and Space Administration Pasadena, Calif. 91109 </text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Deux dômes volcaniques inhabituels sont montrés dans cette mosaïque Magellan à pleine résolution.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>En este mosaico de plena-resolución tomado desde Magallanes se ven dos bóvedas volcánicas poco comunes.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>2 ungew├╢hnliche Vulane sind in diesem detailliertem Magellan-Mosaik dargestellt.</text>
<text> MAGELLAN PROJECT OFFICE P-38811 8/12/91 Two unusual volcanic domes are shown in this Magellan full- resolution mosaicked image. The image covers an area 180 by 240 kilometers (120 by 160 miles) centered at 18.1 degrees north latitude, 303.52 degrees east longitude, just east of Beta Regio. The dome in the south center of the image is about 45 kilometers (30 miles) across, with a 20 kilometer (13 mile) caldera, or volcanic collapse crater, in the center. The dome in the northwest corner of the image is about 30 kilometers (20 miles) across with a small (5 kilometer or 3 mile) summit crater; the very bright radar return from the western flank of this dome indicates that it has steep slopes. The flanks of these volcanoes display prominent gullies which may have been formed by slumping of surface material or thermal erosion by lava flows. Variation in the brightness within the surrounding plains show the extent of lava flows which originated at these volcanoes. Arcuate fractures surrounding the southern edifice indicate that there has been subsidence (down-warping) of the dome following eruptive activity. Jet Propulsion Laboratory California Institute of Technology National Aeronautics and Space Administration Pasadena, Calif. 91109 </text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Deux dômes volcaniques inhabituels sont montrés dans cette mosaïque Magellan à pleine résolution.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>En este mosaico de plena-resolución tomado desde Magallanes se ven dos bóvedas volcánicas poco comunes.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>2 ungew├╢hnliche Vulane sind in diesem detailliertem Magellan-Mosaik dargestellt.</text>
<text> MAGELLAN PROJECT OFFICE P-38741 8/12/91 This remarkable "half crater" is located in the rift between Rhea and Theia Montes in Beta Regio. Radar illumination is from the left. The as yet unnamed crater is 37 (23 miles) kilometers in diameter and is located at latitude 29.91 degrees north, longitude 282.9 degrees east. It has been cut by many fractures or faults since it was formed by the impact of a large asteroid. The eastern half of the crater has been completely destroyed during the formation of a fault-valley that is up to 20 kilometers (12 miles) wide and apparently quite deep. A north-south profile through the very center of this crater is visible as a result of the downdropping and removal of the eastern half of the crater. This "profile view" gives a third dimension to the crater. Thus it will be beneficial to "illuminate" this area from the opposite side (right-looking) with the Magellan SAR during a later mapping cycle, permitting an even more detailed view of the geologic structure of this feature. Jet Propulsion Laboratory California Institute of Technology National Aeronautics and Space Administration Pasadena, Calif. 91109 </text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Remarquable moitié de cratère dans la fissure entre Rhea et Theia Montes dans Beta Regio.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Notable medio cráter en la hendedura entre Rhea y Theia Montes en Beta Regio.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Halber Krater in der Spalte zwischen Rhea und Theia Montes in Beta Regio.</text>
</content>
<content>
<layer>background</layer>
<id>32</id>
<text>¶b Beta Regio, §∂©Û Rhea ©M Theia Montes §ß∂°≠»±o™`∑N™∫•b§ı§s§f.</text>
</content>
<content>
<layer>background</layer>
<id>45</id>
<text>Marte</text>
</content>
<name>split1_card</name>
<script></script>
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card_111187.xml
<?xml version="1.0" encoding="utf-8" ?>
<!DOCTYPE card PUBLIC "-//Apple, Inc.//DTD card V 2.0//EN" "" >
<text> MAGELLAN PROJECT OFFICE P-38741 8/12/91 This remarkable "half crater" is located in the rift between Rhea and Theia Montes in Beta Regio. Radar illumination is from the left. The as yet unnamed crater is 37 (23 miles) kilometers in diameter and is located at latitude 29.91 degrees north, longitude 282.9 degrees east. It has been cut by many fractures or faults since it was formed by the impact of a large asteroid. The eastern half of the crater has been completely destroyed during the formation of a fault-valley that is up to 20 kilometers (12 miles) wide and apparently quite deep. A north-south profile through the very center of this crater is visible as a result of the downdropping and removal of the eastern half of the crater. This "profile view" gives a third dimension to the crater. Thus it will be beneficial to "illuminate" this area from the opposite side (right-looking) with the Magellan SAR during a later mapping cycle, permitting an even more detailed view of the geologic structure of this feature. Jet Propulsion Laboratory California Institute of Technology National Aeronautics and Space Administration Pasadena, Calif. 91109 </text>
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<content>
<layer>background</layer>
<id>29</id>
<text>Remarquable moitié de cratère dans la fissure entre Rhea et Theia Montes dans Beta Regio.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Notable medio cráter en la hendedura entre Rhea y Theia Montes en Beta Regio.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Halber Krater in der Spalte zwischen Rhea und Theia Montes in Beta Regio.</text>
</content>
<content>
<layer>background</layer>
<id>32</id>
<text>¶b Beta Regio, §∂©Û Rhea ©M Theia Montes §ß∂°≠»±o™`∑N™∫•b§ı§s§f.</text>
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<content>
<layer>background</layer>
<id>45</id>
<text>Marte</text>
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<name>split_card</name>
<script></script>
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card_110881.xml
<?xml version="1.0" encoding="utf-8" ?>
<!DOCTYPE card PUBLIC "-//Apple, Inc.//DTD card V 2.0//EN" "" >
<text>Kilauea: A Terrestrial Analogue The Kilauea volcano, located on the big island of Hawaii, is the premier terrestrial analogue for planetary volcanism. Volcanological studies at Kilauea have helped planetary scientists understand volcanism on the moon, Mars, Venus, and Jupiter's moon, Io. In fact, Kilauea, the world's most active volcano, is central to understanding volcanism on Earth. The ultimate goal of these 1995 Kilauea tests is to send sophisticated robotic rovers to the moon and Mars to study volcanic deposits there to gain a better understanding of how volcanic processes operate on Earth, including at Kilauea. The chosen traverse sites allow examination of lava flows, volcanic ash deposits, large fractures along the southwest rift zone and others radial to the summit calders and features formed by water and wind erosion. These feaures are similar to those we will find on other plaetary surfaces. The Rover: A US/Russian Teleoperated Robotic Vehicle The robotic vehicle is based on a six-wheel-drive, Russian-built chassis called Marsokhod, or Mars rover. An international team, including NASA's Ames Research Centeer, McDonnell Douglas and The Planetary Society in cooperation with Russia's Lavochkin Association, VNIITTransMash, and IKI have integrated advanced sensors and computer intelligence with the chassis to make it capable of handling more complex missions. On board the planetary rover is a robotic arm used to pick up surface samples, provide microscopic imaging and, in the future, to deploy scientific instruments. These instruments will support experiments such as determining the chemical composition of soil and rocks, and the mechanical properties of surface materials. The vehicle also uses an array of cameras for scientific imaging, including stereo images for 3D viewing and panoramaic cameras for wide-angle viewing. The fully equipped system is totally wireless. It weights approximately 150 kilograms and is 1.5 meters long, 1 meter wide and 1.7 meters high. Lunar Exploration The simulated lunar test will determine how a science team can use a remotely operated rover to make geological observations. The rover will operate in real time, approximating the round trip travel time for radio waves to the moon which is only 2.5 seconds. The experiment will test the capabilites of the rover and its imaging systems, as well as help increase our understanding of the decision-making process for driving a robotic vehicle on another planet. The traverse will take 3 days and travel over 1 kilometer. The science team, located at NASA's Ames Research Center in California and Johnson Space Center in Texas, will make the geologic observations along the vehicle's course. Their conclusions, drawn for each observation site, will be compared to what can be seen in person, which will be documented by an on-site field geologist during the rover operations. Also, because two different operations centers will be involved, we will be able to demonstrate the ease with which we can hand off control from one location to another. This will allow a future mission to the moon to deadily hand over control of a rover to students, so they can perform scientific lunar experiments from their classrooms on Earth. Mars Exploration Mars presents a more formidable challenge than the moon for performing remote geological observations. This makes this phase of the test a critical one for future missions. The simulated Mars test will apply an intensive operational scenario because the round-trip travel time for data to Mars can vary from 4 to 40 minutes. Theis test will rely on the development of a virtual landscape generated from the rover's stereo cameras to aid the operator in driving the vehicle. This will also allow the Mars scientists located at NASA's Ames Research Center to "fly over" the terrain for overhead observations. Virtual reality can be very helpful because the science team will have only occasional images form the rover, as opposed to real-time video used in the lunar test. It is anticipated that the scientists will investigate over eight science sites in 3 days, traveling over 1 kilometer. As in the lunar test, conclusions drawn for each ovservation site will be compared to what we can see in person.</text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Test Mars simulé du Rover de réalité virtuelle au NASA Ames Center.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Ensayo de realidad virtual en un simulacro de Marte para el R├│ver en el Ames Center de la NASA.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Simulierter Marstest des Rovers durch 'Virutuale Realität' in NASAs Ames Center.</text>
<text>The Planet Mars The full size image of Mars is 207 KB. Last updated February 22, 1995 Constants MEAN RADIUS: 3388.0 km MASS: 0.108 (Earth=1) DENSITY: 3.94 (gm/cm) GRAVITY: 0.380 (Earth=1) ORBIT PERIOD: 686.98 (Earth days) ROTATION PERIOD: 1.026 (Earth days) SEMIMAJOR AXIS OF ORBIT: 1.524 au ECCENTRICITY OF ORBIT: 0.093</text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Image de la planète Mars.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Imagen del planeta Marte.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Bild vom Planeten Mars.</text>
</content>
<content>
<layer>background</layer>
<id>32</id>
<text>§ı¨P™∫πœ§˘.</text>
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<name>mars2_card</name>
<script></script>
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card_109733.xml
<?xml version="1.0" encoding="utf-8" ?>
<!DOCTYPE card PUBLIC "-//Apple, Inc.//DTD card V 2.0//EN" "" >
<text>Kilauea: A Terrestrial Analogue The Kilauea volcano, located on the big island of Hawaii, is the premier terrestrial analogue for planetary volcanism. Volcanological studies at Kilauea have helped planetary scientists understand volcanism on the moon, Mars, Venus, and Jupiter's moon, Io. In fact, Kilauea, the world's most active volcano, is central to understanding volcanism on Earth. The ultimate goal of these 1995 Kilauea tests is to send sophisticated robotic rovers to the moon and Mars to study volcanic deposits there to gain a better understanding of how volcanic processes operate on Earth, including at Kilauea. The chosen traverse sites allow examination of lava flows, volcanic ash deposits, large fractures along the southwest rift zone and others radial to the summit calders and features formed by water and wind erosion. These feaures are similar to those we will find on other plaetary surfaces. The Rover: A US/Russian Teleoperated Robotic Vehicle The robotic vehicle is based on a six-wheel-drive, Russian-built chassis called Marsokhod, or Mars rover. An international team, including NASA's Ames Research Centeer, McDonnell Douglas and The Planetary Society in cooperation with Russia's Lavochkin Association, VNIITTransMash, and IKI have integrated advanced sensors and computer intelligence with the chassis to make it capable of handling more complex missions. On board the planetary rover is a robotic arm used to pick up surface samples, provide microscopic imaging and, in the future, to deploy scientific instruments. These instruments will support experiments such as determining the chemical composition of soil and rocks, and the mechanical properties of surface materials. The vehicle also uses an array of cameras for scientific imaging, including stereo images for 3D viewing and panoramaic cameras for wide-angle viewing. The fully equipped system is totally wireless. It weights approximately 150 kilograms and is 1.5 meters long, 1 meter wide and 1.7 meters high. Lunar Exploration The simulated lunar test will determine how a science team can use a remotely operated rover to make geological observations. The rover will operate in real time, approximating the round trip travel time for radio waves to the moon which is only 2.5 seconds. The experiment will test the capabilites of the rover and its imaging systems, as well as help increase our understanding of the decision-making process for driving a robotic vehicle on another planet. The traverse will take 3 days and travel over 1 kilometer. The science team, located at NASA's Ames Research Center in California and Johnson Space Center in Texas, will make the geologic observations along the vehicle's course. Their conclusions, drawn for each observation site, will be compared to what can be seen in person, which will be documented by an on-site field geologist during the rover operations. Also, because two different operations centers will be involved, we will be able to demonstrate the ease with which we can hand off control from one location to another. This will allow a future mission to the moon to deadily hand over control of a rover to students, so they can perform scientific lunar experiments from their classrooms on Earth. Mars Exploration Mars presents a more formidable challenge than the moon for performing remote geological observations. This makes this phase of the test a critical one for future missions. The simulated Mars test will apply an intensive operational scenario because the round-trip travel time for data to Mars can vary from 4 to 40 minutes. Theis test will rely on the development of a virtual landscape generated from the rover's stereo cameras to aid the operator in driving the vehicle. This will also allow the Mars scientists located at NASA's Ames Research Center to "fly over" the terrain for overhead observations. Virtual reality can be very helpful because the science team will have only occasional images form the rover, as opposed to real-time video used in the lunar test. It is anticipated that the scientists will investigate over eight science sites in 3 days, traveling over 1 kilometer. As in the lunar test, conclusions drawn for each ovservation site will be compared to what we can see in person.</text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Expérience NASA pour trouver comment le Rover fonctionnerait sur la lune ou sur Mars.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Experimento da la NASA para determinar comportamiento del R├│ver en la luna o en Marte.</text>
<text>Kilauea: A Terrestrial Analogue The Kilauea volcano, located on the big island of Hawaii, is the premier terrestrial analogue for planetary volcanism. Volcanological studies at Kilauea have helped planetary scientists understand volcanism on the moon, Mars, Venus, and Jupiter's moon, Io. In fact, Kilauea, the world's most active volcano, is central to understanding volcanism on Earth. The ultimate goal of these 1995 Kilauea tests is to send sophisticated robotic rovers to the moon and Mars to study volcanic deposits there to gain a better understanding of how volcanic processes operate on Earth, including at Kilauea. The chosen traverse sites allow examination of lava flows, volcanic ash deposits, large fractures along the southwest rift zone and others radial to the summit calders and features formed by water and wind erosion. These feaures are similar to those we will find on other plaetary surfaces. The Rover: A US/Russian Teleoperated Robotic Vehicle The robotic vehicle is based on a six-wheel-drive, Russian-built chassis called Marsokhod, or Mars rover. An international team, including NASA's Ames Research Centeer, McDonnell Douglas and The Planetary Society in cooperation with Russia's Lavochkin Association, VNIITTransMash, and IKI have integrated advanced sensors and computer intelligence with the chassis to make it capable of handling more complex missions. On board the planetary rover is a robotic arm used to pick up surface samples, provide microscopic imaging and, in the future, to deploy scientific instruments. These instruments will support experiments such as determining the chemical composition of soil and rocks, and the mechanical properties of surface materials. The vehicle also uses an array of cameras for scientific imaging, including stereo images for 3D viewing and panoramaic cameras for wide-angle viewing. The fully equipped system is totally wireless. It weights approximately 150 kilograms and is 1.5 meters long, 1 meter wide and 1.7 meters high. Lunar Exploration The simulated lunar test will determine how a science team can use a remotely operated rover to make geological observations. The rover will operate in real time, approximating the round trip travel time for radio waves to the moon which is only 2.5 seconds. The experiment will test the capabilites of the rover and its imaging systems, as well as help increase our understanding of the decision-making process for driving a robotic vehicle on another planet. The traverse will take 3 days and travel over 1 kilometer. The science team, located at NASA's Ames Research Center in California and Johnson Space Center in Texas, will make the geologic observations along the vehicle's course. Their conclusions, drawn for each observation site, will be compared to what can be seen in person, which will be documented by an on-site field geologist during the rover operations. Also, because two different operations centers will be involved, we will be able to demonstrate the ease with which we can hand off control from one location to another. This will allow a future mission to the moon to deadily hand over control of a rover to students, so they can perform scientific lunar experiments from their classrooms on Earth. Mars Exploration Mars presents a more formidable challenge than the moon for performing remote geological observations. This makes this phase of the test a critical one for future missions. The simulated Mars test will apply an intensive operational scenario because the round-trip travel time for data to Mars can vary from 4 to 40 minutes. Theis test will rely on the development of a virtual landscape generated from the rover's stereo cameras to aid the operator in driving the vehicle. This will also allow the Mars scientists located at NASA's Ames Research Center to "fly over" the terrain for overhead observations. Virtual reality can be very helpful because the science team will have only occasional images form the rover, as opposed to real-time video used in the lunar test. It is anticipated that the scientists will investigate over eight science sites in 3 days, traveling over 1 kilometer. As in the lunar test, conclusions drawn for each ovservation site will be compared to what we can see in person.</text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Le Rover, un véhicule US/Russe robotique télécommandé pour faire des expériences.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>El Róver, vehículo robótico teleoperado de colaboración USA/Rusia para realizar experimentos científicos.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Der 'Rover,' ein US/ russisches telebefähigtes Roboterfahrzeug für Experimente.</text>
<text>Kilauea: A Terrestrial Analogue The Kilauea volcano, located on the big island of Hawaii, is the premier terrestrial analogue for planetary volcanism. Volcanological studies at Kilauea have helped planetary scientists understand volcanism on the moon, Mars, Venus, and Jupiter's moon, Io. In fact, Kilauea, the world's most active volcano, is central to understanding volcanism on Earth. The ultimate goal of these 1995 Kilauea tests is to send sophisticated robotic rovers to the moon and Mars to study volcanic deposits there to gain a better understanding of how volcanic processes operate on Earth, including at Kilauea. The chosen traverse sites allow examination of lava flows, volcanic ash deposits, large fractures along the southwest rift zone and others radial to the summit calders and features formed by water and wind erosion. These feaures are similar to those we will find on other plaetary surfaces. The Rover: A US/Russian Teleoperated Robotic Vehicle The robotic vehicle is based on a six-wheel-drive, Russian-built chassis called Marsokhod, or Mars rover. An international team, including NASA's Ames Research Centeer, McDonnell Douglas and The Planetary Society in cooperation with Russia's Lavochkin Association, VNIITTransMash, and IKI have integrated advanced sensors and computer intelligence with the chassis to make it capable of handling more complex missions. On board the planetary rover is a robotic arm used to pick up surface samples, provide microscopic imaging and, in the future, to deploy scientific instruments. These instruments will support experiments such as determining the chemical composition of soil and rocks, and the mechanical properties of surface materials. The vehicle also uses an array of cameras for scientific imaging, including stereo images for 3D viewing and panoramaic cameras for wide-angle viewing. The fully equipped system is totally wireless. It weights approximately 150 kilograms and is 1.5 meters long, 1 meter wide and 1.7 meters high. Lunar Exploration The simulated lunar test will determine how a science team can use a remotely operated rover to make geological observations. The rover will operate in real time, approximating the round trip travel time for radio waves to the moon which is only 2.5 seconds. The experiment will test the capabilites of the rover and its imaging systems, as well as help increase our understanding of the decision-making process for driving a robotic vehicle on another planet. The traverse will take 3 days and travel over 1 kilometer. The science team, located at NASA's Ames Research Center in California and Johnson Space Center in Texas, will make the geologic observations along the vehicle's course. Their conclusions, drawn for each observation site, will be compared to what can be seen in person, which will be documented by an on-site field geologist during the rover operations. Also, because two different operations centers will be involved, we will be able to demonstrate the ease with which we can hand off control from one location to another. This will allow a future mission to the moon to deadily hand over control of a rover to students, so they can perform scientific lunar experiments from their classrooms on Earth. Mars Exploration Mars presents a more formidable challenge than the moon for performing remote geological observations. This makes this phase of the test a critical one for future missions. The simulated Mars test will apply an intensive operational scenario because the round-trip travel time for data to Mars can vary from 4 to 40 minutes. Theis test will rely on the development of a virtual landscape generated from the rover's stereo cameras to aid the operator in driving the vehicle. This will also allow the Mars scientists located at NASA's Ames Research Center to "fly over" the terrain for overhead observations. Virtual reality can be very helpful because the science team will have only occasional images form the rover, as opposed to real-time video used in the lunar test. It is anticipated that the scientists will investigate over eight science sites in 3 days, traveling over 1 kilometer. As in the lunar test, conclusions drawn for each ovservation site will be compared to what we can see in person.</text>
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<text>Kilauea, le volcan le plus actif au monde fournit des indications quant aux volcans terrestres.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Kilauea, volcán más activo de la tierra, proporciona evidencia del volcanismo terrestre.</text>
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<id>30</id>
<text>Der aktivste Erden-Vulkan: Kilauea gibt uns Hinweise auf andere Vulkane.</text>
<text>This file is a 640x480 pixel color GIF image of the south polar region of Mars. This is an enlarged detail of the region shown in overview in the image 90S000. The color used is an approximation, rather than "true" color.</text>
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<text>La région polaire sud de Mars. La couleur est approximative et non réele.</text>
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<id>31</id>
<text>Regi├│n del polo sur de Marte. Color aproximado no verdadero.</text>
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<layer>background</layer>
<id>30</id>
<text>Südpol-Region vom Mars. Farben sind ähnlich, nicht genau.</text>
<text>This file is a 640x480 pixel color GIF image of the south polar region of Mars. Part of this area is shown in higher resolution in 90S000-2. The color used is an approximation, rather than "true" color. </text>
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<text>La région polaire sud de Mars. La couleur est approximative et non réele.</text>
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<id>31</id>
<text>Regi├│n del polo sur de Marte. Color aproximado no verdadero.</text>
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<layer>background</layer>
<id>30</id>
<text>Südpol-Region vom Mars. Farben sind ähnlich, nicht genau.</text>
<text>PUBLIC INFORMATION OFFICE JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-39195 Oct. 29, 1991 This full-resolution mosaic centered at 59.1 degrees south latitude, 86.5 degrees east longitude in the Lada Terra Region on Venus is an anaglyph, or combined image, consisting of two data sets slightly displaced from each other and projected in red and blue. This produces a 3-dimensional or stereo effect when viewed through red and blue tinted glasses. Magellan "looked" at the surface from different incidence angles (20 and 14 degrees from a line perpendicular to the surface) as it passed over the same part of the surface in the first and second mapping cycles (November 1990 and July 1991, respectively). The ability to see both the radar image and differences in elevation together is valuable for geologic interpretation. The image is of an area approximately 100 kilometers (62 miles) on a side and shows a deep trough approximately 110 kilometers (68 miles) long, and 8 to 12 kilometers (5 to 7 miles) wide. Analysis of geometric distortions in the two images shows the trough to be about 800 meters (0.5 mile) deep. </text>
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<content>
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<id>29</id>
<text>Mosaïque de la surface de la Région Lada Terra de Vénuse prise par le Magellan.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Mosaico de la superficie de la Regi├│n Lada Terra tomado por Magallanes.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Mosaik auf der Oberfläche der Lada Terra Region auf der Venus; Magellanaufnahme.</text>
</content>
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<layer>background</layer>
<id>32</id>
<text>¶b™˜¨P Lada Terra ¶a∞œ™∫ƒÏ¥O™Ì≠±, Magellan ©“©Áƒ·™∫.</text>
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<text>⌠êØ</text>
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card_104730.xml
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<text>PUBLIC INFORMATION OFFICE JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-39195 Oct. 29, 1991 This full-resolution mosaic centered at 59.1 degrees south latitude, 86.5 degrees east longitude in the Lada Terra Region on Venus is an anaglyph, or combined image, consisting of two data sets slightly displaced from each other and projected in red and blue. This produces a 3-dimensional or stereo effect when viewed through red and blue tinted glasses. Magellan "looked" at the surface from different incidence angles (20 and 14 degrees from a line perpendicular to the surface) as it passed over the same part of the surface in the first and second mapping cycles (November 1990 and July 1991, respectively). The ability to see both the radar image and differences in elevation together is valuable for geologic interpretation. The image is of an area approximately 100 kilometers (62 miles) on a side and shows a deep trough approximately 110 kilometers (68 miles) long, and 8 to 12 kilometers (5 to 7 miles) wide. Analysis of geometric distortions in the two images shows the trough to be about 800 meters (0.5 mile) deep. </text>
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<text>Mosaïque de la surface de la Région Lada Terra de Vénuse prise par le Magellan.</text>
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<content>
<layer>background</layer>
<id>31</id>
<text>Mosaico de la superficie de la Regi├│n Lada Terra tomado por Magallanes.</text>
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<id>30</id>
<text>Mosaik auf der Oberfläche der Lada Terra Region auf der Venus; Magellanaufnahme.</text>
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<id>32</id>
<text>¶b™˜¨P Lada Terra ¶a∞œ™∫ƒÏ¥O™Ì≠±, Magellan ©“©Áƒ·™∫.</text>
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<text>⌠êØ</text>
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card_104635.xml
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<text>This file is a 640x480 pixel color GIF image of a part of Valles Marineris, a large valley on Mars. The detailed structure of the valley's walls looks much like erosion patterns on Earth. Other parts of Valles Marineris are shown in other images. The color used is an approximation, rather than "true" color. </text>
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<id>29</id>
<text>Valles Marineris, une grande vallée sur Mars, avec des sortes d'érosions comme celles de la Terre.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Aparente cauce de erosi├│n en Marte semejante a los terrestres.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Valles Marineris, ein großes Tal auf dem Mars zeigt erdenähnliche Erosionen.</text>
<text>This file is a 640x480 pixel color GIF image of a part of Valles Marineris, a large valley on Mars. The detailed structure of the valley's walls looks much like erosion patterns on Earth. Other parts of Valles Marineris are shown in other images. The color used is an approximation, rather than "true" color. </text>
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<id>29</id>
<text>Valles Marineris, une grande vallée sur Mars, avec des sortes d'érosions comme celles de la Terre.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Aparente cauce de erosi├│n en Marte semejante a los terrestres.</text>
</content>
<content>
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<id>30</id>
<text>Valles Marineris, ein großes Tal auf dem Mars zeigt erdenähnliche Erosionen.</text>
<text>This file is a 640x480 pixel color GIF image of an apparent erosion channel on Mars. The detailed structure of the channel's walls and floor looks much like erosion patterns on Earth. The color used is an approximation, rather than "true" color. </text>
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<layer>background</layer>
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<text>Une érosion apparente d'un canal sur Mars ressemblant au genre d'érosion de la Terre.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Aparente cauce de erosi├│n en Marte semejante a los terrestres.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Wahrscheinlich ein Erosionskanal auf dem Mars, der erdenähnlich aussieht.</text>
<text>This file is a 800x600 pixel color GIF image of the caldera collapse pit at the summit of one of the large volcanos on the Tharsis plateau. An overview of a slightly larger part of the same region is shown in 00n112-2. The color used is an approximation, rather than "true" color.</text>
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<text>Le trou d'effondrement de Caldera au sommet d'un large volcan sur le Tharsis Plateua.</text>
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<content>
<layer>background</layer>
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<text>Fosa de hundimiento tipo caldera en la cima de un gran volcán en el Altiplano de Tharsis.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Caldera Collapse-Pit, auf der Spitze eines großen Vulans auf dem Tharsis Plateau.</text>
<text>This file is a 800x600 pixel color GIF image of the caldera collapse pit at the summit of one of the large volcanos on the Tharsis plateau. An overview of a slightly larger part of the same region is shown in 00n112-2. The color used is an approximation, rather than "true" color.</text>
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<layer>background</layer>
<id>29</id>
<text>Le trou d'effondrement de Caldera au sommet d'un large volcan sur le Tharsis Plateua.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Fosa de hundimiento tipo caldera en la cima de un gran volcán en el Altiplano de Tharsis.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Caldera Collapse-Pit, auf der Spitze eines großen Vulans auf dem Tharsis Plateau.</text>
<text>This file is a 640x480 pixel color GIF image showing an enlargement of part of Valles Marineris, a large valley on Mars. An overview of the area containing this image is shown in 00N107. The detailed structure of the valley looks much like erosion patterns on Earth. Other parts of Valles Marineris are shown in other images. The color used is an approximation, rather than "true" color.</text>
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<content>
<layer>background</layer>
<id>29</id>
<text>Valles Marineris, une grande vallée sur Mars, avec des sortes d'érosions comme celles de la Terre.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Valles Marineris, gran valle en Marte, con patrones de erosi├│n semejante a las terrestres.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Valles Marineris, ein großes Tal auf dem Mars zeigt erdenähnliche Erosionen.</text>
<text>This file is a 640x480 pixel color GIF image showing a large part of Valles Marineris, a large valley on Mars. The detailed structure of the valley looks much like erosion patterns on Earth. An enlargement of part of this image is shown in 00N107-2. Other parts of Valles Marineris are shown in other images. The color used is an approximation, rather than "true" color.</text>
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<layer>background</layer>
<id>29</id>
<text>Valles Marineris, une grande vallée sur Mars, avec des sortes d'érosions comme celles de la Terre.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Valles Marineris, gran valle en Marte, con patrones de erosi├│n semejante a las terrestres.</text>
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<layer>background</layer>
<id>30</id>
<text>Valles Marineris, ein großes Tal auf dem Mars zeigt erdenähnliche Erosionen.</text>
<text>The Planet Mercury The full size image of Mercury is 136 KB. Last updated January 9, 1995 Constants MEAN RADIUS: 2439.7 km MASS: 0.055 (Earth=1) DENSITY: 5.43 (gm/cm) GRAVITY: 0.376 (Earth=1) ORBIT PERIOD: 87.97 (Earth days) ROTATION PERIOD: 58.65 (Earth days) SEMIMAJOR AXIS OF ORBIT: 0.387 au ECCENTRICITY OF ORBIT: 0.206</text>
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<text>Image de la planète Mercure.</text>
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<layer>background</layer>
<id>31</id>
<text>Imagen del planeta Mercurio.</text>
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<id>30</id>
<text>Blick auf den Planeten Merkur.</text>
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<text>§Ù¨Pπœ§˘.</text>
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<text>êÖ êØ</text>
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card_102262.xml
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<text>Kilauea: A Terrestrial Analogue The Kilauea volcano, located on the big island of Hawaii, is the premier terrestrial analogue for planetary volcanism. Volcanological studies at Kilauea have helped planetary scientists understand volcanism on the moon, Mars, Venus, and Jupiter's moon, Io. In fact, Kilauea, the world's most active volcano, is central to understanding volcanism on Earth. The ultimate goal of these 1995 Kilauea tests is to send sophisticated robotic rovers to the moon and Mars to study volcanic deposits there to gain a better understanding of how volcanic processes operate on Earth, including at Kilauea. The chosen traverse sites allow examination of lava flows, volcanic ash deposits, large fractures along the southwest rift zone and others radial to the summit calders and features formed by water and wind erosion. These feaures are similar to those we will find on other plaetary surfaces. The Rover: A US/Russian Teleoperated Robotic Vehicle The robotic vehicle is based on a six-wheel-drive, Russian-built chassis called Marsokhod, or Mars rover. An international team, including NASA's Ames Research Centeer, McDonnell Douglas and The Planetary Society in cooperation with Russia's Lavochkin Association, VNIITTransMash, and IKI have integrated advanced sensors and computer intelligence with the chassis to make it capable of handling more complex missions. On board the planetary rover is a robotic arm used to pick up surface samples, provide microscopic imaging and, in the future, to deploy scientific instruments. These instruments will support experiments such as determining the chemical composition of soil and rocks, and the mechanical properties of surface materials. The vehicle also uses an array of cameras for scientific imaging, including stereo images for 3D viewing and panoramaic cameras for wide-angle viewing. The fully equipped system is totally wireless. It weights approximately 150 kilograms and is 1.5 meters long, 1 meter wide and 1.7 meters high. Lunar Exploration The simulated lunar test will determine how a science team can use a remotely operated rover to make geological observations. The rover will operate in real time, approximating the round trip travel time for radio waves to the moon which is only 2.5 seconds. The experiment will test the capabilites of the rover and its imaging systems, as well as help increase our understanding of the decision-making process for driving a robotic vehicle on another planet. The traverse will take 3 days and travel over 1 kilometer. The science team, located at NASA's Ames Research Center in California and Johnson Space Center in Texas, will make the geologic observations along the vehicle's course. Their conclusions, drawn for each observation site, will be compared to what can be seen in person, which will be documented by an on-site field geologist during the rover operations. Also, because two different operations centers will be involved, we will be able to demonstrate the ease with which we can hand off control from one location to another. This will allow a future mission to the moon to deadily hand over control of a rover to students, so they can perform scientific lunar experiments from their classrooms on Earth. Mars Exploration Mars presents a more formidable challenge than the moon for performing remote geological observations. This makes this phase of the test a critical one for future missions. The simulated Mars test will apply an intensive operational scenario because the round-trip travel time for data to Mars can vary from 4 to 40 minutes. Theis test will rely on the development of a virtual landscape generated from the rover's stereo cameras to aid the operator in driving the vehicle. This will also allow the Mars scientists located at NASA's Ames Research Center to "fly over" the terrain for overhead observations. Virtual reality can be very helpful because the science team will have only occasional images form the rover, as opposed to real-time video used in the lunar test. It is anticipated that the scientists will investigate over eight science sites in 3 days, traveling over 1 kilometer. As in the lunar test, conclusions drawn for each ovservation site will be compared to what we can see in person.</text>
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<text>Kilauea, le volcan le plus actif au monde, fournit des indications quant au volcanisme planétaire.</text>
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<layer>background</layer>
<id>31</id>
<text>Kilauea, volcán más activo de la tierra, proporciona evidencia del volcanismo planetario.</text>
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<id>30</id>
<text>Der aktivste Erden-Vulkan: Kilauea gibt uns Hinweise auf andere Vulkane.</text>
<text>Tycho Crater (346 kb jpeg image) This mosaic of Clementine UVVIS images covers the center of the impact crater Tycho. It was formed when a large meteorite (or comet) slammed into the Moon. The version on the right is a 3 color composite (415 nm, 750 nm, 1000 nm); the version in the center is a color composite of wavelength ratios which show different rock and soil types. Note the distinct color difference of the central peak due to excavation of deep material during the impact that formed the crater. The ratio image on the left enhances an unusual polygonal pattern in the floor of the crater. The origin of this feature is not clear, however future work using all 11 wavelengths collected by the UVVIS and NIR cameras will most likely reveal the origin of these enigmatic "cracks".</text>
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<text>Clementine UVVIS images mosaïques du centre du cratère à collision Tycho.</text>
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<text>Mosaico de imágenes del centro del cráter de impacto tomadas por el Clementine UVVIS.</text>
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<text>Mosaikbilder von Clementine UVVIS auf das Zentrum des Aufschlagskrater Tycho.</text>
<text>Clementine map of the topography of the Moon (449 kb jpeg image) Oblique view of the Moon looking towards the east, with color-coded altimetry on a shaded-relief image. The lowest elevations are shown in purple, increasing to blue, green, and red. 10x vertical exaggeration. Original image was in a Mercator projection from latitude -70 to 70 and with 450 degrees of longitude (repeating region from 90 to 180). The large-scale topography of the Moon is dominated by two giant basins or depressions separated by rugged highlands. The deepest depression is the South Pole/Aitken basin (upper right), and the larger but shallower depression covers most of the central and northern nearside. The nearside basin may be due to a single large impact, several large impacts, or to magma-ocean processes. The highest regions on the Moon occur on the north-central farside, perhaps due to giant-basin ejecta and/or magma ocean processes. Except perhaps for the nearside basin and central farside highlands, all of the large-scale topography of the Moon has been determined by impact events and mare fill. All of the multi-ring impact basins on the Moon are at least 3.9 billion years old. Data processing by NASA Goddard Spaceflight Center and the U.S. Geological Survey.</text>
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<text>Carte Clementine de la topographie de la Lune avec une vue oblique regardant vers l'est.</text>
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<text>Mapa Clementine de la topografía lunar con vista oblícua mirando hacia oriente.</text>
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<text>Clementine-Karte der Mondoberfläche mit einer indirekten Sicht nach Osten.</text>
<text>Star Tracker Earthshine (53 kb jpeg image) In addition to the geologic mapping cameras, the Clementine spacecraft also carried two Star Tracker cameras for navigation. These amazing lightweight (0.3 kg) cameras kept the spacecraft on track by constantly observing the positions of Stars, reminiscent of the age old seafaring tradition of sextant/star navigation. These navigation cameras were also able to take some spectacular wide angle images of the Moon. In this picture the Moon is seen illuminated solely be light reflected from the Earth - Earthshine! the bright glow on the lunar horizon is caused by light from the solar corona, the sun is just behind the lunar limb. The low angle of Earthshine near the limb results in dramatic shadowing which enhances the rings of the Orientale basin - the scar of a massive asteroid (or comet) impact. Also of interest in this image is the planet Venus at the bottom of the frame.</text>
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<text>Image Star Tracker de la Lune illuminée par de la lumière réfléchie par la Terre.</text>
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<text>Retrato de la luna iluminada de la luz terrestre reflejada, tomada desde el Star Tracker (rastreador de estrellas).</text>
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<text>'Star Tracker'-Bild vom Mond, der vom reflektierten Licht der Erde beleuchtet wird.</text>
<text>Earth's Moon The full size image of the Moon is 110 KB. Last updated February 16, 1995 Constants MEAN RADIUS: 1737.4 km MASS: 0.012 (Earth=1) DENSITY: 3.34 (gm/cm) GRAVITY: 0.012 (Earth=1) ORBIT PERIOD: 27.32 (Earth days) ROTATION PERIOD: 27.32 (Earth days) SEMIMAJOR AXIS OF ORBIT: 384,400 km ECCENTRICITY OF ORBIT: 0.055</text>
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<text>Image de la Lune de la Terre.</text>
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<text>Retrato de la luna terrestre.</text>
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<text>Bild vom Mond der Erde.</text>
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<text>¶a≤y™∫§Î≤y.</text>
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<text>Moon</text>
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<text>This photo was taken from Birmingham, Alabama, USA, using Kodak 1600 film with a Meade LX-200 8" (200mm) f6.3 SCT. The exposure time was 3 seconds. The photo was scanned 300 dpi and 24-bit color. I used PhotoStyler to reduce the image to 640x480x256 GIF format. The full-size 24-bit version is in JPEG format. Author: Dennis Ward, <ZU02308@UABDPO.BITNET> Observatory Director, Birmingham Astronomical Society.</text>
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<text>Photo de l'éclipe lunaire partielle prise de Birmingham, Alabama le 24 mai 1994.</text>
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<text>Foto de eclipse parcial de la luna tomada de Birmingham, Alabama, el 24 de mayo del 1994.</text>
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<text>Photo einer teilweisen Mondverfinsterung, von Birmingham, Alabama, 24. Mai '94.</text>
<text>This photo was taken from Birmingham, Alabama, USA, using Kodak 1600 film with a Meade LX-200 8" (200mm) f6.3 SCT. The exposure time was 3 seconds. The photo was scanned 300 dpi and 24-bit color. I used PhotoStyler to reduce the image to 640x480x256 GIF format. The full-size 24-bit version is in JPEG format. Author: Dennis Ward, <ZU02308@UABDPO.BITNET> Observatory Director, Birmingham Astronomical Society.</text>
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<text>Photo de l'éclipe lunaire partielle prise de Birmingham, Alabama le 24 mai 1994.</text>
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<text>Foto de eclipse parcial de la luna tomada de Birmingham, Alabama, el 24 de mayo del 1994.</text>
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<text>Photo einer teilweisen Mondverfinsterung, von Birmingham, Alabama, 24. Mai '94.</text>
<text>LUNA5-24.TIF DESCRIPTION Photo of the partial lunar eclipse taken from Birmingham, Alabama at 2231CDT 24May94 (0331 UT 25May94). This photo was obtained with a Meade LX-200 (8" f6.3) using Fuji hr2 (iso 100) print film at prime (cass) focus at 1/125 sec. Photographer: Dennis Ward</text>
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<text>Photo d'une éclipse lunaire partielle prise de Birmingham, Alabama, le 24 mai 1994.</text>
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<text>Foto de eclipse parcial de la luna tomada de Birmingham, Alabama, el 24 de mayo del 1994.</text>
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<text>Photo einer teilweisen Mondverfinsterung, von Birmingham, Alabama, 24. Mai '94.</text>
<text>Farside Color Mosaic (52 kb jpeg image) Color mosaic of a portion of the lunar farside (left) obtained with the Clementine UVVIS Camera. This spectacular oblique view shows the rugged topography of the lunar highlands. The smooth dark patches seen in the extreme lower right forground and middle left background are mare plains - similar in composition to the large dark areas (mare flood basalts) that define the features of the "man in the Moon" visible to a casual observer on the Earth.</text>
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<text>Vue oblique spectaculaire de la topographie accidentée du paysage lunaire.</text>
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<text>Espectacular vista oblícua de topografía accidentada de las cordilleras lunares.</text>
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<text>Spektakulärer indirekter Blick auf die rauhe Oberfläche des Mondhochlands.</text>
<text> This is a uuencoded gif of the partial lunar eclipse of May 24. It was taken from Ft. Collins, CO with a 6 inch F/7.7 Newtonian handmade reflector.</text>
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<text>Photo d'une éclipse partielle du 24 mai prise à l'aide d'un réflecteur fait à la main.</text>
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<text>Foto de eclipse lunar parcial del 24 de mayo tomada con reflector hecho a mano.</text>
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<text>Photo von einer teilweisen Mondverfinsterung am 24. Mai '94, mit einem selbstgemachten Reflektor.</text>
<text> This is a uuencoded gif of the partial lunar eclipse of May 24. It was taken from Ft. Collins, CO with a 6 inch F/7.7 Newtonian handmade reflector.</text>
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<text>Photo d'une éclipse partielle du 24 mai prise à l'aide d'un réflecteur fait à la main.</text>
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<text>Foto de eclipse lunar parcial del 24 de mayo tomada con reflector hecho a mano.</text>
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<text>Photo von einer teilweisen Mondverfinsterung am 24. Mai '94, mit einem selbstgemachten Reflektor.</text>
<text> This is a uuencoded gif of the partial lunar eclipse of May 24. It was taken from Ft. Collins, CO with a 6 inch F/7.7 Newtonian handmade reflector.</text>
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<text>Photo d'une éclipse partielle du 24 mai prise à l'aide d'un réflecteur fait à la main.</text>
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<text>Foto de eclipse lunar parcial del 24 de mayo tomada con reflector hecho a mano.</text>
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<text>Photo von einer teilweisen Mondverfinsterung am 24. Mai '94, mit einem selbstgemachten Reflektor.</text>
<text>Clementine global albedo map of the Moon About 50,000 Clementine images have been processed and mosaicked to produce a global map of the Moon's albedo (normalized brightness or reflectivity) at a wavelength of 750 nm (just longward of visible red). This provides the best albedo map produced to date for much of the far side. The original images have resolutions of about 100 m/pixel, but were reduced to 1 km/pixel for the mosaic, and have been further reduced to 5 and 10 km/pixel for the versions shown here. Pre-flight calibration was used, which does not fully correct a brightness gradient across each frame, and this results in the north-south striping seen in the mosaic. This artifact will be corrected in future mosaics. The brightnesses are dominated by albedo everywhere except near the poles, where the brightness is dominated by topographic shading. Three versions of the mosaic are shown here: Global simple cylindrical projection at 10 km/pixel. Near side in Lambertian equal-area projection at 5 km/pixel. (300 kb jpeg image) Far side in lambertian equal-area projection at 5 km/pixel. (332 kb jpeg image) Albedo provides first-order information on surface compositions and soil "maturity" (lunar soils darken as a function of time and composition following exposure on the lunar surface). The darkest 2% of the Moon's surface corresponds to titanium-rich mare and dark mantle deposits; all of these areas are on the near side. Other dark areas correspond to the maria, or basaltic flood plains. Extensive bright areas correspond to highland soils. Large areas with intermediate albedo correspond to mixed mare-highland soils, often corresponding to "cryptomare" (hidden mare), where ancient mare basalts are mixed with more recent ejecta from impact basins. Very bright spots are due to relatively recent (less than 1 billion years old) impact craters, which have exposed immature soils. Many new identifications of relatively recent impact craters will result from analysis of the Clementine dataset, which will help us to better understand the impact flux that has profoundly influenced the evolution of life on Earth. The brightest crater larger than 20 km diameter is Giordano Bruno (upper left side of far side image), which is probably less than 50 million years old, more recent than the Cretaceous-Terciary impact on earth which killed the last of the dinosaurs 65 million years ago. Image processing by the U.S. Geological Survey in Flagstaff, Arizona.</text>
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<text>Mosaïque "global albedo" (degré de réflexion et de luminosité normalisés) carte de la Lune.</text>
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<text>Mapa lunar de albedo global (de iluminaci├│n o reflectividad normalizada).</text>
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<text>Mosaik global Albedo (normalisierte Helligkeit und Reflektion) Karte vom Mond.</text>
<text>Clementine global albedo map of the Moon About 50,000 Clementine images have been processed and mosaicked to produce a global map of the Moon's albedo (normalized brightness or reflectivity) at a wavelength of 750 nm (just longward of visible red). This provides the best albedo map produced to date for much of the far side. The original images have resolutions of about 100 m/pixel, but were reduced to 1 km/pixel for the mosaic, and have been further reduced to 5 and 10 km/pixel for the versions shown here. Pre-flight calibration was used, which does not fully correct a brightness gradient across each frame, and this results in the north-south striping seen in the mosaic. This artifact will be corrected in future mosaics. The brightnesses are dominated by albedo everywhere except near the poles, where the brightness is dominated by topographic shading. Three versions of the mosaic are shown here: Global simple cylindrical projection at 10 km/pixel. Near side in Lambertian equal-area projection at 5 km/pixel. (300 kb jpeg image) Far side in lambertian equal-area projection at 5 km/pixel. (332 kb jpeg image) Albedo provides first-order information on surface compositions and soil "maturity" (lunar soils darken as a function of time and composition following exposure on the lunar surface). The darkest 2% of the Moon's surface corresponds to titanium-rich mare and dark mantle deposits; all of these areas are on the near side. Other dark areas correspond to the maria, or basaltic flood plains. Extensive bright areas correspond to highland soils. Large areas with intermediate albedo correspond to mixed mare-highland soils, often corresponding to "cryptomare" (hidden mare), where ancient mare basalts are mixed with more recent ejecta from impact basins. Very bright spots are due to relatively recent (less than 1 billion years old) impact craters, which have exposed immature soils. Many new identifications of relatively recent impact craters will result from analysis of the Clementine dataset, which will help us to better understand the impact flux that has profoundly influenced the evolution of life on Earth. The brightest crater larger than 20 km diameter is Giordano Bruno (upper left side of far side image), which is probably less than 50 million years old, more recent than the Cretaceous-Terciary impact on earth which killed the last of the dinosaurs 65 million years ago. Image processing by the U.S. Geological Survey in Flagstaff, Arizona.</text>
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<text>Mosaïque "global albedo" (degré de réflexion et de luminosité normalisés) carte de la Lune.</text>
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<text>Mapa lunar de albedo global (de iluminaci├│n o reflectividad normalizada).</text>
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<text>Mosaik global Albedo (normalisierte Helligkeit und Reflektion) Karte vom Mond.</text>
<text>Clementine global albedo map of the Moon About 50,000 Clementine images have been processed and mosaicked to produce a global map of the Moon's albedo (normalized brightness or reflectivity) at a wavelength of 750 nm (just longward of visible red). This provides the best albedo map produced to date for much of the far side. The original images have resolutions of about 100 m/pixel, but were reduced to 1 km/pixel for the mosaic, and have been further reduced to 5 and 10 km/pixel for the versions shown here. Pre-flight calibration was used, which does not fully correct a brightness gradient across each frame, and this results in the north-south striping seen in the mosaic. This artifact will be corrected in future mosaics. The brightnesses are dominated by albedo everywhere except near the poles, where the brightness is dominated by topographic shading. Three versions of the mosaic are shown here: Global simple cylindrical projection at 10 km/pixel. Near side in Lambertian equal-area projection at 5 km/pixel. (300 kb jpeg image) Far side in lambertian equal-area projection at 5 km/pixel. (332 kb jpeg image) Albedo provides first-order information on surface compositions and soil "maturity" (lunar soils darken as a function of time and composition following exposure on the lunar surface). The darkest 2% of the Moon's surface corresponds to titanium-rich mare and dark mantle deposits; all of these areas are on the near side. Other dark areas correspond to the maria, or basaltic flood plains. Extensive bright areas correspond to highland soils. Large areas with intermediate albedo correspond to mixed mare-highland soils, often corresponding to "cryptomare" (hidden mare), where ancient mare basalts are mixed with more recent ejecta from impact basins. Very bright spots are due to relatively recent (less than 1 billion years old) impact craters, which have exposed immature soils. Many new identifications of relatively recent impact craters will result from analysis of the Clementine dataset, which will help us to better understand the impact flux that has profoundly influenced the evolution of life on Earth. The brightest crater larger than 20 km diameter is Giordano Bruno (upper left side of far side image), which is probably less than 50 million years old, more recent than the Cretaceous-Terciary impact on earth which killed the last of the dinosaurs 65 million years ago. Image processing by the U.S. Geological Survey in Flagstaff, Arizona.</text>
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<text>Mosaïque "global albedo" (degré de réflexion et de luminosité normalisés) carte de la Lune.</text>
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<text>Mapa lunar de albedo global (de iluminaci├│n o reflectividad normalizada).</text>
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<text>Mosaik global Albedo (normalisierte Helligkeit und Reflektion) Karte vom Mond.</text>
<text>Apollo-12 (28) Pad 39-A (6) Saturn-V AS-507 () High Bay 3 MLP 2 Firing Room 2 Crew: Charles Conrad, Jr. Richard F. Gordon, Jr. Alan L. Bean Backup Crew: Milestones: 03/09/69 - S-IVB ondock at KSC 04/21/69 - S-II Stage ondock at KSC 05/03/69 - S-1C Stage ondock at KSC 05/08/69 - S-IU ondock at KSC 11/14/69 - Launch Payload: Yankee Clipper (CM-108) and Intrepid (LM-6) Mission Objective: Launch: November 14, 1969. Orbit: Duration: 10 Days, 04 hours, 36 min, seconds Distance: miles Landing: November 24, 1969 Mission Highlights: Landing site: Ocean of Storms. Retrieved parts of the unmanned Surveyor 3, which had landed on the Moon in April 1967. Apollo Lunar Surface Experiments Package (ALSEP) deployed. Lunar surface stay-time, 31.5 hours; in lunar orbit 89 hours, with 45 orbits. LM descent stage impacted on Moon. 34kg (75 lbs) of material gathered.</text>
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<text>Photos prises durant 45 orbit Apollo-12 mission to "Ocean of Storms".</text>
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<text>Fotos del 'Mar de Tormentas tomadas' durante la misi├│n de Apollo-12 de 45 ├│rbitas.</text>
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<text>Photos vom 'Ozean der Stürme,' aufgenommen während der 45 Orbit Apollo-12-Mission.</text>
<text>Apollo-8 (24) Pad 39-A (3) Saturn-V AS-503 (3) High Bay 1 MLP 1 Firing Room 1 Crew: Frank Borman, Commander James A. Lovell, Jr. William A. Anders Backup Crew: Milestones: 12/24/67 - S-II Stage ondock at KSC 12/27/67 - S-1C Stage ondock at KSC 12/30/67 - S-IVB ondock at KSC 01/04/68 - S-IU ondock at KSC 08/14/68 - Launch Vehicle at Pad 10/17/68 - Spacecraft at Pad 12/11/68 - Countdown Demonstration Test 12/21/68 - Launch Payload: CSM-103 Mission Objective: Demonstrate crew/space vehicle/mission support facilities during manned Saturn V/CSM mission. Demonstrate translunar injection, CSM navigation, communications, and midcourse corrections. Assess CSM consumables and passive thermal control. Demonstrate CSM performance in cislunar and lunar orbit environment. Demonstrate communications and tracking at lunar distances. Return high-resolution photographs of proposed Apollo landing sites and locations of scientific interest. All mission objectives were achieved. Launch: December 21, 1968, 07:51:00 a.m. EST. Kennedy Space Center Launch Complex 39-A. Orbit: Altitude: 190km x 180km Inclination: xxx degrees Orbits: Duration: 6 Days, 3 hours, 0 min, 42 seconds Distance: miles Landing: December 27, 1968; 10:52 am EST; Landing point 8deg 7.5min North and 165deg 1.2min West. Miss distance was 2.5km; Splashdown time, December 27, 1968 at 10:52 a.m. EST; MET: 147:00:42. Crew on board U.S.S Yorktown at 12:20 p.m. EST; Spacecraft aboard ship at 01:20 p.m. Mission Highlights: Apogee, 190 kilometers; perigee 180 kilometers. Translunar injection at 02:56:05.5 MET; maximum distance from earth, 376,745 kilometers; lunar orbit insertion 69:08:20 MET; lunar orbit 312km by 111km; transearth injection, 89:19:17 MET. In lunar orbit 20 hours, with 10 orbits. First manned lunar orbital mission. Support facilities tested. Photographs taken of Earth and Moon. Live TV broadcasts.</text>
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<text>Photos de la Terre et de la Lune prise par Apollo-8, première mission lunaire orbitale de l'être humain.</text>
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<text>Fotos de la tierra y la luna de Apollo-8, primera misi├│n orbital con tripulaci├│n.</text>
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<text>Photos von Erde und Mond, aufgenommen von Apollo-8, die erste bemannte Mondorbital -Mission.</text>
<text> GALAXY M100 RESOLUTION COMPARISON This sequence of pictures shows successive steps in optical improvement from ground based telescopes to the newly improved Hubble Space Telescope and demonstrates the unique capability of the repaired HST. HST offers superb resolution, which allows astronomers to distinguish individual stars in other galaxies. The resolution also allows very faint stars to be seen. This set of pictures demonstrates that the repaired HST can see stars which could never before be detected. [upper left] An outer region in the galaxy M100 as imaged by Hubble Space Telescope's second generation Wide Field/Planetary Camera (WFPC-2). The WFPC-2 incorporates modified optics that correct for the aberration of the primary mirror on the HST. While this image is not as visually spectacular as the image of the core of the galaxy, it demonstrates one of the most important improvements in the capability of the telescope achieved during the HST servicing mission -- the ability to detect and measure the light from individual faint stars in distant galaxies. Note in particular the stars indicated by the arrows, which have the approximate brightness expected for Cepheid variables in M100. While these specific stars may not be Cepheids, repeated measurements of hundreds of stars of similar brightness spread throughout the galaxy are expected to turn up several dozens of Cepheids. By accurately measuring the brightness of these ``standard candles,'' astronomers will use the WFPC-2 to determine an accurate distance to M100. When combined with similar measurements for other galaxies, this distance will provide a crucial link in the chain that astronomers use to determine the expansion rate, age, and size of the universe. [upper right] A picture taken with the WFPC-1 camera on November 27, 1993, just a few days prior to the STS-61 servicing mission. The resolution in the WFPC-1 image represents a significant improvement over what can be seen from the ground -- a fact that has allowed a wealth of fascinating science to be carried out with the HST since its launch in 1990. However, only the brightest objects seen in the frame to the left could be seen before the servicing mission. The faint objects, which are critical for determining the distance to the galaxy, and for studies of stellar populations, star formation and evolution, and galactic structure, cannot be seen because of the optical aberration present before servicing. [lower left] This panel shows the WFPC-1 image after computer image reconstruction, using algorithms commonly used on Hubble pictures taken before the servicing mission. Although these algorithms can significantly sharpen up features in the original picture, they do not allow the recovery of faint objects; many stars which are detected in the WFPC-2 image cannot even be seen, let alone measured, in the reconstructed WFPC-1 image. Also note that the relative brightnesses of many objects which can be seen in the reconstructed WFPC-1 image differ from the true brightnesses apparent in the WFPC-2 image. This demonstrates that even in cases where image reconstruction could recover interesting morphological information on bright objects, it could not recover the quantitative information that can now be obtained with the WFPC-2. [lower right] An image of the same region in M100 taken with the 200-inch Hale Telescope located on top of Mt. Palomar in California. The resolution is just under an arc second, which is slightly better than typical night sky conditions for ground based observing. PHOTO RELEASE NO.: STScI-PR94-03</text>
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<text>Séquence de photos de la Galaxie M100 montrant des améliorations dans le téléscope Hubble.</text>
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<text>Secuencia de retratos de la Galaxia M100 que muestran mejoras en el telescopio Hubble.</text>
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<text>Serie von Bildern der M100-Galaxis, die Verbesserungen im Hubble-Teleskop zeigen.</text>
<text> HUBBLE OBSERVES A STAR ON THE BRINK OF DESTRUCTION A NASA Hubble Space Telescope "natural color" image of the material surrounding the star Eta Carinae, as imaged by the Wide Field Planetary Camera 2 (WFPC-2). The Camera was installed in the Hubble Space Telescope during the STS-61 Hubble Servicing Mission. The WFPC-2 optically corrects for the aberration of the telescope's primary mirror, restoring the telescope's vision to its originally planned clarity. Eta Carinae has a mass of approximately 150 times that of the sun, and is about 4 million times brighter than our local star, making it one of the most massive and most luminous stars known. Eta Carinae is highly unstable, and prone to violent outbursts. The last of these occurred in 1841, when despite its distance (over 10,000 light years away) Eta Carinae briefly became the second brightest star in the sky. Pre-servicing mission HST observations taken with the WF/PC-I reveled new detail in the rapidly expanding shell of material which was ejected during the last century's outburst. However, the earlier effects of HST's spherical aberration obscured the structure of the material very near Eta Carinae itself. The clear view of Eta Carinae now provided by WFPC-2 dramatically demonstrates the ability of HST to reliable study faint structure near bright objects. The picture is a combination of three different images taken in red, green, and blue light. The ghostly red outer glow surrounding the star is composed of the very fastest moving of the material which was ejected during the last century's outburst. This material, much of which is moving more than two million miles per hour, is largely composed of nitrogen and other elements formed in the interior of the massive star, and subsequently ejected into interstellar space. The bright blue-white nebulosity closer in to the star also consists of ejected stellar material. Unlike the outer nebulosity, this material is very dusty and reflects starlight. The new data show that this structure consists of two lobes of material, one of which (lower left) is moving toward us and the other of which (upper right) is moving away. The knots of ejected material have sizes comparable to that of our solar system. Previous models of such bipolar flows predict a dense disk surrounding the star which funnels the ejected material out of the poles of the system. In Eta Carinae, however, high velocity material is spraying out in the same plane as the hypothetical disk, which is supposed to be channeling the flow. This is quite unexpected. The WFPC-2 observations of Eta Carinae raise as many questions as they answer. credit: J. Hester/Arizona State University NASA PHOTO RELEASE NO.: STScI-PR94-09</text>
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<text>Image Hubble de couleur naturelle de la matière environnant l'étoile Eta Carinae.</text>
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<text>Imagen de color natural de material alrededor de la estrella Eta Carinae.</text>
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<text>Hubble natur-Farben-Bild von Material das den Eta Carinae Stern umgibt.</text>
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<text>≥Ú¬∂¶b Eta Carinae ¨P™∫ Hubble §—µM±m¶‚πœπ≥.</text>
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<text> HUBBLE SPACE TELESCOPE IMAGES OF A BRIGHT STAR IN THE LARGE MAGELLANIC CLOUD The three panels show images of a very bright (Wolf-Rayet) star, Melnick 34, located in the giant star-forming region called 30 Doradus in the Large Magellanic Cloud. In the background are a number of fainter stars that are comparable in brightness to our Sun. [Left] Ground Based View The best available ground-based image of Melnick 34 (Courtesy Dr. Georges Meylan of the European Southern Observatory). This image was taken under ideal atmospheric conditions when the width of a star image was about 0.6 arc seconds. [Middle] WF/PC-1 Image The same field, as imaged by the first Wide Field and Planetary Camera (WF/PC-). The advantages of working in space above Earth's distorting atmosphere are immediately apparent. Atmospheric blurring is gone and many more stars are visible. However, the effects of the Hubble Telescope's spherical aberration also are apparent. In particular there is a four arc second diameter "skirt" around the bright star which obscures the view of the sky in its vicinity. It is very hard to do quantitative measurements on such an image because of the way the light from many stars overlaps. [Right] WFPC-2 Image An image of the same field, made with the new Wide Field and Planetary Camera's (WFPC-2) improved optics. With an exposure equivalent to the WF/PC-1 image, this WFPC-2 image collects all the light from the central star into sharp focus because the telescope's spherical aberration is corrected by the new camera's optics. A large number of fainter stars also become visible. This is because all of their light is concentrated, and enough is gathered to make them visible above the intrinsic noise from the instrument and sky. In the WF/PC-1 image, enough light is distributed in the image "skirt that background stars become lost in the noise. In WFPC-2, not only are the fainter stars visible, but quantitative measurements of their brightness also are possible. By facilitating quantitative measurements in faint and crowded star fields, the Wide Field and Planetary Camera-2 and the Hubble Space Telescope will be able to address all the key programs for which the telescope and instrument were originally designed. PHOTO RELEASE NO.: STScI-PR94-05</text>
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<text>Melnick 34 dans 30 Doradu, la géante région de formation d'étoiles sur le Magellanic Cloud.</text>
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<text>Melnick 34 en 30 Doradus en la región gigante criadero de estrellas de la Nube Magallánica.</text>
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<text>Melnick 34 in 30 Doradus, die gigantische sternenformende Region in der Magellan-Wolke.</text>
<text> MAGELLAN PROJECT OFFICE P-38810 8/12/91 The comet-like tail trending northeast from this volcanic edifice is a relatively radar-bright deposit. The volcano, whose basal diameter is 5 kilometers (about 3 miles), is a local topographic high that has slowed down northeast trending winds enough to cause deposition of this material. The streak is 35 kilometers (about 22 miles) long and 10 kilometers (about 6 miles) wide. The volcano is located at the western end of Parga Chasma at 9.4 degrees south latitude, 247.5 degrees east longitude. Jet Propulsion Laboratory California Institute of Technology National Aeronautics and Space Administration Pasadena, Calif. 91109 </text>
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<text>Edifice volcanique à Parga Chasma avec comète dirigée vers le nord-est.</text>
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<text>Edificio volcánico en Parga Chasma con cola semejante a un cometa hacia con índole hacia el noreste.</text>
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<text>Vulkanische Anhäufung auf Parga Chasma, mit einem kometenartigen Schwanz, nach Nordosten zeigend.</text>
<text>This file describes the first set of gif images produced from black and white photos supplied by NASA Headquarters in Washington DC. Thanks go to Charles Redmond, NASA Washington for the release of the pictures, and all subsequent pictures. Thanks also go to Peter Yee at NASA Ames and James Green of NSSDC. The images will have file names which correspond to the photo number on the back of each photo, this way, it can be traced to a photo quickly in the inventory, and it eliminates duplicate file names. The text which follows each image number is the text exactly as it appears on the back of the photograph. The only exception is of SN1987A, which had no text. These gifs were produced on a 286 machine with a 512X480 monochrome CCD and an 8 bit frame grabber built by Mechanical Engineering department. Again note that the best display will be in 640X480 256 color mode if using VUGIF. The conversion from the lab IMG format to GIF was done using software written by a grad student in Electrical Engineering. Since the pictures are glossy, and sometimes very dark, you may notice some loss of definition. This will be corrected shortly when a proper lighting source is available. Now on to the tasty bits :-} Image 90H283 The space shuttle Discovery soars into the morning skies above Florida, carrying a crew of five, and the Hubble Space Telescope. Launch of Space Shuttle Mission STS-31 from pad 39-B occured at 8:33:51 a.m. EDT, April 24. Crew members are Commander Loren J. Shriver, Pilot Charles F. Bolden, Jr., and Mission Specialists Kathryn D. Sullivan, Steven A. Hawley, and Bruce McCandless II. Image 90H303 STS-31 Onboard Scene Discovery's remote manipulator system (RMS) hoists the huge Hubble Space Telescope (HST) over Earth's horizon prior to deployment of HST's solar panels and antennae. This scene, from a very busy flight day 2, was among the first eight STS-31 photographs released by NASA upon completion of the five-day flight. The scene was photographed with a 70mm handheld Hasselblad. Image 90H301 STS-31 Onboard Scene Most of the giant Hubble Space Telescope (HST) can be seen as it is suspended in space by Discovery's remote manipulator system (RMS) following deployment of part of its solar panels and antennae. This photo was taken with a handheld Hasselblad camera. This was among the first photos NASA released on April 30 from the five-day STS-31 mission. Image 90H350 STS-31 Launch A low angle view of the launch of the STS-31 mission. Onboard Discovery are the crew of five vereran astronauts and the Hubble Space Telescope. Official launch time was 8:33:51.0492 a.m. EDT. Headed for approximately five days in space are astronauts Loren J. Shriver, Charles F. Bolden Jr, Bruce McCandless II, Kathryn D. Sullivan and Steven A. Hawley. Image 90H272 Same text as Image 90H283 Image 90H291 Mission Completed The space shuttle Discovery completes a successful STS-31 mission with an early morning (6:49 a.m.) landing April 29, 1990, on the main 15,000 foot runway (Rwy 22) at Edwards, California. The STS -31 mission deployed the Hubble Space Telescope in a 300 mile high orbit during the five day mission. The instrument is expected to return photographs of the most distant reaches of space once it has been thoroughly tested and begins scientific operations later this year. Members of the Discovery crew were Loren J. Sgriver, commander, Charles F. Bolden, pilot, and mission specialists Steven A. Hawley, Kathryn D. Sullivan and Bruce McCandless II. All had flown on previous space shuttle missions. Image SN1987A This is a monochrome representation of the previously seen color image. There was no accompanying text.</text>
</content>
<content>
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<id>29</id>
<text>Photos pour Space Shuttle Mission STS- 31 avec le téléscope Hubble à bord.</text>
</content>
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<id>31</id>
<text>Fotos de la misi├│n del Shuttle STS-31 con el telescopio Hubble a bordo.</text>
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<text>Photos von der Space-Shuttle-Mission STS-31 mit dem Hubble-Teleskop an Bord.</text>
<text>This file describes the first set of gif images produced from black and white photos supplied by NASA Headquarters in Washington DC. Thanks go to Charles Redmond, NASA Washington for the release of the pictures, and all subsequent pictures. Thanks also go to Peter Yee at NASA Ames and James Green of NSSDC. The images will have file names which correspond to the photo number on the back of each photo, this way, it can be traced to a photo quickly in the inventory, and it eliminates duplicate file names. The text which follows each image number is the text exactly as it appears on the back of the photograph. The only exception is of SN1987A, which had no text. These gifs were produced on a 286 machine with a 512X480 monochrome CCD and an 8 bit frame grabber built by Mechanical Engineering department. Again note that the best display will be in 640X480 256 color mode if using VUGIF. The conversion from the lab IMG format to GIF was done using software written by a grad student in Electrical Engineering. Since the pictures are glossy, and sometimes very dark, you may notice some loss of definition. This will be corrected shortly when a proper lighting source is available. Now on to the tasty bits :-} Image 90H283 The space shuttle Discovery soars into the morning skies above Florida, carrying a crew of five, and the Hubble Space Telescope. Launch of Space Shuttle Mission STS-31 from pad 39-B occured at 8:33:51 a.m. EDT, April 24. Crew members are Commander Loren J. Shriver, Pilot Charles F. Bolden, Jr., and Mission Specialists Kathryn D. Sullivan, Steven A. Hawley, and Bruce McCandless II. Image 90H303 STS-31 Onboard Scene Discovery's remote manipulator system (RMS) hoists the huge Hubble Space Telescope (HST) over Earth's horizon prior to deployment of HST's solar panels and antennae. This scene, from a very busy flight day 2, was among the first eight STS-31 photographs released by NASA upon completion of the five-day flight. The scene was photographed with a 70mm handheld Hasselblad. Image 90H301 STS-31 Onboard Scene Most of the giant Hubble Space Telescope (HST) can be seen as it is suspended in space by Discovery's remote manipulator system (RMS) following deployment of part of its solar panels and antennae. This photo was taken with a handheld Hasselblad camera. This was among the first photos NASA released on April 30 from the five-day STS-31 mission. Image 90H350 STS-31 Launch A low angle view of the launch of the STS-31 mission. Onboard Discovery are the crew of five vereran astronauts and the Hubble Space Telescope. Official launch time was 8:33:51.0492 a.m. EDT. Headed for approximately five days in space are astronauts Loren J. Shriver, Charles F. Bolden Jr, Bruce McCandless II, Kathryn D. Sullivan and Steven A. Hawley. Image 90H272 Same text as Image 90H283 Image 90H291 Mission Completed The space shuttle Discovery completes a successful STS-31 mission with an early morning (6:49 a.m.) landing April 29, 1990, on the main 15,000 foot runway (Rwy 22) at Edwards, California. The STS -31 mission deployed the Hubble Space Telescope in a 300 mile high orbit during the five day mission. The instrument is expected to return photographs of the most distant reaches of space once it has been thoroughly tested and begins scientific operations later this year. Members of the Discovery crew were Loren J. Sgriver, commander, Charles F. Bolden, pilot, and mission specialists Steven A. Hawley, Kathryn D. Sullivan and Bruce McCandless II. All had flown on previous space shuttle missions. Image SN1987A This is a monochrome representation of the previously seen color image. There was no accompanying text.</text>
</content>
<content>
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<id>29</id>
<text>Photos pour Space Shuttle Mission STS- 31 avec le téléscope Hubble à bord.</text>
</content>
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<id>31</id>
<text>Fotos de la misi├│n del Shuttle STS-31 con el telescopio Hubble a bordo.</text>
</content>
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<id>30</id>
<text>Photos von der Space-Shuttle-Mission STS-31 mit dem Hubble-Teleskop an Bord.</text>
<text>A large, mosaic-ed, three-color, infrared image of the Rho-Ophiuchus region taken by Karen M. Strom. The Rho-Ophiuchus Cloud is the set of reddish clouds in the upper right quadrant.</text>
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<text>Grande, image mosaïque, trois-couleurs, infrarouge de la région Rho-Ophiuchus.</text>
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<id>31</id>
<text>Imagen infrarroja mosaica grande tricolor de la regi├│n Rho-Ophiucus. </text>
</content>
<content>
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<id>30</id>
<text>Großes, drei-Farben, infrarot, Mosaikbild der Rho-Ophiuchus-Region.</text>
<text>There are several astronomical images posted here. The pictures: dumbell (M27) horsehead M33 northamerica (NGC7000) orion (M42/M43) were taken by me and Scott Reid using my 8 inch Meade SCT scope. We used hypersensitized Ektar 1000 film. The exposures and development was as follows ("normal" development is 4.5 minutes at 38C) : Time(min) development(min) dumbell 50 6 horsehead 90 x 2 8 M33 75 x 2 6 northamerica 90 x 2 6 orion 35 5 The "x 2" means two negatives were taken and sandwiched together for printing. The pictures grlens r136 sn1987a were obtained by the Faint Object Camera of the Hubble Space Telescope and were obtained from the press office of NASA. Please read the file hubble.txt for lots of data about them. They are not copyright, but NASA asks that they not be use for advertizing. The pictures were digitized using a Microtek scanner on a Mac II. The tiff images were converted to gif on a PC. All these pictures are colormapped with a palette of 256 colors (only 225 of which are used). I use a gif display program for the PC called "picem" and a Video 7 super VGA card. With this setup (640x400x256 colors) all of the information in all of the original photographic prints except the Orion one is actually visible.</text>
</content>
<content>
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<id>29</id>
<text>Images prises par le Faint Object Camera of the Hubble Space Telescope.</text>
</content>
<content>
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<id>31</id>
<text>Imágenes realizadas por la Cámara para Objetos de Mínima Definición del Telescopio Hubble.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Bilder mit der Faint-Object-Kamera des Hubble-Teleskops aufgenommen.</text>
<text>There are several astronomical images posted here. The pictures: dumbell (M27) horsehead M33 northamerica (NGC7000) orion (M42/M43) were taken by me and Scott Reid using my 8 inch Meade SCT scope. We used hypersensitized Ektar 1000 film. The exposures and development was as follows ("normal" development is 4.5 minutes at 38C) : Time(min) development(min) dumbell 50 6 horsehead 90 x 2 8 M33 75 x 2 6 northamerica 90 x 2 6 orion 35 5 The "x 2" means two negatives were taken and sandwiched together for printing. The pictures grlens r136 sn1987a were obtained by the Faint Object Camera of the Hubble Space Telescope and were obtained from the press office of NASA. Please read the file hubble.txt for lots of data about them. They are not copyright, but NASA asks that they not be use for advertizing. The pictures were digitized using a Microtek scanner on a Mac II. The tiff images were converted to gif on a PC. All these pictures are colormapped with a palette of 256 colors (only 225 of which are used). I use a gif display program for the PC called "picem" and a Video 7 super VGA card. With this setup (640x400x256 colors) all of the information in all of the original photographic prints except the Orion one is actually visible.</text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Images prises par le Faint Object Camera of the Hubble Space Telescope.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Imágenes realizadas por la Cámara para Objetos de Mínima Definición del Telescopio Hubble.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Bilder mit der Faint-Object-Kamera des Hubble-Teleskops aufgenommen.</text>
<text>There are several astronomical images posted here. The pictures: dumbell (M27) horsehead M33 northamerica (NGC7000) orion (M42/M43) were taken by me and Scott Reid using my 8 inch Meade SCT scope. We used hypersensitized Ektar 1000 film. The exposures and development was as follows ("normal" development is 4.5 minutes at 38C) : Time(min) development(min) dumbell 50 6 horsehead 90 x 2 8 M33 75 x 2 6 northamerica 90 x 2 6 orion 35 5 The "x 2" means two negatives were taken and sandwiched together for printing. The pictures grlens r136 sn1987a were obtained by the Faint Object Camera of the Hubble Space Telescope and were obtained from the press office of NASA. Please read the file hubble.txt for lots of data about them. They are not copyright, but NASA asks that they not be use for advertizing. The pictures were digitized using a Microtek scanner on a Mac II. The tiff images were converted to gif on a PC. All these pictures are colormapped with a palette of 256 colors (only 225 of which are used). I use a gif display program for the PC called "picem" and a Video 7 super VGA card. With this setup (640x400x256 colors) all of the information in all of the original photographic prints except the Orion one is actually visible.</text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Images prises par le Faint Object Camera of the Hubble Space Telescope.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Imágenes realizadas por la Cámara para Objetos de Mínima Definición del Telescopio Hubble.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Bilder mit der Faint-Object-Kamera des Hubble-Teleskops aufgenommen.</text>
<text>There are several astronomical images posted here. The pictures: dumbell (M27) horsehead M33 northamerica (NGC7000) orion (M42/M43) were taken by me and Scott Reid using my 8 inch Meade SCT scope. We used hypersensitized Ektar 1000 film. The exposures and development was as follows ("normal" development is 4.5 minutes at 38C) : Time(min) development(min) dumbell 50 6 horsehead 90 x 2 8 M33 75 x 2 6 northamerica 90 x 2 6 orion 35 5 The "x 2" means two negatives were taken and sandwiched together for printing. The pictures grlens r136 sn1987a were obtained by the Faint Object Camera of the Hubble Space Telescope and were obtained from the press office of NASA. Please read the file hubble.txt for lots of data about them. They are not copyright, but NASA asks that they not be use for advertizing. The pictures were digitized using a Microtek scanner on a Mac II. The tiff images were converted to gif on a PC. All these pictures are colormapped with a palette of 256 colors (only 225 of which are used). I use a gif display program for the PC called "picem" and a Video 7 super VGA card. With this setup (640x400x256 colors) all of the information in all of the original photographic prints except the Orion one is actually visible.</text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Images prises par le Faint Object Camera of the Hubble Space Telescope.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Imágenes realizadas por la Cámara para Objetos de Mínima Definición del Telescopio Hubble.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Bilder mit der Faint-Object-Kamera des Hubble-Teleskops aufgenommen.</text>
<text>There are several astronomical images posted here. The pictures: dumbell (M27) horsehead M33 northamerica (NGC7000) orion (M42/M43) were taken by me and Scott Reid using my 8 inch Meade SCT scope. We used hypersensitized Ektar 1000 film. The exposures and development was as follows ("normal" development is 4.5 minutes at 38C) : Time(min) development(min) dumbell 50 6 horsehead 90 x 2 8 M33 75 x 2 6 northamerica 90 x 2 6 orion 35 5 The "x 2" means two negatives were taken and sandwiched together for printing. The pictures grlens r136 sn1987a were obtained by the Faint Object Camera of the Hubble Space Telescope and were obtained from the press office of NASA. Please read the file hubble.txt for lots of data about them. They are not copyright, but NASA asks that they not be use for advertizing. The pictures were digitized using a Microtek scanner on a Mac II. The tiff images were converted to gif on a PC. All these pictures are colormapped with a palette of 256 colors (only 225 of which are used). I use a gif display program for the PC called "picem" and a Video 7 super VGA card. With this setup (640x400x256 colors) all of the information in all of the original photographic prints except the Orion one is actually visible.</text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Images prises avec le Faint Object Camera of the Hubble Space Telescope.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Imágenes realizadas por la Cámara para Objetos de Mínima Definición del Telescopio Hubble.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Bilder mit der Faint-Object-Kamera des Hubble-Teleskops aufgenommen.</text>
<text>This is a CCD image of comet 1993a "Mueller", taken on October 6, 1993, using SBIG's ST-6 CCD-camera and a 288mm f/5.2 Schmidt-Cassegrain telescope.The exposure lasted from 19:11 U.T. to 19:21 U.T. The field of view is 19.6' x 14.4'. The comet has a coma diameter of some- what more than 3' and a fan-shaped tail, up to 7' long, between P.A. 220o and P.A. 310o. (Sorry, I mixed that up in my posting last week: 1993a has a fan-shaped tail oriented around P.A. 270o, while 1993p shows a slender AN-tail pointing nearly exactly northward. However, this an-tail may not be visible any longer...) The brightest star visible (PPM 7788) is of photographic magnitude 8.8. In this GIF-image, this star and the head of the comet appear to be nearly of the same brightness. However, a close inspection of the original CCD-image (which has a resolution of 16 bit per pixel rather than 8 bit for GIFs) shows that the star trail is satured at a value of 65535, while the brightest pixel in the comet's head reaches a value of only 15608. According to our measurements, the comet is of mag 10.5 in red light (where unfiltered, thick CCD's are most sensitive).Keep in mind that a comet has usually bright emissions in blue and green light, where our CCD is not that sensitive.</text>
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<text>Image CCD de la comète 1993a Mueller prise le 6 october 1993 montrant la queue en forme d'évantail.</text>
</content>
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<id>31</id>
<text>Imagen CCD del cometa 1993a Mueller tomada el 6 de oct., 1993, que muestra una cola en forma de abanico.</text>
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<id>30</id>
<text>CCD Aufnahme vom Kometen 1993a Mueller mit Fächergeformtem Schwanz, vom 6.10.'93.</text>
<text>There are several astronomical images posted here. The pictures: dumbell (M27) horsehead M33 northamerica (NGC7000) orion (M42/M43) were taken by me and Scott Reid using my 8 inch Meade SCT scope. We used hypersensitized Ektar 1000 film. The exposures and development was as follows ("normal" development is 4.5 minutes at 38C) : Time(min) development(min) dumbell 50 6 horsehead 90 x 2 8 M33 75 x 2 6 northamerica 90 x 2 6 orion 35 5 The "x 2" means two negatives were taken and sandwiched together for printing. The pictures grlens r136 sn1987a were obtained by the Faint Object Camera of the Hubble Space Telescope and were obtained from the press office of NASA. Please read the file hubble.txt for lots of data about them. They are not copyright, but NASA asks that they not be use for advertizing. The pictures were digitized using a Microtek scanner on a Mac II. The tiff images were converted to gif on a PC. All these pictures are colormapped with a palette of 256 colors (only 225 of which are used). I use a gif display program for the PC called "picem" and a Video 7 super VGA card. With this setup (640x400x256 colors) all of the information in all of the original photographic prints except the Orion one is actually visible.</text>
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<id>29</id>
<text>Différentes images astonomiques comprenant Horsehead et Orion.</text>
</content>
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<id>31</id>
<text>Varias imágenes astronómicas inclusive de la Cabeza de Caballo y de Orión.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Verschiedene astronomische Bilder, Pferdekopf und Orion mit eingschlossen</text>
<text>From: jtws@dalsol.rtc.sc.ti.com (Jason Ware-Dallas) Subject: Orion Nebula Region (1of6)24M Date: 25 Jul 1994 20:39:34 GMT The following file is a picture of the Orion Nebula, M-42, in the constellation Orion. I took it with a Meade 6" diameter 152 ED APO refractor telescope and Fuji HG400 film (120 format). The photo is an integation of four exposures running 60 long. Notice that the center of the nebula is not washed out like most pictures of this object. This is because I took a fifth exposure lasting 12-minutes long, and added it to the other four using an un-sharp mask in the darkroom. The blue object above the Orion Nebula (to the right in this image) is NGC - 1973/5/7. This photo was recently published in Sky & Telescope as a full page image. It is also currenlty being used as a backdrop in the Meade logo for their adds......Enjoy!! I have 16x20 and 8x10 prints available if you are interested. Jason Ware</text>
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<id>29</id>
<text>Image d'Orion Nebula, M-42, dans la constellation Orion.</text>
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<id>31</id>
<text>Retrato de la Nebulosa de Ori├│n, M-42, en la constelaci├│n de Ori├│n.</text>
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<id>30</id>
<text>Bild von der Orion Nebula, M-42, in der Orion-Konstellation.</text>
<text>Jason Ware <jtws@dalsol.rtc.sc.ti.com> from Dallas has some time ago posted this image of the Andromeda Galaxy M31 (NGC 224) and its companions M32 (NGC 221) and M110 (NGC 205) to the abpm Usenet group. I upload it due to request. The photo is also currenlty being used as a backdrop in the Meade logo for their adds... ...Enjoy!!</text>
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<text>Andromeda Galaxy M31 (NGC 224) et M32 (NGC 221) et M110 (NGC 205).</text>
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<id>31</id>
<text>Galaxia M31 de Andr├│meda (NGC 224) y M32 (NGC 221) y M110 (NGC 205).</text>
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<text>Andromeda Galaxis M31 (NGC 224) und M32 (NGC 221) und M110 (NGC 205)</text>
<text> Figure Caption for pair of images of 'Comet Nucleus Q'. 21Jul94 Last Look at the Q-nuclei First image - March 30, 1994. Two Q-nuclei and a split nucleus, P. Second image - July 20, 1994. at T - 10 hours. Both nuclei still show no sign of further fragmentation, although the coma near each is being stretched out along the direction of motion. Both images were taken with the WFPC2 Planetary Camera using a red filter. Credit: H. A. Weaver and T. E. Smith</text>
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<id>29</id>
<text>Images de la Comète Nucleus Q et d'un nucleus partagé, P.</text>
</content>
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<id>31</id>
<text>Imágenes del Núcleo de Cometa Q y un Núcleo Fragmentado, P.</text>
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<content>
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<id>30</id>
<text>Bilder vom Kometenkern Q und einem gespaltenen Kern P.</text>
</content>
<content>
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<id>32</id>
<text>¶bºz¨PÆ÷§fl Q ©MÆ÷§fl P ™∫πœπ≥.</text>
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<text>äO âF íà</text>
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<text>There are several astronomical images posted here. The pictures: dumbell (M27) horsehead M33 northamerica (NGC7000) orion (M42/M43) were taken by me and Scott Reid using my 8 inch Meade SCT scope. We used hypersensitized Ektar 1000 film. The exposures and development was as follows ("normal" development is 4.5 minutes at 38C) : Time(min) development(min) dumbell 50 6 horsehead 90 x 2 8 M33 75 x 2 6 northamerica 90 x 2 6 orion 35 5 The "x 2" means two negatives were taken and sandwiched together for printing. The pictures grlens r136 sn1987a were obtained by the Faint Object Camera of the Hubble Space Telescope and were obtained from the press office of NASA. Please read the file hubble.txt for lots of data about them. They are not copyright, but NASA asks that they not be use for advertizing. The pictures were digitized using a Microtek scanner on a Mac II. The tiff images were converted to gif on a PC. All these pictures are colormapped with a palette of 256 colors (only 225 of which are used). I use a gif display program for the PC called "picem" and a Video 7 super VGA card. With this setup (640x400x256 colors) all of the information in all of the original photographic prints except the Orion one is actually visible.</text>
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<id>29</id>
<text>Images du Faint Object Camera du téléscope Hubble.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Imágenes realizadas por la Cámara para Objetos de Mínima Definición del Telescopio Hubble.</text>
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<content>
<layer>background</layer>
<id>30</id>
<text>Bilder von der Faint Objekt-Kamera des Hubble-Teleskops.</text>
<text>Halley's Comet The full size image of Halley's Comet is 49 KB. Constants MEAN RADIUS: (4 x 8) km MASS: ? (Earth=1) DENSITY: ? (gm/cm) GRAVITY: ? (Earth=1) ORBIT PERIOD: 76.6 (Earth years) ROTATION PERIOD: ? (Earth days) SEMIMAJOR AXIS OF ORBIT: 17.8 au ECCENTRICITY OF ORBIT: 0.967</text>
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<text>Photo de la comète Halley.</text>
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<content>
<layer>background</layer>
<id>31</id>
<text>Foto del cometa de Halley con el número de índice de un renglón (1546?))</text>
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<content>
<layer>background</layer>
<id>30</id>
<text>Photo vom Halley'schen Kometen.</text>
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<text>Halley ™∫ºz¨P∑”§˘.</text>
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<text>äO âF íà</text>
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<text>There are several astronomical images posted here. The pictures: dumbell (M27) horsehead M33 northamerica (NGC7000) orion (M42/M43) were taken by me and Scott Reid using my 8 inch Meade SCT scope. We used hypersensitized Ektar 1000 film. The exposures and development was as follows ("normal" development is 4.5 minutes at 38C) : Time(min) development(min) dumbell 50 6 horsehead 90 x 2 8 M33 75 x 2 6 northamerica 90 x 2 6 orion 35 5 The "x 2" means two negatives were taken and sandwiched together for printing. The pictures grlens r136 sn1987a were obtained by the Faint Object Camera of the Hubble Space Telescope and were obtained from the press office of NASA. Please read the file hubble.txt for lots of data about them. They are not copyright, but NASA asks that they not be use for advertizing. The pictures were digitized using a Microtek scanner on a Mac II. The tiff images were converted to gif on a PC. All these pictures are colormapped with a palette of 256 colors (only 225 of which are used). I use a gif display program for the PC called "picem" and a Video 7 super VGA card. With this setup (640x400x256 colors) all of the information in all of the original photographic prints except the Orion one is actually visible.</text>
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<text>Images obtenues par le Faint object Camera du téléscope Hubble Space.</text>
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<text>Imágenes realizadas por la Cámara para Objetos de Mínima Definición del Telescopio Hubble.</text>
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<text>Bilder von der Faint-Object Kamera des Hubble-Teleskops.</text>
<text> COMPARATIVE VIEW OF A STAR BEFORE AND AFTER THE INSTALLATION OF THE CORRECTIVE OPTICS SPACE TELESCOPE AXIAL REPLACEMENT (COSTAR) This pair of images of a single star, taken with the European Space Agency's Faint Object Camera (FOC), demonstrate that NASA's Hubble Space Telescope has been restored fully to its planned optical performance. The COSTAR mirrors remove the effect of spherical aberration in the HST's primary mirror. The FOC will now be able to observe extremely faint celestial objects with a clarity and sensitivity unmatched by ground-based telescopes. [left] An FOC image a star taken prior to the sts-61 space shuttle HST servicing mission that installed COSTAR. The broad halo (one arc second diameter) around the star is caused by scattered unfocussed starlight. Because of aberration, only a small fraction of the light is concentrated in the star's pinpoint image (.1 arc second diameter). [right] Following the installation, deployment, and alignment of COSTAR, the FOC met its pre-launch specifications. Most of the starlight is concentrated into a .1 arc second circle, and the blurry "skirt" of light is completely gone. By comparison, large ground based telescopes can concentrate 1/10th of starlight into an area smaller than one arc second, even under optimum observing condition. This clearly shows that the effects of spherical aberration have been successfully removed from the FOC. PHOTO RELEASE NO: STScI-PR94-08</text>
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<text>Vue comparative d'une étoile avant et après la réparation du téléscope Hubble.</text>
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<text>Una vista comparativa de una estrella tomada antes y después de la restauración del telescopio Hubble.</text>
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<text>Ein vergleichendes Bild von einem Stern, vor und nach der Hubblerestauration.</text>
<text> HUBBLE SEES CHANGES IN GAS SHELL AROUND NOVA CYGNI 1992 The European Space Agency's ESA Faint Object Camera utilizing the corrective optics provided by NASA's COSTAR (Corrective Optics Space Telescope Axial Replacement), has given astronomers their best look yet at a rapidly ballooning bubble of gas blasted off a star. The shell surrounds Nova Cygni 1992, which erupted on February 19, 1992. A nova is a thermonuclear explosion that occurs on the surface of a white dwarf star in a double star system. The new HST image [right] reveals an elliptical and slightly lumpy ring-like structure. The ring is the edge of a bubble of hot gas blasted into space by the nova. The shell is so thin that the FOC does not resolve its true thickness, even with HST's restored vision. An HST image taken on May 31 1993, [left] 467 days after the explosion, provided the first glimpse of the ring and a mysterious bar-like structure. But the image interpretation was severely hampered by HST's optical aberration, that scattered light from the central star which contaminated the ring's image. A comparison of the pre and post COSTAR/FOC images reveals that the ring has evolved in the seven months that have elapsed between the two observations. The ring has expanded from a diameter of approximately 74 to 96 billion miles. The bar-like structure seen in the earlier HST image has disappear. These changes might confirm theories that the bar was produced by a dense layer of gas thrown off in the orbital plane of the double star system. The gas has subsequently grown more tenuous and so the bar has faded. The ring has also grown noticeably more oblong since the earlier image. This suggests the hot gas is escaping more rapidly above and below the system's orbital plane. As the gas continues escaping the ring should grow increasingly egg-shaped in the coming years. HST's newly improved sensitivity and high resolution provides a unique opportunity to understand the novae by resolving the effects of the explosion long before they can be resolved in ground based telescopes. Nova Cygni is 10,430 light years away (as measured directly from the ring's diameter), and located in the summer constellation Cygnus the Swan. Credit: F. Paresce, R. Jedrzejewski (STScI) NASA/ESA PHOTO RELEASE NO.: STScI-PR94-06</text>
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<text>Image de Nova Cygni 1992 après explosion, montrant une barre de structure en expansion.</text>
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<text>Imagen de la nova Cygni 1992 después de una explosión, que muestra una estructura de barra en expansión.</text>
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<text>Bild von Nova Cygni 1992, post Explosion, mit einer sich ausdehnenden Stabstruktur.</text>
<text>HUBBLE UNCOVERS FAINT STARS IN THE CORE OF GLOBULAR CLUSTER 47 TUCANE These comparison images of the core of the globular cluster 47 Tucanae (NGC104) were taken with the COSTAR-corrected Faint Object Camera to show the improvement in performance when compared to images taken with the uncorrected camera. (left) The pre-COSTAR image was taken on 27 October 1993 using the F/96 mode. Even prior to the servicing mission this was considered an impressive HST image. The star density is high and none of the stars are bright enough to show the halo caused by a flaw in Hubble's primary mirror. (right) The COSTAR-corrected image was taken on 10th January 1994 reveals stellar images that are crisp and clean, and stellar magnitudes and colors can be accurately measured. (The pre-COSTAR image was rotated and magnified to match the scale and orientation of the COSTAR-corrected image, and both images are 14 arcseconds on a side). A preliminary analysis of the data reveals the apparent presence of white dwarf stars in the image. Prior to the Hubble observation white dwarfs have generally been too dim to be seen within such a cluster. A globular cluster is a tight aggregate of thousands to millions of very old stars. White dwarfs are the earth-sized remains of ordinary stars like the sun. Finding them in a known globular cluster allows accurate estimates of their age and provides clues to reconstructing their history. Credit: Dr. R. Jedrzejewski (STScI) NASA, ESA</text>
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<text>Etoile naine blanche dans le centre d'amas globulaire 47 Tucanae (NGC 104).</text>
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<text>Estrellas enanas blancas en el centro de la agrupaci├│n estelar 47 Tucunae (NGC 104).</text>
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<text>Weiße Zwergensterne im Kern der globulären Gruppe 47 Tucanae (NGC 104).</text>
<text> HST REVEALS THE CENTRAL REGION OF AN ACTIVE GALAXY The refurbished HST has provided this outstanding image of the nuclear region of the galaxy NGC1068. NGC1068 is located at a distance of approximately 60 Million Light Years and is the prototype of a class of galaxies, known as Seyfert Type 2. In active galaxies, typically the core shines with the brightness of a billion solar luminosities, and the brightness of the core fluctuates over the period of a few days implying that the energy is being released from a region only a few light-days in extent. The most likely source for this enormous amount of energy is a "super massive" black-hole with a total mass of 100 million stars like the Sun. In the case of NGC1068, previous HST observations (left) have shown a number of hot gaseous clouds ionized or heated by the intense radiation from the nuclear source. A torus of "donut" of opaque dust and gas orbiting the black hole confines escaping radiation to a diverging beam or "cone" of emission. The new FOC/COSTAR observations (right) show with unprecedented clarity a much more extensive area of emission, produced by radiation from the active nucleus. An incredible wealth of new and previously unsuspected filamentary detail is also revealed in this near-nuclear gas, embedded within the diffuse emission. The knots and streamers of emission will enable the geometry of this fascinating nuclear region to be understood, and will offer new information on the nature of the clouds themselves. A comparison between the ultraviolet light and the light emission of the clouds will provide insight into the hidden source of all the energy - perhaps an obscured black-hole. These data were taken by a team led by Duccio Macchetto of the European Space Agency (ESA) and Space Telescope Science Institute (STScI), and including William Sparks and Alessandro Capetti of STScI, using the Faint Object Camera and COSTAR "combination." PHOTO RELEASE NO.: STScI-PR94-07</text>
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<text>Région nucléaire de la galaxie NGC 1068 montrant des nuages de gaz ionisés par radiation.</text>
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<text>Regi├│n nuclear de la galaxia NGC 1068 que muestra nubes gaseosas ionizadas por la radiaci├│n.</text>
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<text>Kernregion der NGC 1068 Galaxis mit Gaswolken, durch Strahlung ionisiert.</text>
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<text>ª»™e®t™∫ NGC 1068 ™∫Æ÷§l™∫¶a∞œ≈„•‹∂≥¬«µ€øÁÆgΩu¬˜§l§∆™∫Æ≈È.</text>
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<text>El Espacio</text>
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<text>This is a mosaic of short-period comet Encke composed of images obtained by Jim Scotti on 1993 October 24.14, November 17.14, December 8.11 and 1994 January 5 while using the 0.91-meter Spacewatch Telescope on Kitt Peak. The image is 9.18 arcminutes by 6.92 arcminutes with north on the right and east at top. The integration time in each is 150 seconds.</text>
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<text>Image de comète de courte période Encke prise par Spacewatch Telescope sur Kitt Peak.</text>
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<text>Imagen de breve duraci├│n del cometa Encke tomado del telescopio Spacewatch en Kitt Peak.</text>
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<text>Kurzzeit Komet Encke, vom Spacewatch Teleskop auf Kitt Peak aufgenommen.</text>
<text>This is a mosaic of short-period comet Encke composed of images obtained by Jim Scotti on 1993 October 24.14, November 17.14, December 8.11 and 1994 January 5 while using the 0.91-meter Spacewatch Telescope on Kitt Peak. The image is 9.18 arcminutes by 6.92 arcminutes with north on the right and east at top. The integration time in each is 150 seconds.</text>
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<text>Image de comète de courte période Encke prise par Spacewatch Telescope sur Kitt Peak.</text>
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<text>Imagen de breve duraci├│n del cometa Encke tomado del telescopio Spacewatch en Kitt Peak.</text>
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<text>Kurzzeit Komet Encke, vom Spacewatch Teleskop auf Kitt Peak aufgenommen.</text>
<text>This is an image of short-period comet Encke obtained by Jim Scotti on 1994 January 5.09 while using the 0.91-meter Spacewatch Telescope on Kitt Peak. The image is 9.18 arcminutes square with north on the right and east at top. The integration time is 150 seconds.</text>
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<text>Image de comète de courte période Encke prise par Spacewatch Telescope sur Kitt Peak.</text>
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<text>Imagen de breve duraci├│n del cometa Encke tomado del telescopio Spacewatch en Kitt Peak.</text>
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<text>Kurzzeit Komet Encke, vom Spacewatch Teleskop auf Kitt Peak aufgenommen.</text>
<text>This is an image of short-period comet Encke obtained by Jim Scotti on 1993 December 8.11 while using the 0.91-meter Spacewatch Telescope on Kitt Peak. The image is 9.18 arcminutes square with north on the right and east at top. The integration time is 150 seconds.</text>
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<text>Image de comète de courte période Encke prise par Spacewatch Telescope sur Kitt Peak.</text>
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<text>Imagen de breve duraci├│n del cometa Encke tomado del telescopio Spacewatch en Kitt Peak.</text>
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<text>Kurzzeit Komet Encke, vom Spacewatch Teleskop auf Kitt Peak aufgenommen.</text>
<text>This is an image of short-period comet Encke obtained by Jim Scotti on 1993 November 17.14 while using the 0.91-meter Spacewatch Telescope on Kitt Peak. The image is 9.18 arcminutes square with north on the right and east at top. The integration time is 150 seconds.</text>
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<text>Image de comète de courte période Encke prise par Spacewatch Telescope sur Kitt Peak.</text>
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<text>Imagen de breve duraci├│n del cometa Encke tomado del telescopio Spacewatch en Kitt Peak.</text>
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<text>Kurzzeit Komet Encke, vom Spacewatch Teleskop auf Kitt Peak aufgenommen.</text>
<text>This is an image of short-period comet Encke obtained by Jim Scotti on 1993 October 24.14 while using the 0.91-meter Spacewatch Telescope on Kitt Peak. The image is 9.18 arcminutes square with north on the right and east at top. The integration time is 150 seconds.</text>
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<text>Image de comète de courte période Encke prise par Spacewatch Telescope sur Kitt Peak.</text>
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<text>Imagen de breve duraci├│n del cometa Encke tomado del telescopio Spacewatch en Kitt Peak.</text>
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<text>Kurzzeit Komet Encke, vom Spacewatch Teleskop auf Kitt Peak aufgenommen.</text>
<text>There are several astronomical images posted here. The pictures: dumbell (M27) horsehead M33 northamerica (NGC7000) orion (M42/M43) were taken by me and Scott Reid using my 8 inch Meade SCT scope. We used hypersensitized Ektar 1000 film. The exposures and development was as follows ("normal" development is 4.5 minutes at 38C) : Time(min) development(min) dumbell 50 6 horsehead 90 x 2 8 M33 75 x 2 6 northamerica 90 x 2 6 orion 35 5 The "x 2" means two negatives were taken and sandwiched together for printing. The pictures grlens r136 sn1987a were obtained by the Faint Object Camera of the Hubble Space Telescope and were obtained from the press office of NASA. Please read the file hubble.txt for lots of data about them. They are not copyright, but NASA asks that they not be use for advertizing. The pictures were digitized using a Microtek scanner on a Mac II. The tiff images were converted to gif on a PC. All these pictures are colormapped with a palette of 256 colors (only 225 of which are used). I use a gif display program for the PC called "picem" and a Video 7 super VGA card. With this setup (640x400x256 colors) all of the information in all of the original photographic prints except the Orion one is actually visible.</text>
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<text>Plusieurs images astronomiques, y compris photos du Hubble Telescope.</text>
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<text>Varias imágenes astronómicos inclusive de fotos tomadas del telescopio Hubble.</text>
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<text>Einige astronomische Bilder, die auch einige Hubblebilder einschließen.</text>
<text>Text message for GIF image CmtBorly.gif: This is a ccd image of Comet Borrelly (1994l) taken with an ST6 camera attached to a LX200 10" SCT. The image was taken by Doug Snyder (snyder@netcom.netcom.com) on the morning of 20 October 1994 at 1235 UT. The position of the comet at this time was 7h 9m 34s +8d 34m 46s. Some minor processing was performed on the image to increase the contrast and detail of the objects.</text>
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<text>Image de Comet Borrelly prise par Doug Snyder 10-20-94.</text>
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<text>Imagen del cometa Borrelly tomado por Doug Snyder 20.10.1994.</text>
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<text>Bild vom Kometen Borrelly, aufgenommen von Doug Snyder am 20.10.'94.</text>
<text>The glorious globular cluster 47 Tucanae lying in the Smaller Magellanic Cloud. This is second only to Omega Centauri in terms of magnificence. This photograph was taken with the 74 inch telescope, originally at the Radcliffe Observatory, near Pretoria and now located at the Sutherland station of the South African Astronomical Observatory. Scanned from a monochrome print using a black and white scanner and artificially colored by GR.</text>
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<text>Photo de l'amas globulaire Glorious 47 Tucanae dans un plus petit nuage Magellanic.</text>
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<text>Foto de la magnífica agrupación estelar globular 47 Tucanae en la Nube Magallánica Menor.</text>
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<text>Photo der Glorius globulären Gruppe 47 Tucanae in der kleinen Magellanwolke.</text>
<text>30 Doradus as photographed with the 74-inch reflector at the Radcliffe Observatory, Pretoria, South Africa. This observatory was closed down in the early 70's and the 74-inch telescope was removed to the Sutherland site of the South African Astronomical Observatory where it is currently the largest telescope. This picture was scanned from a monochrome photograph with a black and white scanner and artificially colored by GR.</text>
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<text>Photo avec un 74-inch réflecteur de 30 Doradus à l'Observatoire Radcliffe.</text>
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<text>Foto tomada de 30 Doradus en el observatorio de Radcliffe con el reflector de 74 pulgadas.</text>
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<text>Photo mit 74-inch Reflektoren von 30 Doradus des Radcliffe Observatorium.</text>
<text>Comet Halley as photographed at the South African Astronomical Observatory on 15 March 1986 using an 11- inch schmidt camera on loan from the University of Perugia, Italy. This file was scanned from a monochrome print using a black/white scanner and artificially colored by GR.</text>
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<text>Comet Halley prise en photo à l'Observatoire Astronomique d'Afrique du Sud le 15 mars 1986.</text>
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<text>El cometa de Halley en el Observatorio Astron├│mico de Sud-Africa, 15 de marzo, 1986.</text>
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<text>Halley'scher Komet von dem s├╝dafrikanischem Observatorium am 15.3.'86 aufgenommen.</text>
<text>Umbriel (A Satellite of Uranus) The full size image of Umbriel is 101 KB. Last updated January 9, 1995 Constants MEAN RADIUS: 584.7 km MASS: 0.00022 (Earth=1) DENSITY: 1.52 (gm/cm) GRAVITY: 0.022 (Earth=1) ORBIT PERIOD: 4.144 (Earth days) ROTATION PERIOD: 4.144 (Earth days) SEMIMAJOR AXIS OF ORBIT: 267,000 km ECCENTRICITY OF ORBIT: 0.005</text>
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<text>Vue d'Umbriel, un satellite d'Uranus.</text>
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<text>Vista de Umbriel, satélite de Urano.</text>
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<text>Blick auf Umbriel, ein Uranus-Satellit.</text>
<text>View of Triton, a satellite of Neptune.</text>
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<text>äCâ§êØÇÃâqê؃ÿƒ›</text>
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<text>Triton (A Satellite of Neptune) The full size image of Triton is 145 KB. Last updated January 9, 1995 Constants MEAN RADIUS: 1352.6 km MASS: 0.0056 (Earth=1) DENSITY: (2.0) (gm/cm) GRAVITY: (0.077) (Earth=1) ORBIT PERIOD: 5.88 (Earth days) ROTATION PERIOD: 5.88 (Earth days) SEMIMAJOR AXIS OF ORBIT: 355,000 km ECCENTRICITY OF ORBIT: 0.000</text>
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<text>Vue de Triton, un satellite de Neptune.</text>
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<text>Vista de Tritón, satélite de Neptuno.</text>
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<text>Blick auf Triton, ein Neptun-Satellit.</text>
<text>Titania (A Satellite of Uranus) The full size image of Titania is 186 KB. Last updated January 9, 1995 Constants MEAN RADIUS: 788.9 km MASS: 0.00058 (Earth=1) DENSITY: 1.70 (gm/cm) GRAVITY: 0.029 (Earth=1) ORBIT PERIOD: 8.706 (Earth days) ROTATION PERIOD: 8.706 (Earth days) SEMIMAJOR AXIS OF ORBIT: 438,000 km ECCENTRICITY OF ORBIT: 0.002</text>
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<text>Image de Titania, un satellite d'Urans.</text>
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<text>Imagen de Titania, satélite de Urano.</text>
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<text>Blick auf Titania, ein Satellit des Saturn.</text>
<text>Titan (A Satellite of Saturn) The full size image of Titan is 84 KB. Last updated January 9, 1995 Constants MEAN RADIUS: 2575 km MASS: 0.0226 (Earth=1) DENSITY: 1.88 (gm/cm) GRAVITY: 0.138 (Earth=1) ORBIT PERIOD: 15.945 (Earth days) ROTATION PERIOD: 15.945 (Earth days) SEMIMAJOR AXIS OF ORBIT: 1,221,860 km ECCENTRICITY OF ORBIT: 0.029</text>
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<text>Image de Titan, un satellite de Saturne.</text>
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<text>Imagen de Titan, satélite de Saturno.</text>
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<text>Blick auf Titan, ein Satellit des Saturn.</text>
<text>Tethys (A Satellite of Saturn) The full size image of Tethys is 95 KB. Last updated January 9, 1995 Constants MEAN RADIUS: 523 km MASS: 0.000126 (Earth=1) DENSITY: 1.21 (gm/cm) GRAVITY: 0.018 (Earth=1) ORBIT PERIOD: 1.888 (Earth days) ROTATION PERIOD: 1.888 (Earth days) SEMIMAJOR AXIS OF ORBIT: 294,670 km ECCENTRICITY OF ORBIT: (0)</text>
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<text>Image de Tethys, un satellite de Saturne.</text>
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<text>Imagen de Tethys, satélite de Saturno.</text>
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<text>Bild von Tethys, ein Saturn-Satellit.</text>
<text>Rhea (A Satellite of Saturn) The full size image of Rhea is 188 KB. Last updated January 9, 1995 Constants MEAN RADIUS: 764 km MASS: 0.000416 (Earth=1) DENSITY: 1.33 (gm/cm) GRAVITY: 0.029 (Earth=1) ORBIT PERIOD: 4.518 (Earth days) ROTATION PERIOD: 4.518 (Earth days) SEMIMAJOR AXIS OF ORBIT: 527,100 km ECCENTRICITY OF ORBIT: 0.001</text>
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<text>Vue de Rhea, un satellite de Saturne.</text>
<text>PHOTOMOSAIC OF PHOBOS Phobos.gif is a photomosaic of Phobos, the inner satellite of Mars. The original mosaic, at much higher resolution than shown here, was prepared by Peter Thomas, Damon Simonelli and colleagues at Cornell University. It was published in cylindrical and sinusoidal map projections in: Simonelli. D.P., Thomas, P.C., Carcich, B.T. and Veverka, J., 1993. "The Generation and Use of Numerical Shape Models for Irregular Solar System Objects", ICARUS, V. 103, pp. 49-61. and is also discussed in: Thomas, P.C., 1993. "Gravity, Tides, and Topography on Small Satellites and Asteroids: Application to Surface Features of the Martian Satellites", ICARUS, V. 105, pp. 326-344, 1993. Positions in the mosaic are controlled by a new shape model, described in those papers. A print of the cylindrical projection was kindly provided by D. Simonelli, and the digital shape data by P. Thomas. I filled small gaps in the mosaic using additional Viking images. For the image presented here, the three dimensional convex hull of the shape model was projected into the Morphographic Conformal Projection (the conventional Stereographic Projection modified for non-spherical worlds). The cylindrical projection mosaic was scanned and reprojected to fit the Morphographic grid. A higher resolution version of this map with latitude-longitude grid and feature names will be published in 1995. The leading side (longitude 90 runs vertically down the centre) faces forwards in the orbit of Phobos. The trailing side (longitude 270 runs vertically down its centre) faces backwards along the orbit. Longitude 0 is at the more sharply rounded end with the most prominent grooves, and faces Mars. As with all conformal (true shape) projections, the scale in these maps varies, increasing from the centre to the outer edge. The map projection is described in: Stooke, P.J. and Keller, C.P., 1990. "Map Projections for Non-Spherical Worlds / the Variable-Radius Map Projections", CARTOGRAPHICA, V. 27, No. 2, pp. 82-100.</text>
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<text>Photomosaïque de Phobos, satellite intérieur de Mars scanné et reprojeté.</text>
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<text>Fotomosaico de Phobos, satélite interior de Marte escandido y reproyectado.</text>
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<text>Phobos, innerer Mars-Satellit, abgetastet und reproduziert.</text>
<text>Oberon (A Satellite of Uranus) The full size image of Oberon is 175 KB. Last updated January 9, 1995 Constants MEAN RADIUS: 761.4 km MASS: 0.00051 (Earth=1) DENSITY: 1.64 (gm/cm) GRAVITY: 0.028 (Earth=1) ORBIT PERIOD: 13.463 (Earth days) ROTATION PERIOD: 13.463 (Earth days) SEMIMAJOR AXIS OF ORBIT: 387,000 km ECCENTRICITY OF ORBIT: 0.001</text>
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<text>Image d'Oberon, un satellite d'Uranus.</text>
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<text>Imagen de Oberón, satélite de Urano.</text>
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<text>Blick auf Oberon, ein Satellit des Uranus.</text>
<text>SHADED RELIEF MAP OF JANUS Janus.gif is a shaded relief map of Janus, the larger co-orbital satellite of Saturn. As with all maps, it is the cartographer's interpretation and not all features are necessarily certain given the limited data available - this interpretation stretches the data as far as is feasible. The original map was published in its full form with latitude-longitude grid, in: Stooke, P.J. and Lumsdon, M.P., 1993. "The Topography of Janus", EARTH, MOON AND PLANETS, V. 62, pp. 223-237. Positions in the map are controlled by a digital shape model, described in that paper. For this map, the three dimensional convex hull of the shape model was projected into the Morphographic Conformal Projection (the conventional Stereographic Projection modified for non-spherical worlds). The leading side (longitude 90 runs vertically down the centre) faces forwards in the orbit of Janus. The trailing side (longitude 270 runs vertically down its centre) faces backwards along the orbit. Longitude 0 is at the righthand end of the leading side, and faces Saturn. As with all conformal (true shape) projections, the scale in these maps varies, increasing from the centre to the outer edge. The map projection is described in: Stooke, P.J. and Keller, C.P., 1990. "Map Projections for Non-Spherical Worlds / the Variable-Radius Map Projections", CARTOGRAPHICA, V. 27, No. 2, pp. 82-100.</text>
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<text>Carte à relief ombragé de Janus, le plus grand satellite co-orbital de Saturne.</text>
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<text>Mapa de relieve sombreado de Janus, satélite mayor co-orbital de Saturno.</text>
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<text>Eine schattierte Reliefkarte von Janus, der größere co-Orbital Satellit von Saturn.</text>
<text>Io (A Satellite of Jupiter) The full size image of Io is 80 KB. Last Updated January 9, 1995 Constants MEAN RADIUS: 1830 km MASS: 0.0149 (Earth=1) DENSITY: 3.55 (gm/cm) GRAVITY: 0.138 (Earth=1) ORBIT PERIOD: 1.769 (Earth days) ROTATION PERIOD: 1.769 (Earth days) SEMIMAJOR AXIS OF ORBIT: 422,600 km ECCENTRICITY OF ORBIT: 0.004</text>
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<text>Image d'Io, un satellite de Jupiter.</text>
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<text>Imagen de Io, satélite de Júpiter.</text>
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<text>Bild von Io, ein Satellit von Jupiter.</text>
<text>Iapetus (A Satellite of Saturn) The full size image of Iapetus is 120 KB. Last Updated January 9, 1995 Constants MEAN RADIUS: 718 km MASS: 0.000314 (Earth=1) DENSITY: 1.16 (gm/cm) GRAVITY: 0.024 (Earth=1) ORBIT PERIOD: 79.331 (Earth days) ROTATION PERIOD: 79.331 (Earth days) SEMIMAJOR AXIS OF ORBIT: 3,560,800 km ECCENTRICITY OF ORBIT: 0.028</text>
<text>Ganymede (A Satellite of Jupiter) The full size image of Ganymede is 247 KB. Last Updated January 9, 1995 Constants MEAN RADIUS: 2634 km MASS: 0.0175 (Earth=1) DENSITY: 1.93 (gm/cm) GRAVITY: 0.145 (Earth=1) ORBIT PERIOD: 7.155 (Earth days) ROTATION PERIOD: 7.155 (Earth days) SEMIMAJOR AXIS OF ORBIT: 1,070,00 km ECCENTRICITY OF ORBIT: 0.002</text>
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<text>Vue de Ganymede, un satellite de Jupiter.</text>
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<text>Vista de Ganímedes, satélite de Júpiter.</text>
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<text>Blick auf Ganymede, ein Satellit von Jupiter.</text>
<text>View of Europa, a satellite of Jupiter.</text>
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<text>ñÿêØÇÃâqêØ•¥≥€ fl</text>
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<text>Europa (A Satellite of Jupiter) The full size image of Europa is 81 KB. Last Updated January 9, 1995 Constants MEAN RADIUS: 1565 km MASS: 0.0081 (Earth=1) DENSITY: 3.04 (gm/cm) GRAVITY: 0.138 (Earth=1) ORBIT PERIOD: 3.551 (Earth days) ROTATION PERIOD: 3.551 (Earth days) SEMIMAJOR AXIS OF ORBIT: 670,900 km ECCENTRICITY OF ORBIT: 0.009</text>
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<content>
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<text>Vue d'Europa, un satellite de Jupiter.</text>
</content>
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<text>Vista de Europa, satélite de Júpiter.</text>
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<text>Blick auf Europa, ein Satellit von Jupiter.</text>
<text>SHADED RELIEF MAP OF EPIMETHEUS Epimethe.gif is a shaded relief map of Epimetheus, the smaller co-orbital satellite of Saturn. As with all maps, it is the cartographer's interpretation and not all features are necessarily certain given the limited data available - this interpretation stretches the data as far as is feasible. The original map was published in its full form with latitude-longitude grid, in: Stooke, P.J., 1993. "The Topography of Epimetheus", EARTH, MOON AND PLANETS, V. 63, pp. 67-83. Positions in the map are controlled by a digital shape model, described in that paper. For this map, the three dimensional convex hull of the shape model was projected into the Morphographic Conformal Projection (the conventional Stereographic Projection modified for non-spherical worlds). The leading side (longitude 90 runs vertically down the centre) faces forwards in the orbit of Epimetheus. The trailing side (longitude 270 runs vertically down its centre) faces backwards along the orbit. Longitude 0 is at the righthand end of the leading side, and faces Saturn. As with all conformal (true shape) projections, the scale in these maps varies, increasing from the centre to the outer edge. The map projection is described in: Stooke, P.J. and Keller, C.P., 1990. "Map Projections for Non-Spherical Worlds / the Variable-Radius Map Projections", CARTOGRAPHICA, V. 27, No. 2, pp. 82-100.</text>
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<text>Carte à relief ombragé d'Epimetheurs, le plus petit satellite co-orbital de Saturne.</text>
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<text>Mapa de relieve sombreado de Epimethus, satélite menor co-orbital de Saturno.</text>
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<text>Schattierte Reliefkarte von Epimetheus, dem kleineren co-Orbital Satellit von Saturn.</text>
<text>Dione (A Satellite of Saturn) The full size image of Dione is 69 KB. Last Updated January 9, 1995 Constants MEAN RADIUS: 560 km MASS: 0.000176 (Earth=1) DENSITY: 1.43 (gm/cm) GRAVITY: 0.023 (Earth=1) ORBIT PERIOD: 2.737 (Earth days) ROTATION PERIOD: 2.737 (Earth days) SEMIMAJOR AXIS OF ORBIT: 377,420 km ECCENTRICITY OF ORBIT: 0.002</text>
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<text>Image de Dione, un satellite de Saturne.</text>
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<text>Imagen de Dion, satélite de Saturno.</text>
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<text>Bild von Dione, ein Satellit des Saturns.</text>
<text>PHOTOMOSAIC OF DEIMOS Deimos.gif is a photomosaic of Deimos, the outer satellite of Mars. The original mosaic, at much higher resolution than shown here, was prepared by Peter Thomas and colleagues at Cornell University. It was published in a cylindrical map projection in: Thomas, P.C., 1993. "Gravity, Tides, and Topography on Small Satellites and Asteroids: Application to Surface Features of the Martian Satellites", ICARUS, V. 105, pp. 326-344, 1993. Positions in the mosaic are controlled by a new shape model, discussed in that paper. A print of the cylindrical projection and the digital shape data were kindly provided by P. Thomas. I have used Viking and Mariner 9 images to fill a large gap in the published mosaic. This required small changes to the shape model, and the positional accuracy of the mosaic in this region (longitudes 300 to 350 degrees, left-hand side of the lower image) is not as great as in the rest of the mosaic. For the image presented here, the three dimensional convex hull of the shape model was projected into the Morphographic Conformal Projection (the conventional Stereographic Projection modified for non-spherical worlds). The cylindrical projection mosaic was scanned and reprojected to fit the Morphographic grid. A higher resolution version of this map with latitude-longitude grid and feature names will be published in 1995. The leading side (longitude 90 runs vertically down the centre) faces forwards in the orbit of Deimos. The trailing side (longitude 270 runs vertically down its centre) faces backwards along the orbit. Longitude 0 is at the blunter end with the most prominent craters, and faces Mars. As with all conformal (true shape) projections, the scale in these maps varies, increasing from the centre to the outer edge. The map projection is described in: Stooke, P.J. and Keller, C.P., 1990. "Map Projections for Non-Spherical Worlds / the Variable-Radius Map Projections", CARTOGRAPHICA, V. 27, No. 2, pp. 82-100.</text>
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<text>Une photomosaïque de Deimos, le satellite extérieur de Mars.</text>
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<text>Fotomosaico de Deimos, satélite exterior de Marte.</text>
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<text>Ein Photomosaik von Deimos, der äßere Satellit von Mars.</text>
<text>Calisto (A Satellite of Jupiter) The full size image of Calisto is 188 KB. Last Updated January 9, 1995 Constants MEAN RADIUS: 3404 km MASS: 0.0179 (Earth=1) DENSITY: 1.81 (gm/cm) GRAVITY: 0.124 (Earth=1) ORBIT PERIOD: 16.689 (Earth days) ROTATION PERIOD: 16.689 (Earth days) SEMIMAJOR AXIS OF ORBIT: 1,883,000 km ECCENTRICITY OF ORBIT: 0.007</text>
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<text>Image de Callisto.</text>
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<text>Imagen de Calisto.</text>
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<text>Bild von Callisto.</text>
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<text>Callisto ™∫πœπ≥.</text>
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<text>Satélite</text>
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card_53812.xml
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<text>Ariel (A Satellite of Uranus) The full size image of Ariel is 103 KB. Last Updated January 9, 1995 Constants MEAN RADIUS: 578.9 km MASS: 0.00021 (Earth=1) DENSITY: 1.56 (gm/cm) GRAVITY: 0.021 (Earth=1) ORBIT PERIOD: 2.520 (Earth days) ROTATION PERIOD: 2.520 (Earth days) SEMIMAJOR AXIS OF ORBIT: 192,000 km ECCENTRICITY OF ORBIT: 0.003</text>
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<text>Image d'Ariel, un satellite d'Uranus. Dernier mise-à-jour 1-9-95.</text>
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<text>Imagen de Ariel, satélite de Urano. Ultima actualización 9.1.1995</text>
<text>SHADED RELIEF MAP OF AMALTHEA Amalthea.gif is a shaded relief map of Amalthea, a small satellite of Jupiter. As with all maps, it is the cartographer's interpretation and not all features are necessarily certain given the limited data available - this interpretation stretches the data as far as is feasible. The original map was published in its full form with latitude-longitude grid and feature names, in: Stooke, P.J., 1994. "The Geology of Amalthea", EARTH, MOON AND PLANETS V. 64, pp. 187-197. Positions in the map are controlled by a digital shape model, described in that paper. For this map, the three dimensional convex hull of the shape model was projected into the Morphographic Conformal Projection (the conventional Stereographic Projection modified for non-spherical worlds). The leading side (longitude 90 runs vertically down the centre) faces forwards in the orbit of Amalthea. The trailing side (longitude 270 runs vertically down its centre) faces backwards along the orbit. Longitude 0 is at the righthand end of the leading side, and faces Jupiter. As with all conformal (true shape) projections, the scale in these maps varies, increasing from the centre to the outer edge. The map projection is described in: Stooke, P.J. and Keller, C.P., 1990. "Map Projections for Non-Spherical Worlds / the Variable-Radius Map Projections", CARTOGRAPHICA, V. 27, No. 2, pp. 82-100.</text>
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<text>Carte à relief ombragé d'Amalthea, un petit satellite de Jupiter.</text>
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<text>Mapa de relieve sombreado de Amalthea, pequeño satélite de Júpiter.</text>
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<text>Eine schattierte Relierkarte von Amalthea, ein kleiner Satellit vom Jupiter.</text>
<text>PUBLIC INFORMATION OFFICE JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109. (818) 354-5011 PHOTO CAPTION (TOP) P-41525 January 4, 1993 Toutatis Radar Images These are radar images of asteroid 4179 Toutatis made during the object's recent close approach to Earth. The images reveal two irregularly shaped, cratered objects about 4 and 2.5 kilometers (2.5 and 1.6 miles) in average diameter which are probably in contact with each other. The four frames shown here (from left to right) were obtained on Dec. 8, 9, 10 and 13 when Toutatis was an average of about 4 million kilometers (2.5 million miles) from Earth. The time required to obtain each of these images was 55, 14, 37 and 85 minutes, respectively. On each day, the asteroid was in a different orientation with respect to Earth. In these images, the radar illumination comes from the top of the page, so parts of each component facing toward the bottom are not seen. The large crater shown in the Dec. 9 image (upper right) is about 700 meters (2,300 feet) in diameter. The radar observations were carried out at the Goldstone Deep Space Communications Complex in California's Mojave desert by a team led by Dr. Steven Ostro of JPL. For most of the work, a 400,000-watt coded radio transmission was beamed at Toutatis from the Goldstone main 70-meter (230-foot) antenna. The echoes, which took as little as 24 seconds to travel to Toutatis and back, were received by the new 34-meter (112-foot) antenna and relayed back to the 70-meter station where they were decoded and processed into images. The radar observations were part of the Planetary Astronomy Program of NASA's Office of Space Science and Applications. #####</text>
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<text>Images radar de l'astéroïde 4179 Toutatis au moment de son approche vers la Terre.</text>
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<text>Imágenes de radar del asteroide 4179 Toutatis durante su aproximación cercana a la tierra.</text>
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<text>Radarbild des Asteroiden 4179 Toutatis während seiner Näherung zur Erde.</text>
<text>SHADED RELIEF MAP OF PROTEUS, CYLINDRICAL PROJECTION Proteus2.gif is a shaded relief map of Proteus, a small inner satellite of Neptune. As with all maps, it is the cartographer's interpretation and not all features are necessarily certain given the limited data available - this interpretation stretches the data as far as is feasible. A small part of this map was published in: Stooke, P.J., 1994. "The Surfaces of Larissa and Proteus", EARTH, MOON AND PLANETS, V. 65, pp. 31-54. Positions in the map are controlled by a digital shape model, described in that paper. For this map, the three dimensional convex hull of the shape model was projected into the Morphographic Conformal Projection (the conventional Stereographic Projection modified for non-spherical worlds). The map was compiled in that projection and reprojected to the Simple Cylindrical projection. Longitude 0 is at the center of the map and faces Neptune. As with all cylindrical projections, this map is severely distorted near the poles (top and bottom edges).</text>
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<text>Carte à relief ombragé de Proteus, un petit satellite intérieur de Neptune.</text>
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<text>Mapa de relieve sombreado de Próteo, satélite menor interior de Neptuno.</text>
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<text>Schattierte Reliefkarte von Prometheus, der Hirtensatellit vom inneren F Ring, Saturn.</text>
<text>SHADED RELIEF MAP OF PROTEUS Proteus.gif is a shaded relief map of Proteus, a small inner satellite of Neptune. As with all maps, it is the cartographer's interpretation and not all features are necessarily certain given the limited data available - this interpretation stretches the data as far as is feasible. The original map was published in its full form with latitude-longitude grid and feature names, in: Stooke, P.J., 1994. "The Surfaces of Larissa and Proteus", EARTH, MOON AND PLANETS, V. 65, pp. 31-54. Positions in the map are controlled by a digital shape model, described in that paper. For this map, the three dimensional convex hull of the shape model was projected into the Morphographic Conformal Projection (the conventional Stereographic Projection modified for non-spherical worlds). The leading side (longitude 90 runs vertically down the centre) faces forwards in the orbit of Proteus. The trailing side (longitude 270 runs vertically down its centre) faces backwards along the orbit. Longitude 0 is at the righthand end of the leading side, and faces Neptune. As with all conformal (true shape) projections, the scale in these maps varies, increasing from the centre to the outer edge. The map projection is described in: Stooke, P.J. and Keller, C.P., 1990. "Map Projections for Non-Spherical Worlds / the Variable-Radius Map Projections", CARTOGRAPHICA, V. 27, No. 2, pp. 82-100.</text>
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<text>Carte à relief ombragé de Proteus, un petit satellite intérieur de Neptune.</text>
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<text>Mapa de relieve sombreado de Próteo, satélite menor interior de Neptuno.</text>
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<text>Schattierte Reliefkarte von Prometheus, der Hirtensatellit vom inneren F Ring, Saturn.</text>
<text>SHADED RELIEF MAP OF PROMETHEUS Promethe.gif is a shaded relief map of Prometheus, the inner F Ring Shepherd satellite of Saturn. As with all maps, it is the cartographer's interpretation and not all features are necessarily certain given the limited data available - this interpretation stretches the data as far as is feasible. The original map was published in its full form with latitude-longitude grid, in: Stooke, P.J., 1993. "The Shapes and Surface Features of Prometheus and Pandora", EARTH, MOON AND PLANETS, V. 62, pp. 199-221. Positions in the map are controlled by a digital shape model, described in that paper. For this map, the three dimensional convex hull of the shape model was projected into the Morphographic Conformal Projection (the conventional Stereographic Projection modified for non-spherical worlds). The leading side (longitude 90 runs vertically down the centre) faces forwards in the orbit of Prometheus. The trailing side (longitude 270 runs vertically down its centre) faces backwards along the orbit. Longitude 0 is at the righthand end of the leading side, and faces Saturn. As with all conformal (true shape) projections, the scale in these maps varies, increasing from the centre to the outer edge. The map projection is described in: Stooke, P.J. and Keller, C.P., 1990. "Map Projections for Non-Spherical Worlds / the Variable-Radius Map Projections", CARTOGRAPHICA, V. 27, No. 2, pp. 82-100.</text>
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<text>Carte à relief ombragé de Prometheus, le satellite F Ring Shepherd intérieur de Saturne.</text>
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<text>Mapa de relieve sombreado de Prometeo, anillo F interior satélite Pastor de Saturno.</text>
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<text>Schattierte Reliefkarte von Prometheus, der Hirtensatellit vom inneren F Ring, Saturn.</text>
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<text>Prometheus ™∫≥±∑t¨Ô¥°¶aπœ,§∫≥° F ≥Ú¬∂§g¨P™∫ Shepherd Ω√¨P.</text>
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<text>Astro Peque├▒o</text>
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card_47775.xml
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<text>PUBLIC INFORMATION OFFICE JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109. TELEPHONE (818) 354-5011 PHOTO CAPTION GALILEO December 1, 1992 P-41382 TOP GLL/GA7 This montage shows asteroid 951 Gaspra (top) compared with Deimos (lower left) and Phobos (lower right), the moons of Mars. The three bodies are shown at the same scale and nearly the same lighting conditions. Gaspra is about 17 kilometers (10 miles) long. All three bodies have irregular shapes, due to past catastrophic conditions. However their surfaces appear remarkably different, possibly because of differences in composition but most likely because of very different impact histories. The Phobos and Deimos images were obtained by the Viking Orbiter spacecraft in 1977; the Gaspra image is the best of a series obtained by the Galileo spacecraft on October 29, 1991. Galileo is scheduled to add the detailed view of another asteroid when it flies by Ida in August 1993. The Galileo project, whose primary mission is the exploration of the Jupiter system in 1995-97, is managed for NASA's Office of Space Science and Applications by the Jet Propulsion Laboratory. #####</text>
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<text>Montage comparant Gaspra, Deimos et Phobos à l'aide de la même échelle et du même éclairage.</text>
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<text>Montage comparando Gaspra, Deimos y Phobos con la misma escala e iluminaci├│n.</text>
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<id>30</id>
<text>Montage, die Gaspra, Deimos und Phobos mit dem gleichen Maßstab und Belichtung vergleichen.</text>
<text>PUBLIC INFORMATION OFFICE JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109. TELEPHONE (818) 354-5011 PHOTO CAPTION GALILEO December 1, 1992 P-41383 TOP GLL/GA6 This montage of 11 images taken by the Galileo spacecraft as it flew by the asteroid Gaspra on October 29, 1991, shows Gaspra growing progressively larger in the field of view of Galileo's solid-state imaging camera as the spacecraft approached the asteroid. Sunlight is coming from the right. Gaspra is roughly 17 kilometers (10 miles) long, 10 kilometers (6 miles) wide. The earliest view (upper left) was taken 5 3/4 hours before closest approach when the spacecraft was 164,000 kilometers (102,000 miles) from Gaspra, the last (lower right)at a range of 16,000 kilometers (10,000 miles), 30 minutes before closest approach. Gaspra spins once in roughly 7 hours, so these images capture almost one full rotation of the asteroid. Gaspra spins counterclockwise; its north pole is to the upper left, and the "nose" which points upward in the first image, is seen rotating back into shadow, emerging at lower left, and rotating to upper right. Several craters are visible on the newly seen sides of Gaspra, but none approaches the scale of the asteroid's radius. Evidently, Gaspra lacks the large craters common on the surfaces of many planetary satellites, consistent with Gaspra's comparatively recent origin from the collisional breakup of a larger body. The Galileo project, whose primary mission is the exploration of the Jupiter system in 1995-97, is managed for NASA's Office of Space Science and Applications by the Jet Propulsion Laboratory. #####</text>
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<text>Montage de 11 images prises par le Galileo lorsqu'il vola près de l'astéroïde Gaspra.</text>
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<text>Montage de 11 imágenes tomadas por Galileo al sobrevolar el asteroide Gaspra.</text>
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<text>Montage mit 11 Bildern von Asteroid Gaspra, aufgenommen von Galileo.</text>
<text>SHADED RELIEF MAP OF ASTEROID 4769 CASTALIA Castalia.gif is a shaded relief map of asteroid 4769 Castalia, previously known as 1989 PB. As with all maps, it is the cartographer's interpretation and not all features are necessarily certain given the limited data available - this interpretation stretches the data as far as is feasible. This map has not yet been published. Castalia was discovered by E. Helin on 9 August 1989, and imaged at very low resolution by delay-doppler radar at Goldstone and Arecibo later in August 1989. Images are described in: Ostro, S.J., Chandler, J.F., Hine, A.A., Rosema, K.D., Shapiro, I.I. and Yeomans, D.K., 1990. "Radar Images of Asteroid 1989 PB". SCIENCE, v. 248, pp. 1523-1528. A spherical harmonic model of the shape of Castalia was derived from the radar images and is described in: Hudson, R.S. and Ostro, S.J., 1994. "Shape of Asteroid 4769 Castalia (1989 PB) from Inversion of Radar Images". SCIENCE, v. 263, pp. 940- 943. I used the published rendered images of that shape model to derive a digital shape model (radii at regular increments of latitude and longitude). The digital model was constrained by the positions of edges and other features in the rendered images, as if they were limbs in spacecraft images. Positions in the map are controlled by the digital shape model. For this map, the three dimensional convex hull of the shape model was projected into the Morphographic Conformal Projection (the conventional Stereographic Projection modified for non-spherical worlds). Longitudes are arbitrary, but for consistency with maps of other small bodies the prime meridian (longitude 0) has been placed at one end of the elongated body. This is 60 degrees west of the prime meridian as defined by Hudson and Ostro. As with all conformal (true shape) projections, the scale in these maps varies, increasing from the centre to the outer edge. Because the model is represented as its convex hull, the deep valley separating two lobes of the asteroid is shown only by shading. Surface features are based on the rendered images, and the 'dimples' are not necessarily to be considered as impact craters, though some probably are. The map projection is described in: Stooke, P.J. and Keller, C.P., 1990. "Map Projections for Non-Spherical Worlds / the Variable-Radius Map Projections", CARTOGRAPHICA, V. 27, No. 2, pp. 82-100.</text>
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<text>Carte à relief ombragé de l'astéroïde 4769 Castalia découvert par E. Helin 8-9-89.</text>
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<text>Mapa de relieve sombreado del asteroide 4769 Castalia descubierto por E. Helin el 9.8.89.</text>
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<text>Schtattierte Reliefkarte vom Asteroiden 4769, von E. Helin am 9.8.'89 entdeckt.</text>
<text>Annular Eclipse Info Although there were partly cloudy skies during most of the eclipse, most of the scientific objectives were successfully obtained while the Sun was in a clear area of the sky (about 70% of the time). Several preliminary images are available here. disk_ha.gif is time series of H-alpha images that were digitized from a video tape of the CCD video camera on the Flare</text>
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<text>Image de l'éclipse annulaire montrant un limbre lunaire et un limbre solaire éclipsés.</text>
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<text>Imágenes de eclipse anular que muestra los miembros solares y lunares.</text>
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<text>Bilder von der jährlichen Verfinsterung, mit verfinstertem Sonnen- und Mond-limb.</text>
<text>Annular Eclipse Info Although there were partly cloudy skies during most of the eclipse, most of the scientific objectives were successfully obtained while the Sun was in a clear area of the sky (about 70% of the time). Several preliminary images are available here. disk_ha.gif is time series of H-alpha images that were digitized from a video tape of the CCD video camera on the Flare</text>
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<text>Image de l'éclipse annulaire montrant un limbre lunaire et un limbre solaire éclipsés.</text>
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<text>Imágenes de eclipse anular que muestra los miembros solares y lunares.</text>
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<text>Bilder von der jährlichen Verfinsterung, mit verfinstertem Sonnen- und Mond-limb.</text>
<text>From: Gary Kronk <C09630GK@wuvmd.wustl.edu> Organization: Washington University, St. Louis Someone recently asked if satellite photos of the eclipse had ever been obtained. Well, if you can ftp to various sites, try VMD.SCO.UIUC.EDU (or 128.174.5.98) and there are five files by a weather satellite which show the moon's shadow moving across the Pacific, into Mexico, and into the Gulf of Mexico. The files are GIFs and each is nearly 400K. They are 1200x600 and 256 shades of gray. The moon's shadow is very distinct. Gary W. Kronk C09630GK@WUVMD.WUSTL.EDU =========================================================================== ===== From: cloister@milton.u.washington.edu (cloister bell) Organization: University of Washington there are 5 pictures of what i believe to be this eclipse available for anonymous ftp from vmd.cso.uiuc.edu in the PHIL.515 directory. this is a ibm vm/cms site, so it's version of ftp may be a little different than you're used to. the images are labeled solar17z.gif thru solar20z.gif. they appear to be taken an hour apart each. these are 1200x600 gif files, with 64 level grayscale. -- +-------------------------------------------------+---------------------------+ |i thought of a good sig, but it was a sight gag. | cloister@u.washington.edu | +-------------------------------------------------+---------------------------+ =========================================================================== ===== From: cloister@milton.u.washington.edu (cloister bell) Organization: University of Washington oh, i should mention that these are sattelite photos of the earth, not ground-based photos of the sun. all in all, though, it looks like a big hole in the world. -- +-------------------------------------------------+---------------------------+ |i thought of a good sig, but it was a sight gag. | cloister@u.washington.edu | +-------------------------------------------------+---------------------------+</text>
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<text>Photos satellites de la terre au moment d'une éclipse, montrant l'ombre de la lune.</text>
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<text>Fotos de satélite de la tierra durante un eclipse que muestra la sombra de la luna.</text>
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<text>Satellitenphotos von der Erde, mit Schatten vom Mond, während einer Vefinsterung.</text>
<text>From: Gary Kronk <C09630GK@wuvmd.wustl.edu> Organization: Washington University, St. Louis Someone recently asked if satellite photos of the eclipse had ever been obtained. Well, if you can ftp to various sites, try VMD.SCO.UIUC.EDU (or 128.174.5.98) and there are five files by a weather satellite which show the moon's shadow moving across the Pacific, into Mexico, and into the Gulf of Mexico. The files are GIFs and each is nearly 400K. They are 1200x600 and 256 shades of gray. The moon's shadow is very distinct. Gary W. Kronk C09630GK@WUVMD.WUSTL.EDU =========================================================================== ===== From: cloister@milton.u.washington.edu (cloister bell) Organization: University of Washington there are 5 pictures of what i believe to be this eclipse available for anonymous ftp from vmd.cso.uiuc.edu in the PHIL.515 directory. this is a ibm vm/cms site, so it's version of ftp may be a little different than you're used to. the images are labeled solar17z.gif thru solar20z.gif. they appear to be taken an hour apart each. these are 1200x600 gif files, with 64 level grayscale. -- +-------------------------------------------------+---------------------------+ |i thought of a good sig, but it was a sight gag. | cloister@u.washington.edu | +-------------------------------------------------+---------------------------+ =========================================================================== ===== From: cloister@milton.u.washington.edu (cloister bell) Organization: University of Washington oh, i should mention that these are sattelite photos of the earth, not ground-based photos of the sun. all in all, though, it looks like a big hole in the world. -- +-------------------------------------------------+---------------------------+ |i thought of a good sig, but it was a sight gag. | cloister@u.washington.edu | +-------------------------------------------------+---------------------------+</text>
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<text>Photos satellites de la terre au moment d'une éclipse, montrant l'ombre de la lune.</text>
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<text>Fotos de satélite de la tierra durante un eclipse que muestra la sombra de la luna.</text>
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<text>Satellitenphotos von der Erde, mit Schatten vom Mond, während einer Vefinsterung.</text>
<text>From: Gary Kronk <C09630GK@wuvmd.wustl.edu> Organization: Washington University, St. Louis Someone recently asked if satellite photos of the eclipse had ever been obtained. Well, if you can ftp to various sites, try VMD.SCO.UIUC.EDU (or 128.174.5.98) and there are five files by a weather satellite which show the moon's shadow moving across the Pacific, into Mexico, and into the Gulf of Mexico. The files are GIFs and each is nearly 400K. They are 1200x600 and 256 shades of gray. The moon's shadow is very distinct. Gary W. Kronk C09630GK@WUVMD.WUSTL.EDU =========================================================================== ===== From: cloister@milton.u.washington.edu (cloister bell) Organization: University of Washington there are 5 pictures of what i believe to be this eclipse available for anonymous ftp from vmd.cso.uiuc.edu in the PHIL.515 directory. this is a ibm vm/cms site, so it's version of ftp may be a little different than you're used to. the images are labeled solar17z.gif thru solar20z.gif. they appear to be taken an hour apart each. these are 1200x600 gif files, with 64 level grayscale. -- +-------------------------------------------------+---------------------------+ |i thought of a good sig, but it was a sight gag. | cloister@u.washington.edu | +-------------------------------------------------+---------------------------+ =========================================================================== ===== From: cloister@milton.u.washington.edu (cloister bell) Organization: University of Washington oh, i should mention that these are sattelite photos of the earth, not ground-based photos of the sun. all in all, though, it looks like a big hole in the world. -- +-------------------------------------------------+---------------------------+ |i thought of a good sig, but it was a sight gag. | cloister@u.washington.edu | +-------------------------------------------------+---------------------------+</text>
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<text>Photos satellites de la terre au moment d'une éclipse, montrant l'ombre de la lune.</text>
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<text>Fotos de satélite de la tierra durante un eclipse que muestra la sombra de la luna.</text>
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<text>Satellitenphotos von der Erde, mit Schatten vom Mond, während einer Vefinsterung.</text>
<text>From: Gary Kronk <C09630GK@wuvmd.wustl.edu> Organization: Washington University, St. Louis Someone recently asked if satellite photos of the eclipse had ever been obtained. Well, if you can ftp to various sites, try VMD.SCO.UIUC.EDU (or 128.174.5.98) and there are five files by a weather satellite which show the moon's shadow moving across the Pacific, into Mexico, and into the Gulf of Mexico. The files are GIFs and each is nearly 400K. They are 1200x600 and 256 shades of gray. The moon's shadow is very distinct. Gary W. Kronk C09630GK@WUVMD.WUSTL.EDU =========================================================================== ===== From: cloister@milton.u.washington.edu (cloister bell) Organization: University of Washington there are 5 pictures of what i believe to be this eclipse available for anonymous ftp from vmd.cso.uiuc.edu in the PHIL.515 directory. this is a ibm vm/cms site, so it's version of ftp may be a little different than you're used to. the images are labeled solar17z.gif thru solar20z.gif. they appear to be taken an hour apart each. these are 1200x600 gif files, with 64 level grayscale. -- +-------------------------------------------------+---------------------------+ |i thought of a good sig, but it was a sight gag. | cloister@u.washington.edu | +-------------------------------------------------+---------------------------+ =========================================================================== ===== From: cloister@milton.u.washington.edu (cloister bell) Organization: University of Washington oh, i should mention that these are sattelite photos of the earth, not ground-based photos of the sun. all in all, though, it looks like a big hole in the world. -- +-------------------------------------------------+---------------------------+ |i thought of a good sig, but it was a sight gag. | cloister@u.washington.edu | +-------------------------------------------------+---------------------------+</text>
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<text>Photos satellites de la terre au moment d'une éclipse, montrant l'ombre de la lune.</text>
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<text>Fotos de satélite de la tierra durante un eclipse que muestra la sombra de la luna.</text>
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<text>Satellitenphotos von der Erde, mit Schatten vom Mond, während einer Vefinsterung.</text>
<text>From: Gary Kronk <C09630GK@wuvmd.wustl.edu> Organization: Washington University, St. Louis Someone recently asked if satellite photos of the eclipse had ever been obtained. Well, if you can ftp to various sites, try VMD.SCO.UIUC.EDU (or 128.174.5.98) and there are five files by a weather satellite which show the moon's shadow moving across the Pacific, into Mexico, and into the Gulf of Mexico. The files are GIFs and each is nearly 400K. They are 1200x600 and 256 shades of gray. The moon's shadow is very distinct. Gary W. Kronk C09630GK@WUVMD.WUSTL.EDU =========================================================================== ===== From: cloister@milton.u.washington.edu (cloister bell) Organization: University of Washington there are 5 pictures of what i believe to be this eclipse available for anonymous ftp from vmd.cso.uiuc.edu in the PHIL.515 directory. this is a ibm vm/cms site, so it's version of ftp may be a little different than you're used to. the images are labeled solar17z.gif thru solar20z.gif. they appear to be taken an hour apart each. these are 1200x600 gif files, with 64 level grayscale. -- +-------------------------------------------------+---------------------------+ |i thought of a good sig, but it was a sight gag. | cloister@u.washington.edu | +-------------------------------------------------+---------------------------+ =========================================================================== ===== From: cloister@milton.u.washington.edu (cloister bell) Organization: University of Washington oh, i should mention that these are sattelite photos of the earth, not ground-based photos of the sun. all in all, though, it looks like a big hole in the world. -- +-------------------------------------------------+---------------------------+ |i thought of a good sig, but it was a sight gag. | cloister@u.washington.edu | +-------------------------------------------------+---------------------------+</text>
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<text>Photos satellites de la terre au moment d'une éclipse, montrant l'ombre de la lune.</text>
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<text>Fotos de satélite de la tierra durante un eclipse que muestra la sombra de la luna.</text>
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<text>Satellitenphotos von der Erde, mit Schatten vom Mond, während einer Vefinsterung.</text>
<text>Annular Eclipse Info Although there were partly cloudy skies during most of the eclipse, most of the scientific objectives were successfully obtained while the Sun was in a clear area of the sky (about 70% of the time). Several preliminary images are available here. disk_ha.gif is time series of H-alpha images that were digitized from a video tape of the CCD video camera on the Flare</text>
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<text>Images préliminaires de l'éclipse annulaire montrant les limbes lunaires et solaires.</text>
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<text>Imágenes preliminares de eclipse anular que muestra los miembros solares y lunares.</text>
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<text>Einleitende Bilder der jährlichen Verfinsterung, die die lunaren und solar</text>
<text>From: garyo@think.com (Gary Oberbrunner) Organization: Thinking Machines Corporation, Cambridge, MA (USA) Keywords: total eclipse scan pictures GIF FTP I scanned in three of the pictures I took of the 7/11/91 total solar eclipse. To get them, anonymous ftp to think.com (131.239.2.1), cd to /public/garyo, and get (in binary mode!) eclipse.*.gif. They were taken from La Penita (or something like that, pop. about 60), Nayarit, Mexico, about 60 miles north of Puerto Vallarta, on the beach. They were taken with a Nikon f6006 with a 210 mm lens and a 3x teleconverter (making 630mm altogether) at 1/4, 1/2 and 1 second (I think), all at f/16. I scanned the 3x5 prints at 300dpi in RGB color; the resulting TIFF files were converted to 8-bit GIF via tifftopnm | ppmquant -fs 256 | ppmtoggif. The sizes vary according to how much corona you can see in each one: eclipse.1.gif is a 674x597 GIF image with 237 colors eclipse.2.gif is a 750x634 GIF image with 231 colors eclipse.3.gif is a 638x635 GIF image with 239 colors They're each about 250k (more or less) in size. Enjoy!</text>
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<text>Photos de l'éclipse solaire totale de juillet 1991 avec des tailles variables de couronnes solaires de Mexico.</text>
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<text>Fotos de julio del 1994 eclipse total solar con corona de varios tamaños de México.</text>
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<text>Totale Sonnenerfinsterung im Juli '91 mit verschiedenen Koronagrößen; Mexiko.</text>
<text>From: garyo@think.com (Gary Oberbrunner) Organization: Thinking Machines Corporation, Cambridge, MA (USA) Keywords: total eclipse scan pictures GIF FTP I scanned in three of the pictures I took of the 7/11/91 total solar eclipse. To get them, anonymous ftp to think.com (131.239.2.1), cd to /public/garyo, and get (in binary mode!) eclipse.*.gif. They were taken from La Penita (or something like that, pop. about 60), Nayarit, Mexico, about 60 miles north of Puerto Vallarta, on the beach. They were taken with a Nikon f6006 with a 210 mm lens and a 3x teleconverter (making 630mm altogether) at 1/4, 1/2 and 1 second (I think), all at f/16. I scanned the 3x5 prints at 300dpi in RGB color; the resulting TIFF files were converted to 8-bit GIF via tifftopnm | ppmquant -fs 256 | ppmtoggif. The sizes vary according to how much corona you can see in each one: eclipse.1.gif is a 674x597 GIF image with 237 colors eclipse.2.gif is a 750x634 GIF image with 231 colors eclipse.3.gif is a 638x635 GIF image with 239 colors They're each about 250k (more or less) in size. Enjoy!</text>
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<text>Photos de l'éclipse solaire totale de juillet 1991 avec des tailles variables de couronnes solaires de Mexico.</text>
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<text>Fotos de julio del 1994 eclipse total solar con corona de varios tamaños de México.</text>
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<text>Totale Sonnenerfinsterung im Juli '91 mit verschiedenen Koronagrößen; Mexiko.</text>
<text>From: garyo@think.com (Gary Oberbrunner) Organization: Thinking Machines Corporation, Cambridge, MA (USA) Keywords: total eclipse scan pictures GIF FTP I scanned in three of the pictures I took of the 7/11/91 total solar eclipse. To get them, anonymous ftp to think.com (131.239.2.1), cd to /public/garyo, and get (in binary mode!) eclipse.*.gif. They were taken from La Penita (or something like that, pop. about 60), Nayarit, Mexico, about 60 miles north of Puerto Vallarta, on the beach. They were taken with a Nikon f6006 with a 210 mm lens and a 3x teleconverter (making 630mm altogether) at 1/4, 1/2 and 1 second (I think), all at f/16. I scanned the 3x5 prints at 300dpi in RGB color; the resulting TIFF files were converted to 8-bit GIF via tifftopnm | ppmquant -fs 256 | ppmtoggif. The sizes vary according to how much corona you can see in each one: eclipse.1.gif is a 674x597 GIF image with 237 colors eclipse.2.gif is a 750x634 GIF image with 231 colors eclipse.3.gif is a 638x635 GIF image with 239 colors They're each about 250k (more or less) in size. Enjoy!</text>
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<text>Photos de l'éclipse solaire totale de juillet 1991 avec des tailles variables de couronnes solaires de Mexico.</text>
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<text>Fotos de julio del 1994 eclipse total solar con corona de varios tamaños de México.</text>
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<text>Totale Sonnenerfinsterung im Juli '91 mit verschiedenen Koronagrößen; Mexiko.</text>
<text>Short: Sun Eclipse of May 10 1994, with Green Flash. Type: JPEG image 24bit Uploader: roelle@grant.jhuapl.edu for mc7414@mclink.it Author: mc7414@mclink.it This is an under-exposed image of the Sun eclipse in May 10 1994. This picture even shows the strange phenomena called "Green Flash". The image was converted from a Kodak PhotoCD (tm) at resolution 4 on the Amiga 4000/40 with ADPro 2.5 The original picture was taken with the follwing data: Film : Fuji Velvia 50 ISO, Color DIA Exp : 1"/60 F : f/10 Camera : Nikon F-601, direct focus on Mead 2045S Site : Rome, Italy Time : 18:18 U.T. In the little rectangle at top-right you can see a zoomed view of the Green Flash. This is a plain image, not filtered or so... Question to you all: When I saw the green flash, the Sun was completely above the horizon. Usually this phenomena can be seen when the Sun is, at least, half under the horizon. So the partial reduced luminosity of the Sun is one of the factor that make the Green Flash visibile. Is it right? Stefano Iacus E-Mail: mc7414@mclink.it</text>
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<text>Photo d'une éclipse solaire du 5-10-94 montrant le phénomène Green Flash.</text>
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<text>Foto de eclipse solar del 10.5.94 que muestra fen├│meno del Fulgor Verde.</text>
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<text>Photo der Sonnenverfinsterung vom 10.5. '94, die das Green-Flash-Phänomen zeigt.</text>
<text>Total Solar Eclipse 03 November 1994 ==================================== These are some views of the shadow of the moon on the earths surface as seen from the geostationary weather satellite METEOSAT 5. They were received by Greg Roberts,Cape Town using his weather satellite station equipped with a 7 foot dish and reception on 1691-1694.5 Mhz. ecl-1 A little too early for the shadow to be apparent from Meteosat 5 at 1200 UT ecl-2 By 1500UT the shadow was very obvious and may be seen off the South west coast of Southern Africa. ecl-3 In this close-up of the mid-southern Atlantic the shadow is very obvious again ecl-4 The shadow is quite obvious off the south west coast of southern Africa. Note that the eastern edge of the picture is in near darkness as a result of approaching night ecl-5 The shadow can still be detected at the left edge whilst the rest of the picture is in almost total darkness as a result of illumination being too low for a visible light picture Pictures taken in infra-red were also received but the shadow is not obvious. GRR@da.saao.ac.za</text>
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<text>L'ombre de la lune sur la surface de la terre vue au moment d'une éclipse solaire totale.</text>
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<text>Sombra de la luna en la superficie de la tierra vista durante un eclipse total del sol.</text>
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<text>Der Mondschattn auf der Erdoberfläche, während einer totalen Sonnenfinsternis.</text>
<text>Total Solar Eclipse 03 November 1994 ==================================== These are some views of the shadow of the moon on the earths surface as seen from the geostationary weather satellite METEOSAT 5. They were received by Greg Roberts,Cape Town using his weather satellite station equipped with a 7 foot dish and reception on 1691-1694.5 Mhz. ecl-1 A little too early for the shadow to be apparent from Meteosat 5 at 1200 UT ecl-2 By 1500UT the shadow was very obvious and may be seen off the South west coast of Southern Africa. ecl-3 In this close-up of the mid-southern Atlantic the shadow is very obvious again ecl-4 The shadow is quite obvious off the south west coast of southern Africa. Note that the eastern edge of the picture is in near darkness as a result of approaching night ecl-5 The shadow can still be detected at the left edge whilst the rest of the picture is in almost total darkness as a result of illumination being too low for a visible light picture Pictures taken in infra-red were also received but the shadow is not obvious. GRR@da.saao.ac.za</text>
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<text>L'ombre de la lune sur la surface de la terre vue au moment d'une éclipse solaire totale.</text>
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<id>31</id>
<text>Sombra de la luna en la superficie de la tierra vista durante un eclipse total del sol.</text>
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<content>
<layer>background</layer>
<id>30</id>
<text>Der Mondschattn auf der Erdoberfläche, während einer totalen Sonnenfinsternis.</text>
<text>Total Solar Eclipse 03 November 1994 ==================================== These are some views of the shadow of the moon on the earths surface as seen from the geostationary weather satellite METEOSAT 5. They were received by Greg Roberts,Cape Town using his weather satellite station equipped with a 7 foot dish and reception on 1691-1694.5 Mhz. ecl-1 A little too early for the shadow to be apparent from Meteosat 5 at 1200 UT ecl-2 By 1500UT the shadow was very obvious and may be seen off the South west coast of Southern Africa. ecl-3 In this close-up of the mid-southern Atlantic the shadow is very obvious again ecl-4 The shadow is quite obvious off the south west coast of southern Africa. Note that the eastern edge of the picture is in near darkness as a result of approaching night ecl-5 The shadow can still be detected at the left edge whilst the rest of the picture is in almost total darkness as a result of illumination being too low for a visible light picture Pictures taken in infra-red were also received but the shadow is not obvious. GRR@da.saao.ac.za</text>
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<layer>background</layer>
<id>29</id>
<text>L'ombre de la lune sur la surface de la terre vue au moment d'une éclipse solaire totale.</text>
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<content>
<layer>background</layer>
<id>31</id>
<text>Sombra de la luna en la superficie de la tierra vista durante un eclipse total del sol.</text>
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<content>
<layer>background</layer>
<id>30</id>
<text>Der Mondschattn auf der Erdoberfläche, während einer totalen Sonnenfinsternis.</text>
<text>Total Solar Eclipse 03 November 1994 ==================================== These are some views of the shadow of the moon on the earths surface as seen from the geostationary weather satellite METEOSAT 5. They were received by Greg Roberts,Cape Town using his weather satellite station equipped with a 7 foot dish and reception on 1691-1694.5 Mhz. ecl-1 A little too early for the shadow to be apparent from Meteosat 5 at 1200 UT ecl-2 By 1500UT the shadow was very obvious and may be seen off the South west coast of Southern Africa. ecl-3 In this close-up of the mid-southern Atlantic the shadow is very obvious again ecl-4 The shadow is quite obvious off the south west coast of southern Africa. Note that the eastern edge of the picture is in near darkness as a result of approaching night ecl-5 The shadow can still be detected at the left edge whilst the rest of the picture is in almost total darkness as a result of illumination being too low for a visible light picture Pictures taken in infra-red were also received but the shadow is not obvious. GRR@da.saao.ac.za</text>
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<content>
<layer>background</layer>
<id>29</id>
<text>L'ombre de la lune sur la surface de la terre vue au moment d'une éclipse solaire totale.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Sombra de la luna en la superficie de la tierra vista durante un eclipse total del sol.</text>
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<content>
<layer>background</layer>
<id>30</id>
<text>Der Mondschattn auf der Erdoberfläche, während einer totalen Sonnenfinsternis.</text>
<text>Total Solar Eclipse 03 November 1994 ==================================== These are some views of the shadow of the moon on the earths surface as seen from the geostationary weather satellite METEOSAT 5. They were received by Greg Roberts,Cape Town using his weather satellite station equipped with a 7 foot dish and reception on 1691-1694.5 Mhz. ecl-1 A little too early for the shadow to be apparent from Meteosat 5 at 1200 UT ecl-2 By 1500UT the shadow was very obvious and may be seen off the South west coast of Southern Africa. ecl-3 In this close-up of the mid-southern Atlantic the shadow is very obvious again ecl-4 The shadow is quite obvious off the south west coast of southern Africa. Note that the eastern edge of the picture is in near darkness as a result of approaching night ecl-5 The shadow can still be detected at the left edge whilst the rest of the picture is in almost total darkness as a result of illumination being too low for a visible light picture Pictures taken in infra-red were also received but the shadow is not obvious. GRR@da.saao.ac.za</text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>L'ombre de la lune sur la surface de la terre vue au moment d'une éclipse solaire totale.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Sombra de la luna en la superficie de la tierra vista durante un eclipse total del sol.</text>
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<content>
<layer>background</layer>
<id>30</id>
<text>Der Mondschattn auf der Erdoberfläche, während einer totalen Sonnenfinsternis.</text>
<text>annular.gif This is a digitally composed picture, taken from 9 shots I took during the recent annular eclipse. The pictures were taken through a Meade 2045 1000mm focal length f/10 Schmidt-Cassegrain telescope at prime focus, with a full-aperture solar filter on the front. They were 1/125 second exposures onto Kodak Gold 200 ASA print film. They were scanned with an HP Scanjet IICX, and composited with xpaint and color contrast enhanced with xv3. Enjoy! -- Ross Cunniff Hewlett-Packard Graphics Software Lab cunniff@fc.hp.com Memo to myself: do the dumb things I gotta do. Touch the puppet head.</text>
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<text>Image composée digitallement, faite à partir de 9 prises de vues de la récente éclipse annulaire.</text>
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<content>
<layer>background</layer>
<id>31</id>
<text>Foto compuesta digitalmente tomada de nueve fotos del reciente eclipse anular.</text>
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<content>
<layer>background</layer>
<id>30</id>
<text>Von 9 Bildern einer jährlichen Verdunkelung digital-zusammengesetztes Bild.</text>
<text> annular.gif This is a digitally composed picture, taken from 9 shots I took during the recent annular eclipse. The pictures were taken through a Meade 2045 1000mm focal length f/10 Schmidt-Cassegrain telescope at prime focus, with a full-aperture solar filter on the front. They were 1/125 second exposures onto Kodak Gold 200 ASA print film. They were scanned with an HP Scanjet IICX, and composited with xpaint and color contrast enhanced with xv3. Enjoy! -- Ross Cunniff Hewlett-Packard Graphics Software Lab cunniff@fc.hp.com Memo to myself: do the dumb things I gotta do. Touch the puppet head.</text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Image composée digitallement, faite à partir de 9 prises de vues de la récente éclipse annulaire.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Foto compuesta digitalmente tomada de nueve fotos del reciente eclipse anular.</text>
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<content>
<layer>background</layer>
<id>30</id>
<text>Von 9 Bildern einer jährlichen Verdunkelung digital-zusammengesetztes Bild.</text>
<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37789 MGN-37 3/5/91 This Magellan image is located in the Eistla Region of Venus in the southern hemisphere and is centered at 5.5 degrees east longitude, 18 degrees south latitude. It is 122.8 kilometers (76.1 miles) across east-west and 107.5 kilometers (66.6 miles) across north-south. North is oriented towards the top of the image. Shown in the image is an unusual volcanic edifice unlike all others previously observed. It is approximately 65.6 kilometers (40.7 miles) across at the base and has a relatively flat, slightly concave summit 34.8 kilometers (21.6 miles) in diameter. The sides of the edifice are characterized by radiating ridges and valleys that impart a fluted appearance to the construct. To the west, the rim of the edifice appears to have been breached by dark lava flows that emanated from a shallow summit pit approximately 5.4 kilometers (3.3 miles) in diameter and traveled west along a channel approximately 5.4 kilometers (3.3 miles) wide and 26.8 kilometers (16.6 miles) long. A series of coalescing, collapsed pits 2-10 kilometers (1.2-6.2 miles) in diameter are located 10 kilometers (6.2 miles) west of the summit rim. The edifice and western pits are circumscribed by faint, concentric lineaments up to 70.3 kilometers (43.6 miles) in diameter. A series of north-northwest-trending graben are deflected eastwards around the edifice; the interplay of these graben and the fluted rim of the edifice produce a distinctive scalloped pattern in the image. Several north-northwest-trending lineaments cut directly across the summit region. This peculiar volcanic construct is located 25-30 kilometers (15.5-18.6 miles) north of Alpha Regio, a highly deformed region of tessera terrain. A collection of at least 6 similar volcanoes has been observed near Thetis Regio, a region of tessera within Aphrodite Terra. Thus, these unusual constructs tentatively appear to be spatially associated with regions of tessera. The implications of this spatial association on the unusual morphology of these constructs are being investigated. </text>
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<content>
<layer>background</layer>
<id>29</id>
<text>Image Magellan d'un édifice volcanique inhabituel dans la région Eistla de Vénus.</text>
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<content>
<layer>background</layer>
<id>31</id>
<text>Imagen desde Magallanes de una estructura volcánica rara en la Región Eistla de Venus.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Magellanbild eines ungew├╢hnlichen vulkanischem Gebildes, Eistla Region -Venus.</text>
<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37789 MGN-37 3/5/91 This Magellan image is located in the Eistla Region of Venus in the southern hemisphere and is centered at 5.5 degrees east longitude, 18 degrees south latitude. It is 122.8 kilometers (76.1 miles) across east-west and 107.5 kilometers (66.6 miles) across north-south. North is oriented towards the top of the image. Shown in the image is an unusual volcanic edifice unlike all others previously observed. It is approximately 65.6 kilometers (40.7 miles) across at the base and has a relatively flat, slightly concave summit 34.8 kilometers (21.6 miles) in diameter. The sides of the edifice are characterized by radiating ridges and valleys that impart a fluted appearance to the construct. To the west, the rim of the edifice appears to have been breached by dark lava flows that emanated from a shallow summit pit approximately 5.4 kilometers (3.3 miles) in diameter and traveled west along a channel approximately 5.4 kilometers (3.3 miles) wide and 26.8 kilometers (16.6 miles) long. A series of coalescing, collapsed pits 2-10 kilometers (1.2-6.2 miles) in diameter are located 10 kilometers (6.2 miles) west of the summit rim. The edifice and western pits are circumscribed by faint, concentric lineaments up to 70.3 kilometers (43.6 miles) in diameter. A series of north-northwest-trending graben are deflected eastwards around the edifice; the interplay of these graben and the fluted rim of the edifice produce a distinctive scalloped pattern in the image. Several north-northwest-trending lineaments cut directly across the summit region. This peculiar volcanic construct is located 25-30 kilometers (15.5-18.6 miles) north of Alpha Regio, a highly deformed region of tessera terrain. A collection of at least 6 similar volcanoes has been observed near Thetis Regio, a region of tessera within Aphrodite Terra. Thus, these unusual constructs tentatively appear to be spatially associated with regions of tessera. The implications of this spatial association on the unusual morphology of these constructs are being investigated. </text>
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<content>
<layer>background</layer>
<id>29</id>
<text>Image Magellan d'un édifice volcanique inhabituel dans la région Eistla de Vénus.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Imagen desde Magallanes de una estructura volcánica rara en la Región Eistla de Venus.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Magellanbild eines ungew├╢hnlichen vulkanischem Gebildes, Eistla Region -Venus.</text>
<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37789 MGN-37 3/5/91 This Magellan image is located in the Eistla Region of Venus in the southern hemisphere and is centered at 5.5 degrees east longitude, 18 degrees south latitude. It is 122.8 kilometers (76.1 miles) across east-west and 107.5 kilometers (66.6 miles) across north-south. North is oriented towards the top of the image. Shown in the image is an unusual volcanic edifice unlike all others previously observed. It is approximately 65.6 kilometers (40.7 miles) across at the base and has a relatively flat, slightly concave summit 34.8 kilometers (21.6 miles) in diameter. The sides of the edifice are characterized by radiating ridges and valleys that impart a fluted appearance to the construct. To the west, the rim of the edifice appears to have been breached by dark lava flows that emanated from a shallow summit pit approximately 5.4 kilometers (3.3 miles) in diameter and traveled west along a channel approximately 5.4 kilometers (3.3 miles) wide and 26.8 kilometers (16.6 miles) long. A series of coalescing, collapsed pits 2-10 kilometers (1.2-6.2 miles) in diameter are located 10 kilometers (6.2 miles) west of the summit rim. The edifice and western pits are circumscribed by faint, concentric lineaments up to 70.3 kilometers (43.6 miles) in diameter. A series of north-northwest-trending graben are deflected eastwards around the edifice; the interplay of these graben and the fluted rim of the edifice produce a distinctive scalloped pattern in the image. Several north-northwest-trending lineaments cut directly across the summit region. This peculiar volcanic construct is located 25-30 kilometers (15.5-18.6 miles) north of Alpha Regio, a highly deformed region of tessera terrain. A collection of at least 6 similar volcanoes has been observed near Thetis Regio, a region of tessera within Aphrodite Terra. Thus, these unusual constructs tentatively appear to be spatially associated with regions of tessera. The implications of this spatial association on the unusual morphology of these constructs are being investigated. </text>
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<content>
<layer>background</layer>
<id>29</id>
<text>Image Magellan d'un édifice volcanique inhabituel dans la région Eistla de Vénus.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Imagen desde Magallanes de una estructura volcánica rara en la Región Eistla de Venus.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Magellanbild eines ungew├╢hnlichen vulkanischem Gebildes, Eistla Region -Venus.</text>
<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37137 MGN-19 11/16/90 This Magellan image reveals Sacajawea Patera, a large, elongate caldera located in Western Ishtar Terra on the smooth plateau of Lakshmi Planum. The image is centered at 64.5 degrees North latitude and 337 degrees East longitude. It is approximately 420 kilometers (252 miles) wide at the base. Sacajawea is a depression approximately 1-2 kilometers (0.6 -1.2 miles) deep and 120 x 215 kilometers (74 x 133 miles) in diameter; it is elongate in a southwest-northeast direction. The depression is bounded by a zone of circumferential curvilinear structures interpreted to be graben and fault scarps. These structures are spaced 0.5-4 kilometers (0.3-2.5 miles) apart, are 0.6-4.0 kilometers (0.4-2.5 miles) in width and up to 100 kilometers (62 miles) in length. Extending up to approximately 140 kilometers (87 miles) in length from the southeast of the patera is a system of linear structures thought to represent a flanking rift zone along which the lateral injection and eruption of magma may have occurred. A shield edifice 12 kilometers (7 miles) in diameter with a prominent central pit lies along the trend of one of these features. The impact crater Zlata , approximately 6 kilometers (4 miles) in diameter is located within the zone of graben to the northwest of the patera. Few flow features are observed in association with Sacajawea, possibly due to age and state of degradation of the flows. Mottled bright deposits 4-20 kilometers (2.5-12 miles) in width are located near the periphery and in the center of the patera floor within local topographic lows. Diffuse patches of dark material approximately 40 kilometers (25 miles) in width are observed southwest of the patera, superposed on portions of the surrounding graben. The formation of Sacajawea is thought to be related to the drainage and collapse of a large magma chamber. Gravitational relaxation may have caused the resultant caldera to sag, producing the numerous faults and graben that circumscribe the patera. Regions of complex, highly deformed tessera-like terrain are located north and east of the patera and are seen in the upper portion of the image. Color has been added to this image to simulate the appearance of the Venus surface. </text>
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<text>Sacajawea Patera, une caldera large et allongée située dans Western Ishtar Terra.</text>
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<id>31</id>
<text>Sacajawea Patera, caldera alargada, ubicada en Ishtar Terra occidental.</text>
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<id>30</id>
<text>Sacajawea Patera, eine große, verlängerte Kaldera, im westlichen Ishtar Terra.</text>
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<text>Sacajawea Patera, ¶Ï¶b Ishtar Terra ¶Ë√‰™∫•®§j™∫, ©µ¶˘™∫§ı§s§f.</text>
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<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37137 MGN-19 11/16/90 This Magellan image reveals Sacajawea Patera, a large, elongate caldera located in Western Ishtar Terra on the smooth plateau of Lakshmi Planum. The image is centered at 64.5 degrees North latitude and 337 degrees East longitude. It is approximately 420 kilometers (252 miles) wide at the base. Sacajawea is a depression approximately 1-2 kilometers (0.6 -1.2 miles) deep and 120 x 215 kilometers (74 x 133 miles) in diameter; it is elongate in a southwest-northeast direction. The depression is bounded by a zone of circumferential curvilinear structures interpreted to be graben and fault scarps. These structures are spaced 0.5-4 kilometers (0.3-2.5 miles) apart, are 0.6-4.0 kilometers (0.4-2.5 miles) in width and up to 100 kilometers (62 miles) in length. Extending up to approximately 140 kilometers (87 miles) in length from the southeast of the patera is a system of linear structures thought to represent a flanking rift zone along which the lateral injection and eruption of magma may have occurred. A shield edifice 12 kilometers (7 miles) in diameter with a prominent central pit lies along the trend of one of these features. The impact crater Zlata , approximately 6 kilometers (4 miles) in diameter is located within the zone of graben to the northwest of the patera. Few flow features are observed in association with Sacajawea, possibly due to age and state of degradation of the flows. Mottled bright deposits 4-20 kilometers (2.5-12 miles) in width are located near the periphery and in the center of the patera floor within local topographic lows. Diffuse patches of dark material approximately 40 kilometers (25 miles) in width are observed southwest of the patera, superposed on portions of the surrounding graben. The formation of Sacajawea is thought to be related to the drainage and collapse of a large magma chamber. Gravitational relaxation may have caused the resultant caldera to sag, producing the numerous faults and graben that circumscribe the patera. Regions of complex, highly deformed tessera-like terrain are located north and east of the patera and are seen in the upper portion of the image. Color has been added to this image to simulate the appearance of the Venus surface. </text>
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<text>Sacajawea Patera, une caldera large et allongée située dans Western Ishtar Terra.</text>
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<text>Sacajawea Patera, caldera alargada, ubicada en Ishtar Terra occidental.</text>
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<text>Sacajawea Patera, eine große, verlängerte Kaldera, im westlichen Ishtar Terra.</text>
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<text>Sacajawea Patera, ¶Ï¶b Ishtar Terra ¶Ë√‰™∫•®§j™∫, ©µ¶˘™∫§ı§s§f.</text>
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<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37137 MGN-19 11/16/90 This Magellan image reveals Sacajawea Patera, a large, elongate caldera located in Western Ishtar Terra on the smooth plateau of Lakshmi Planum. The image is centered at 64.5 degrees North latitude and 337 degrees East longitude. It is approximately 420 kilometers (252 miles) wide at the base. Sacajawea is a depression approximately 1-2 kilometers (0.6 -1.2 miles) deep and 120 x 215 kilometers (74 x 133 miles) in diameter; it is elongate in a southwest-northeast direction. The depression is bounded by a zone of circumferential curvilinear structures interpreted to be graben and fault scarps. These structures are spaced 0.5-4 kilometers (0.3-2.5 miles) apart, are 0.6-4.0 kilometers (0.4-2.5 miles) in width and up to 100 kilometers (62 miles) in length. Extending up to approximately 140 kilometers (87 miles) in length from the southeast of the patera is a system of linear structures thought to represent a flanking rift zone along which the lateral injection and eruption of magma may have occurred. A shield edifice 12 kilometers (7 miles) in diameter with a prominent central pit lies along the trend of one of these features. The impact crater Zlata , approximately 6 kilometers (4 miles) in diameter is located within the zone of graben to the northwest of the patera. Few flow features are observed in association with Sacajawea, possibly due to age and state of degradation of the flows. Mottled bright deposits 4-20 kilometers (2.5-12 miles) in width are located near the periphery and in the center of the patera floor within local topographic lows. Diffuse patches of dark material approximately 40 kilometers (25 miles) in width are observed southwest of the patera, superposed on portions of the surrounding graben. The formation of Sacajawea is thought to be related to the drainage and collapse of a large magma chamber. Gravitational relaxation may have caused the resultant caldera to sag, producing the numerous faults and graben that circumscribe the patera. Regions of complex, highly deformed tessera-like terrain are located north and east of the patera and are seen in the upper portion of the image. Color has been added to this image to simulate the appearance of the Venus surface. </text>
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<text>Sacajawea Patera, une caldera large et allongée située dans Western Ishtar Terra.</text>
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<text>Sacajawea Patera, caldera alargada, ubicada en Ishtar Terra occidental.</text>
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<text>Sacajawea Patera, eine große, verlängerte Kaldera, im westlichen Ishtar Terra.</text>
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<text>Sacajawea Patera, ¶Ï¶b Ishtar Terra ¶Ë√‰™∫•®§j™∫, ©µ¶˘™∫§ı§s§f.</text>
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card_19267.xml
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<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37137 MGN-19 11/16/90 This Magellan image reveals Sacajawea Patera, a large, elongate caldera located in Western Ishtar Terra on the smooth plateau of Lakshmi Planum. The image is centered at 64.5 degrees North latitude and 337 degrees East longitude. It is approximately 420 kilometers (252 miles) wide at the base. Sacajawea is a depression approximately 1-2 kilometers (0.6 -1.2 miles) deep and 120 x 215 kilometers (74 x 133 miles) in diameter; it is elongate in a southwest-northeast direction. The depression is bounded by a zone of circumferential curvilinear structures interpreted to be graben and fault scarps. These structures are spaced 0.5-4 kilometers (0.3-2.5 miles) apart, are 0.6-4.0 kilometers (0.4-2.5 miles) in width and up to 100 kilometers (62 miles) in length. Extending up to approximately 140 kilometers (87 miles) in length from the southeast of the patera is a system of linear structures thought to represent a flanking rift zone along which the lateral injection and eruption of magma may have occurred. A shield edifice 12 kilometers (7 miles) in diameter with a prominent central pit lies along the trend of one of these features. The impact crater Zlata , approximately 6 kilometers (4 miles) in diameter is located within the zone of graben to the northwest of the patera. Few flow features are observed in association with Sacajawea, possibly due to age and state of degradation of the flows. Mottled bright deposits 4-20 kilometers (2.5-12 miles) in width are located near the periphery and in the center of the patera floor within local topographic lows. Diffuse patches of dark material approximately 40 kilometers (25 miles) in width are observed southwest of the patera, superposed on portions of the surrounding graben. The formation of Sacajawea is thought to be related to the drainage and collapse of a large magma chamber. Gravitational relaxation may have caused the resultant caldera to sag, producing the numerous faults and graben that circumscribe the patera. Regions of complex, highly deformed tessera-like terrain are located north and east of the patera and are seen in the upper portion of the image. Color has been added to this image to simulate the appearance of the Venus surface. </text>
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<text>Sacajawea Patera, une caldera large et allongée située dans Western Ishtar Terra.</text>
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<text>Sacajawea Patera, caldera alargada, ubicada en Ishtar Terra occidental.</text>
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<text>Sacajawea Patera, eine große, verlängerte Kaldera, im westlichen Ishtar Terra.</text>
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<text>Sacajawea Patera, ¶Ï¶b Ishtar Terra ¶Ë√‰™∫•®§j™∫, ©µ¶˘™∫§ı§s§f.</text>
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<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37137 MGN-19 11/16/90 This Magellan image reveals Sacajawea Patera, a large, elongate caldera located in Western Ishtar Terra on the smooth plateau of Lakshmi Planum. The image is centered at 64.5 degrees North latitude and 337 degrees East longitude. It is approximately 420 kilometers (252 miles) wide at the base. Sacajawea is a depression approximately 1-2 kilometers (0.6 -1.2 miles) deep and 120 x 215 kilometers (74 x 133 miles) in diameter; it is elongate in a southwest-northeast direction. The depression is bounded by a zone of circumferential curvilinear structures interpreted to be graben and fault scarps. These structures are spaced 0.5-4 kilometers (0.3-2.5 miles) apart, are 0.6-4.0 kilometers (0.4-2.5 miles) in width and up to 100 kilometers (62 miles) in length. Extending up to approximately 140 kilometers (87 miles) in length from the southeast of the patera is a system of linear structures thought to represent a flanking rift zone along which the lateral injection and eruption of magma may have occurred. A shield edifice 12 kilometers (7 miles) in diameter with a prominent central pit lies along the trend of one of these features. The impact crater Zlata , approximately 6 kilometers (4 miles) in diameter is located within the zone of graben to the northwest of the patera. Few flow features are observed in association with Sacajawea, possibly due to age and state of degradation of the flows. Mottled bright deposits 4-20 kilometers (2.5-12 miles) in width are located near the periphery and in the center of the patera floor within local topographic lows. Diffuse patches of dark material approximately 40 kilometers (25 miles) in width are observed southwest of the patera, superposed on portions of the surrounding graben. The formation of Sacajawea is thought to be related to the drainage and collapse of a large magma chamber. Gravitational relaxation may have caused the resultant caldera to sag, producing the numerous faults and graben that circumscribe the patera. Regions of complex, highly deformed tessera-like terrain are located north and east of the patera and are seen in the upper portion of the image. Color has been added to this image to simulate the appearance of the Venus surface. </text>
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<text>Sacajawea Patera, une caldera large et allongée située dans Western Ishtar Terra.</text>
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<id>31</id>
<text>Sacajawea Patera, caldera alargada, ubicada en Ishtar Terra occidental.</text>
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<id>30</id>
<text>Sacajawea Patera, eine große, verlängerte Kaldera, im westlichen Ishtar Terra.</text>
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<text>Sacajawea Patera, ¶Ï¶b Ishtar Terra ¶Ë√‰™∫•®§j™∫, ©µ¶˘™∫§ı§s§f.</text>
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card_18754.xml
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<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37137 MGN-19 11/16/90 This Magellan image reveals Sacajawea Patera, a large, elongate caldera located in Western Ishtar Terra on the smooth plateau of Lakshmi Planum. The image is centered at 64.5 degrees North latitude and 337 degrees East longitude. It is approximately 420 kilometers (252 miles) wide at the base. Sacajawea is a depression approximately 1-2 kilometers (0.6 -1.2 miles) deep and 120 x 215 kilometers (74 x 133 miles) in diameter; it is elongate in a southwest-northeast direction. The depression is bounded by a zone of circumferential curvilinear structures interpreted to be graben and fault scarps. These structures are spaced 0.5-4 kilometers (0.3-2.5 miles) apart, are 0.6-4.0 kilometers (0.4-2.5 miles) in width and up to 100 kilometers (62 miles) in length. Extending up to approximately 140 kilometers (87 miles) in length from the southeast of the patera is a system of linear structures thought to represent a flanking rift zone along which the lateral injection and eruption of magma may have occurred. A shield edifice 12 kilometers (7 miles) in diameter with a prominent central pit lies along the trend of one of these features. The impact crater Zlata , approximately 6 kilometers (4 miles) in diameter is located within the zone of graben to the northwest of the patera. Few flow features are observed in association with Sacajawea, possibly due to age and state of degradation of the flows. Mottled bright deposits 4-20 kilometers (2.5-12 miles) in width are located near the periphery and in the center of the patera floor within local topographic lows. Diffuse patches of dark material approximately 40 kilometers (25 miles) in width are observed southwest of the patera, superposed on portions of the surrounding graben. The formation of Sacajawea is thought to be related to the drainage and collapse of a large magma chamber. Gravitational relaxation may have caused the resultant caldera to sag, producing the numerous faults and graben that circumscribe the patera. Regions of complex, highly deformed tessera-like terrain are located north and east of the patera and are seen in the upper portion of the image. Color has been added to this image to simulate the appearance of the Venus surface. </text>
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<id>29</id>
<text>Sacajawea Patera, une caldera large et allongée située dans Western Ishtar Terra.</text>
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<content>
<layer>background</layer>
<id>31</id>
<text>Sacajawea Patera, caldera alargada, ubicada en Ishtar Terra occidental.</text>
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<content>
<layer>background</layer>
<id>30</id>
<text>Sacajawea Patera, eine große, verlängerte Kaldera, im westlichen Ishtar Terra.</text>
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<id>32</id>
<text>Sacajawea Patera, ¶Ï¶b Ishtar Terra ¶Ë√‰™∫•®§j™∫, ©µ¶˘™∫§ı§s§f.</text>
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card_18508.xml
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<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37137 MGN-19 11/16/90 This Magellan image reveals Sacajawea Patera, a large, elongate caldera located in Western Ishtar Terra on the smooth plateau of Lakshmi Planum. The image is centered at 64.5 degrees North latitude and 337 degrees East longitude. It is approximately 420 kilometers (252 miles) wide at the base. Sacajawea is a depression approximately 1-2 kilometers (0.6 -1.2 miles) deep and 120 x 215 kilometers (74 x 133 miles) in diameter; it is elongate in a southwest-northeast direction. The depression is bounded by a zone of circumferential curvilinear structures interpreted to be graben and fault scarps. These structures are spaced 0.5-4 kilometers (0.3-2.5 miles) apart, are 0.6-4.0 kilometers (0.4-2.5 miles) in width and up to 100 kilometers (62 miles) in length. Extending up to approximately 140 kilometers (87 miles) in length from the southeast of the patera is a system of linear structures thought to represent a flanking rift zone along which the lateral injection and eruption of magma may have occurred. A shield edifice 12 kilometers (7 miles) in diameter with a prominent central pit lies along the trend of one of these features. The impact crater Zlata , approximately 6 kilometers (4 miles) in diameter is located within the zone of graben to the northwest of the patera. Few flow features are observed in association with Sacajawea, possibly due to age and state of degradation of the flows. Mottled bright deposits 4-20 kilometers (2.5-12 miles) in width are located near the periphery and in the center of the patera floor within local topographic lows. Diffuse patches of dark material approximately 40 kilometers (25 miles) in width are observed southwest of the patera, superposed on portions of the surrounding graben. The formation of Sacajawea is thought to be related to the drainage and collapse of a large magma chamber. Gravitational relaxation may have caused the resultant caldera to sag, producing the numerous faults and graben that circumscribe the patera. Regions of complex, highly deformed tessera-like terrain are located north and east of the patera and are seen in the upper portion of the image. Color has been added to this image to simulate the appearance of the Venus surface. </text>
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<id>29</id>
<text>Sacajawea Patera, une caldera large et allongée située dans Western Ishtar Terra.</text>
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<content>
<layer>background</layer>
<id>31</id>
<text>Sacajawea Patera, caldera alargada, ubicada en Ishtar Terra occidental.</text>
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<layer>background</layer>
<id>30</id>
<text>Sacajawea Patera, eine große, verlängerte Kaldera, im westlichen Ishtar Terra.</text>
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<id>32</id>
<text>Sacajawea Patera, ¶Ï¶b Ishtar Terra ¶Ë√‰™∫•®§j™∫, ©µ¶˘™∫§ı§s§f.</text>
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card_18193.xml
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<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37431 1/3/91 Perspective view of the southern boundary of Lakshmi Planum, Ishtar Terra, Venus. The southern scarp and basin province of western Ishtar Terra in the northern hemisphere of Venus is portrayed in this three-dimensional perspective view of Magellan radar image data. Western Ishtar Terra is an Australia-sized highland terrain that is a major focus of Magellan investigations. The highland is centered on a 2.5-to 4-kilometer-high (1.5 -to 2.5- miles-high) plateau, Lakshmi Planum, which can be seen in the distance and to the right. Along this part of the Planum, the surface of the high plateau drops precipitously into the bounding lowlands, with slopes that exceed 5 percent over 50 kilometers (30 miles). The numerous fractures and valleys located on and adjacent to the steep outer slope of the plateau are clues to the formation of this unusually abrupt topographic drop. Along other parts of the boundary of Lakshmi are mountain ranges that rise as much as 6 kilometers (3.5 miles) above the plateau surface to over 11,000 meters (35,000 feet) above the mean elevation of the surface of Venus. One of these mountain ranges, Danu Montes, rises over 1.5 kilometers (1.0 mile) above the plateau and can be seen in the upper center of the image. Images such as this one show the relationship of geological features to topography and yield a valuable new perception of the radar data. For example, the small dome-shaped high (center left) is a volcano that is not apparent in the normal map-view display of Magellan images. Only when combined with topography in this fashion is the nature of the feature clearly evident. These perspective views also display fractures of the surface in their actual topographic setting. Understanding the relationship of topography to these fractures, which express the stresses and motions in the outer layers of the planet, helps geologists and geophysicists to formulate and test models for the formation of western Ishtar. The results of these studies will add to our understanding of the interior forces that shape the surface of Venus. </text>
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<id>29</id>
<text>Vue en perspective des limites du sud de Lakshmi Planum, Ishtar Terra, Vénus.</text>
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<content>
<layer>background</layer>
<id>31</id>
<text>Vista perspectiva de la frontera sur de Lakshmi Planum, Venus.</text>
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<id>30</id>
<text>Perspektive, die s├╝dliche Grenze von Lakshmi Planum, Ishtar Terra, Venus zeigend.</text>
<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37125 MGN-18 11/16/90 This image of the eastern edge of Alpha Regio, 30 degrees south latitude, 11.8 east longitude, was acquired on November 7, 1990. It shows seven circular domical hills averaging 25 kilometers (15 miles) in diameter and maximum heights of 750 meters (2475 feet). These features can be interpreted as viscous or thick eruptions of lava coming from a vent on the relatively level ground allowing the lava to flow in an even lateral pattern. The concentric and radial fracture pattern on their surfaces suggests if they are extrusive that a chilled outer layer formed then further intrusion in the interior stretched the surface. The domes may be analogous to volcanic domes on Earth. An alternative interpretation is that the domes are the result of shallow intrusions up-doming the surface layers. If they are intrusive, then magma withdrawal near the end of the eruptions then produced the fractures. The bright margins possibly indicate the presence of rock debris or talus at the slopes of the domes. Fractures on the surrounding plains are both older and younger than the domical hills. Resolution of the Magellan data is about 120 meters (400 feet). </text>
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<content>
<layer>background</layer>
<id>29</id>
<text>Image du bord est d'Alpha Regio montrant sept collines circulaires et sphériques.</text>
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<content>
<layer>background</layer>
<id>31</id>
<text>Imagen del límite oriental de Alpha Regio que muestra siete cerros circulares abovedados.</text>
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<content>
<layer>background</layer>
<id>30</id>
<text>Bild des ├╢stlichen Rands von Alpha Regio, sieben runde domartige H├╝gel zeigend.</text>
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<id>32</id>
<text>¶b Alpha Regio ™F≥°πœπ≥, ≈„•‹§C≠”∂Í©w¬I™∫§p§s•C.</text>
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<name>pancakes_card</name>
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card_17911.xml
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<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37125 MGN-18 11/16/90 This image of the eastern edge of Alpha Regio, 30 degrees south latitude, 11.8 east longitude, was acquired on November 7, 1990. It shows seven circular domical hills averaging 25 kilometers (15 miles) in diameter and maximum heights of 750 meters (2475 feet). These features can be interpreted as viscous or thick eruptions of lava coming from a vent on the relatively level ground allowing the lava to flow in an even lateral pattern. The concentric and radial fracture pattern on their surfaces suggests if they are extrusive that a chilled outer layer formed then further intrusion in the interior stretched the surface. The domes may be analogous to volcanic domes on Earth. An alternative interpretation is that the domes are the result of shallow intrusions up-doming the surface layers. If they are intrusive, then magma withdrawal near the end of the eruptions then produced the fractures. The bright margins possibly indicate the presence of rock debris or talus at the slopes of the domes. Fractures on the surrounding plains are both older and younger than the domical hills. Resolution of the Magellan data is about 120 meters (400 feet). </text>
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<content>
<layer>background</layer>
<id>29</id>
<text>Image du bord est d'Alpha Regio montrant sept collines circulaires et sphériques.</text>
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<content>
<layer>background</layer>
<id>31</id>
<text>Imagen del límite oriental de Alpha Regio que muestra siete cerros circulares abovedados.</text>
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<content>
<layer>background</layer>
<id>30</id>
<text>Bild des ├╢stlichen Rands von Alpha Regio, sieben runde domartige H├╝gel zeigend.</text>
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<content>
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<id>32</id>
<text>¶b Alpha Regio ™F≥°πœπ≥, ≈„•‹§C≠”∂Í©w¬I™∫§p§s•C.</text>
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<name>pancake1_card</name>
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card_17486.xml
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<!DOCTYPE card PUBLIC "-//Apple, Inc.//DTD card V 2.0//EN" "" >
<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37125 MGN-18 11/16/90 This image of the eastern edge of Alpha Regio, 30 degrees south latitude, 11.8 east longitude, was acquired on November 7, 1990. It shows seven circular domical hills averaging 25 kilometers (15 miles) in diameter and maximum heights of 750 meters (2475 feet). These features can be interpreted as viscous or thick eruptions of lava coming from a vent on the relatively level ground allowing the lava to flow in an even lateral pattern. The concentric and radial fracture pattern on their surfaces suggests if they are extrusive that a chilled outer layer formed then further intrusion in the interior stretched the surface. The domes may be analogous to volcanic domes on Earth. An alternative interpretation is that the domes are the result of shallow intrusions up-doming the surface layers. If they are intrusive, then magma withdrawal near the end of the eruptions then produced the fractures. The bright margins possibly indicate the presence of rock debris or talus at the slopes of the domes. Fractures on the surrounding plains are both older and younger than the domical hills. Resolution of the Magellan data is about 120 meters (400 feet). </text>
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<content>
<layer>background</layer>
<id>29</id>
<text>Image du bord est d'Alpha Regio montrant sept collines circulaires et sphériques.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Imagen del límite oriental de Alpha Regio que muestra siete cerros circulares abovedados.</text>
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<content>
<layer>background</layer>
<id>30</id>
<text>Bild des ├╢stlichen Rands von Alpha Regio, sieben runde domartige H├╝gel zeigend.</text>
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<content>
<layer>background</layer>
<id>32</id>
<text>¶b Alpha Regio ™F≥°πœπ≥, ≈„•‹§C≠”∂Í©w¬I™∫§p§s•C.</text>
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<name>pan10_card</name>
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card_17398.xml
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<!DOCTYPE card PUBLIC "-//Apple, Inc.//DTD card V 2.0//EN" "" >
<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37787 MGN-35 3/5/91 This Magellan image shows part of the northern boundary of Ovda Regio, one of the large highlands ringing the equator of Venus. The scene consists largely of low-relief, rounded linear ridges. These ridges, 8-15 kilometers (5-9 miles) in width and 30-60 kilometers (20-40 miles) long, lie mostly along a 100-200 kilometer (60-120 mile) wide slope where the elevation drops 3 kilometers (2 miles) from Ovda Regio to the surrounding plains. Some of the ridges have been cut at right angles by extension fractures. Dark material, either lava or windblown dirt, fills the region between the ridges. The curvilinear, banded nature of these ridges suggests that crustal shortening, roughly oriented north-south, is largely responsible for their formation. Such crustal shortening was unexpected by Magellan scientists, who believed that Ovda Regio, a likely site of hot upwelling from the interior of Venus, should be dominated by volcanism and crustal extension. This image, centered approximately at 1 N 81 E, measures 300 kilometers (190 miles) by 225 kilometers (140 miles) and was acquired by Magellan in November 1990. </text>
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<content>
<layer>background</layer>
<id>29</id>
<text>Image Magellan des limites du nord d'Ovda Regio, allant autour de l'équateur de Vénus.</text>
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<content>
<layer>background</layer>
<id>31</id>
<text>Imagen desde Magallanes de la frontera norte de Ovda regio, que circunda el ecuador de Venus.</text>
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<layer>background</layer>
<id>30</id>
<text>Magellan-Bild der n├╢rdlichen Grenze zu Ovda Regio, die den Venus umringt.</text>
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<id>32</id>
<text>¶b Ovda Regio •_√‰√‰¨…™∫ Magellan ¨Mπ≥, ≥Ú¬∂™˜¨P®™πD.</text>
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<name>ovdan3_card</name>
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card_17046.xml
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<!DOCTYPE card PUBLIC "-//Apple, Inc.//DTD card V 2.0//EN" "" >
<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37787 MGN-35 3/5/91 This Magellan image shows part of the northern boundary of Ovda Regio, one of the large highlands ringing the equator of Venus. The scene consists largely of low-relief, rounded linear ridges. These ridges, 8-15 kilometers (5-9 miles) in width and 30-60 kilometers (20-40 miles) long, lie mostly along a 100-200 kilometer (60-120 mile) wide slope where the elevation drops 3 kilometers (2 miles) from Ovda Regio to the surrounding plains. Some of the ridges have been cut at right angles by extension fractures. Dark material, either lava or windblown dirt, fills the region between the ridges. The curvilinear, banded nature of these ridges suggests that crustal shortening, roughly oriented north-south, is largely responsible for their formation. Such crustal shortening was unexpected by Magellan scientists, who believed that Ovda Regio, a likely site of hot upwelling from the interior of Venus, should be dominated by volcanism and crustal extension. This image, centered approximately at 1 N 81 E, measures 300 kilometers (190 miles) by 225 kilometers (140 miles) and was acquired by Magellan in November 1990. </text>
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<content>
<layer>background</layer>
<id>29</id>
<text>Image Magellan des limites du nord d'Ovda Regio, allant autour de l'équateur de Vénus.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Imagen desde Magallanes de la frontera norte de Ovda regio, que circunda el ecuador de Venus.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Magellan-Bild der n├╢rdlichen Grenze zu Ovda Regio, die den Venus umringt.</text>
</content>
<content>
<layer>background</layer>
<id>32</id>
<text>¶b Ovda Regio •_√‰√‰¨…™∫ Magellan ¨Mπ≥, ≥Ú¬∂™˜¨P®™πD.</text>
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<name>ovdan2_card</name>
<script></script>
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card_16891.xml
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<!DOCTYPE card PUBLIC "-//Apple, Inc.//DTD card V 2.0//EN" "" >
<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37787 MGN-35 3/5/91 This Magellan image shows part of the northern boundary of Ovda Regio, one of the large highlands ringing the equator of Venus. The scene consists largely of low-relief, rounded linear ridges. These ridges, 8-15 kilometers (5-9 miles) in width and 30-60 kilometers (20-40 miles) long, lie mostly along a 100-200 kilometer (60-120 mile) wide slope where the elevation drops 3 kilometers (2 miles) from Ovda Regio to the surrounding plains. Some of the ridges have been cut at right angles by extension fractures. Dark material, either lava or windblown dirt, fills the region between the ridges. The curvilinear, banded nature of these ridges suggests that crustal shortening, roughly oriented north-south, is largely responsible for their formation. Such crustal shortening was unexpected by Magellan scientists, who believed that Ovda Regio, a likely site of hot upwelling from the interior of Venus, should be dominated by volcanism and crustal extension. This image, centered approximately at 1 N 81 E, measures 300 kilometers (190 miles) by 225 kilometers (140 miles) and was acquired by Magellan in November 1990. </text>
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<content>
<layer>background</layer>
<id>29</id>
<text>Image Magellan des limites du nord d'Ovda Regio, allant autour de l'équateur de Vénus.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Imagen desde Magallanes de la frontera norte de Ovda regio, que circunda el ecuador de Venus.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Magellan-Bild der n├╢rdlichen Grenze zu Ovda Regio, die den Venus umringt.</text>
</content>
<content>
<layer>background</layer>
<id>32</id>
<text>¶b Ovda Regio •_√‰√‰¨…™∫ Magellan ¨Mπ≥, ≥Ú¬∂™˜¨P®™πD.</text>
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<name>ovdan1_card</name>
<script></script>
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card_16471.xml
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<!DOCTYPE card PUBLIC "-//Apple, Inc.//DTD card V 2.0//EN" "" >
<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37787 MGN-35 3/5/91 This Magellan image shows part of the northern boundary of Ovda Regio, one of the large highlands ringing the equator of Venus. The scene consists largely of low-relief, rounded linear ridges. These ridges, 8-15 kilometers (5-9 miles) in width and 30-60 kilometers (20-40 miles) long, lie mostly along a 100-200 kilometer (60-120 mile) wide slope where the elevation drops 3 kilometers (2 miles) from Ovda Regio to the surrounding plains. Some of the ridges have been cut at right angles by extension fractures. Dark material, either lava or windblown dirt, fills the region between the ridges. The curvilinear, banded nature of these ridges suggests that crustal shortening, roughly oriented north-south, is largely responsible for their formation. Such crustal shortening was unexpected by Magellan scientists, who believed that Ovda Regio, a likely site of hot upwelling from the interior of Venus, should be dominated by volcanism and crustal extension. This image, centered approximately at 1 N 81 E, measures 300 kilometers (190 miles) by 225 kilometers (140 miles) and was acquired by Magellan in November 1990. </text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Image Magellan des limites du nord d'Ovda Regio, allant autour de l'équateur de Vénus.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Imagen desde Magallanes de la frontera norte de Ovda regio, que circunda el ecuador de Venus.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Magellan-Bild der n├╢rdlichen Grenze zu Ovda Regio, die den Venus umringt.</text>
</content>
<content>
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<text>¶b Ovda Regio •_√‰√‰¨…™∫ Magellan ¨Mπ≥, ≥Ú¬∂™˜¨P®™πD.</text>
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card_16153.xml
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<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37788 MGN-36 3/5/91 This Magellan image shows part the interior of Ovda Regio, one of the large highlands ringing the equator of Venus. Several tectonic events formed this complex block-fractured terrain. An underlying fabric of ridges and valleys strikes NE-SW. These ridges are spaced 10-20 kilometers (6-12 miles) apart and may have been caused by shortening of the crust at right angles to this trend. These structures are cut by throughgoing extension fractures trending NW-SE, suggesting a later episode of NE-SW extension. Lastly, the largest valleys, particularly the 20 kilometer (12 mile)-wide one extending across the image, were filled with dark material, probably lava. The complex internal fabric of Ovda Regio attests to a long history of tectonic deformation. This image, centered approximately at 1 S 81 E, measures 225 kilometers (140 miles) by 150 kilometers (90 miles) and was acquired by Magellan in November 1990. </text>
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<text>Intérieur de Ovda Regio, une des larges régions montagneuses allant autour de l'équateur de Vénus.</text>
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<id>31</id>
<text>Interior de Ovda Regio, uno de los grandes altiplanos que circundan el ecuador de Venus.</text>
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<id>30</id>
<text>Innenseite des Ovda Regio, eines der großen Hochebenen, die den Venusäquator umringen.</text>
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<id>32</id>
<text>¶b Ovda Regio §∫≥°, §@§j™∫™˜¨P®™πD≥Ú¬∂™∫∞™¶a.</text>
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card_15987.xml
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<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37788 MGN-36 3/5/91 This Magellan image shows part the interior of Ovda Regio, one of the large highlands ringing the equator of Venus. Several tectonic events formed this complex block-fractured terrain. An underlying fabric of ridges and valleys strikes NE-SW. These ridges are spaced 10-20 kilometers (6-12 miles) apart and may have been caused by shortening of the crust at right angles to this trend. These structures are cut by throughgoing extension fractures trending NW-SE, suggesting a later episode of NE-SW extension. Lastly, the largest valleys, particularly the 20 kilometer (12 mile)-wide one extending across the image, were filled with dark material, probably lava. The complex internal fabric of Ovda Regio attests to a long history of tectonic deformation. This image, centered approximately at 1 S 81 E, measures 225 kilometers (140 miles) by 150 kilometers (90 miles) and was acquired by Magellan in November 1990. </text>
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<content>
<layer>background</layer>
<id>29</id>
<text>Intérieur de Ovda Regio, une des larges régions montagneuses allant autour de l'équateur de Vénus.</text>
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<content>
<layer>background</layer>
<id>31</id>
<text>Interior de Ovda Regio, uno de los grandes altiplanos que circundan el ecuador de Venus.</text>
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<content>
<layer>background</layer>
<id>30</id>
<text>Innenseite des Ovda Regio, eines der großen Hochebenen, die den Venusäquator umringen.</text>
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<id>32</id>
<text>¶b Ovda Regio §∫≥°, §@§j™∫™˜¨P®™πD≥Ú¬∂™∫∞™¶a.</text>
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card_15672.xml
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<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37788 MGN-36 3/5/91 This Magellan image shows part the interior of Ovda Regio, one of the large highlands ringing the equator of Venus. Several tectonic events formed this complex block-fractured terrain. An underlying fabric of ridges and valleys strikes NE-SW. These ridges are spaced 10-20 kilometers (6-12 miles) apart and may have been caused by shortening of the crust at right angles to this trend. These structures are cut by throughgoing extension fractures trending NW-SE, suggesting a later episode of NE-SW extension. Lastly, the largest valleys, particularly the 20 kilometer (12 mile)-wide one extending across the image, were filled with dark material, probably lava. The complex internal fabric of Ovda Regio attests to a long history of tectonic deformation. This image, centered approximately at 1 S 81 E, measures 225 kilometers (140 miles) by 150 kilometers (90 miles) and was acquired by Magellan in November 1990. </text>
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<content>
<layer>background</layer>
<id>29</id>
<text>Intérieur de Ovda Regio, une des larges régions montagneuses allant autour de l'équateur de Vénus.</text>
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<content>
<layer>background</layer>
<id>31</id>
<text>Interior de Ovda Regio, uno de los grandes altiplanos que circundan el ecuador de Venus.</text>
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<content>
<layer>background</layer>
<id>30</id>
<text>Innenseite des Ovda Regio, eines der großen Hochebenen, die den Venusäquator umringen.</text>
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<content>
<layer>background</layer>
<id>32</id>
<text>¶b Ovda Regio §∫≥°, §@§j™∫™˜¨P®™πD≥Ú¬∂™∫∞™¶a.</text>
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card_15602.xml
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<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37788 MGN-36 3/5/91 This Magellan image shows part the interior of Ovda Regio, one of the large highlands ringing the equator of Venus. Several tectonic events formed this complex block-fractured terrain. An underlying fabric of ridges and valleys strikes NE-SW. These ridges are spaced 10-20 kilometers (6-12 miles) apart and may have been caused by shortening of the crust at right angles to this trend. These structures are cut by throughgoing extension fractures trending NW-SE, suggesting a later episode of NE-SW extension. Lastly, the largest valleys, particularly the 20 kilometer (12 mile)-wide one extending across the image, were filled with dark material, probably lava. The complex internal fabric of Ovda Regio attests to a long history of tectonic deformation. This image, centered approximately at 1 S 81 E, measures 225 kilometers (140 miles) by 150 kilometers (90 miles) and was acquired by Magellan in November 1990. </text>
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<content>
<layer>background</layer>
<id>29</id>
<text>Intérieur de Ovda Regio, une des larges régions montagneuses allant autour de l'équateur de Vénus.</text>
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<content>
<layer>background</layer>
<id>31</id>
<text>Interior de Ovda Regio, uno de los grandes altiplanos que circundan el ecuador de Venus.</text>
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<content>
<layer>background</layer>
<id>30</id>
<text>Innenseite des Ovda Regio, eines der großen Hochebenen, die den Venusäquator umringen.</text>
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<content>
<layer>background</layer>
<id>32</id>
<text>¶b Ovda Regio §∫≥°, §@§j™∫™˜¨P®™πD≥Ú¬∂™∫∞™¶a.</text>
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card_15153.xml
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<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-36642 MGN-11 9/17/90 On September 15, 1990, the Magellan spacecraft started radar operations for its mapping mission at Venus. This image is taken from the first set of radar data collected in the normal operating mode. This Magellan radar image is of an impact crater in the Navka Region of Venus. The image is a mosaic of data taken from orbits 376 and 377 on September 15, 1990. The crater is located at 334.5 E. longitude, 21.4 S. latitude, and is about 9 x 12 kilometers (5 x 7 miles) in size. This crater is very unusual, and is in some ways different from anything seen elsewhere in the solar system. It is fresh, with a sharp rim, terraces on the walls, and a well- developed ejecta blanket. The rim, however, is distinctly kidney- shaped rather than circular, and the crater's fresh appearance suggests, that it formed with that shape at impact. The ejecta blanket is markedly non-symmetric, with lobes extending to the north (top) and south (bottom) of the image, and a major extension stretching to the east (right). On the crater floor are several smooth, flat, dark regions. The asymmetric shape of the ejecta blanket has been observed on other planets and in impact experiments, and probably indicates that the impactor struck the surface at a low, oblique angle. The impactor would have been moving from west to east, sending ejecta lobes off to either side and a long streamer in the forward direction. The truly unusual aspect of the crater is its shape. One possible explanation is that the impactor broke up as it passed through the dense Venusian atmosphere, causing several large chunks of material to strike the surface almost simultaneously in an irregular pattern. The dark patches on the crater floor may be solidified pools of molten rock generated by the impact, or could be volcanic material extruded some time after the crater's formation. </text>
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<content>
<layer>background</layer>
<id>29</id>
<text>Image radar Magellan d'un cratère inhabituel dans la région Navka de Vénus.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Imagen de radar desde Magallanes de un cráter poco común en la región Navka de Venus.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Radarbild eines auergew├╢hnlichen Aufschlagskrater in der Venus-Navkaregion.</text>
<text> MAGELLAN PROJECT OFFICE P-37601 2/19/91 This is a Magellan full-resolution radar mosaic of the Lavinia region of Venus. The mosaic is centered at 50 degrees south latitude, 345 degrees east longitude, and spans 540 kilometers (338 miles) north to south and 900 kilometers (563 miles) east to west. As with all Magellan images acquired thus far, the illumination of the radar is from the left-hand side of the image. This area shows a diverse set of geologic features. The bright area running from the upper right to the lower left is interpreted as part of a belt of ridges, formed by compression and thickening of the upper layers of the planet. The areas between ridges suggest flooding by radar dark (and thus presumably) smoother lavas. The varied textures of the lavas can be seen in the mottled appearance of the plains which are cut by the ridges; brighter, rougher flows are also quite common. The particularly bright flows in the lower right corner are the northern extension of Mylitta Fluctus. The bright ridges adjacent to Mylitta Fluctus at the bottom center of the image also appear to have been affected by the volcanic activity. Some of these bright features have been interpreted as down-dropped areas roughly 5 kilometers (3 miles) wide. This would imply a region of extension where the crust has been pulled apart and thus was more easily flooded by the later lava flows. The thinner fractures running from the upper left seem to end at the ridge belt in the center of this mosaic. These thinner fractures are a continuation of a pattern seen throughout much of Lavinia and suggest a pattern of compression over a very large region. At the bottom of the image, overlying the ridges, is an impact crater 10-15 kilometers (6-10 miles) in diameter. The double or overlapped crater structure and asymmetrical ejecta pattern suggests that the incoming body broke up shortly before it hit, leaving closely-spaced craters. The placement of the crater on top of the ridges implies it is younger than the ridges; in fact, the crater may be one of the youngest features in this image.</text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Pleine résolution radar mosaïque de régions Lavinia de Vénus géologiquement différentes.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Imagen mosaica de radar de resoluci├│n completa de la regi├│n Lavinia de Venus geol├│gicamente diversa.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Detailliertes Radar-Mosaik von verschiedenen geologischen Laviniaregionen der Venus.</text>
<text> MAGELLAN PROJECT OFFICE P-37601 2/19/91 This is a Magellan full-resolution radar mosaic of the Lavinia region of Venus. The mosaic is centered at 50 degrees south latitude, 345 degrees east longitude, and spans 540 kilometers (338 miles) north to south and 900 kilometers (563 miles) east to west. As with all Magellan images acquired thus far, the illumination of the radar is from the left-hand side of the image. This area shows a diverse set of geologic features. The bright area running from the upper right to the lower left is interpreted as part of a belt of ridges, formed by compression and thickening of the upper layers of the planet. The areas between ridges suggest flooding by radar dark (and thus presumably) smoother lavas. The varied textures of the lavas can be seen in the mottled appearance of the plains which are cut by the ridges; brighter, rougher flows are also quite common. The particularly bright flows in the lower right corner are the northern extension of Mylitta Fluctus. The bright ridges adjacent to Mylitta Fluctus at the bottom center of the image also appear to have been affected by the volcanic activity. Some of these bright features have been interpreted as down-dropped areas roughly 5 kilometers (3 miles) wide. This would imply a region of extension where the crust has been pulled apart and thus was more easily flooded by the later lava flows. The thinner fractures running from the upper left seem to end at the ridge belt in the center of this mosaic. These thinner fractures are a continuation of a pattern seen throughout much of Lavinia and suggest a pattern of compression over a very large region. At the bottom of the image, overlying the ridges, is an impact crater 10-15 kilometers (6-10 miles) in diameter. The double or overlapped crater structure and asymmetrical ejecta pattern suggests that the incoming body broke up shortly before it hit, leaving closely-spaced craters. The placement of the crater on top of the ridges implies it is younger than the ridges; in fact, the crater may be one of the youngest features in this image.</text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Pleine résolution radar mosaïque de régions Lavinia de Vénus géologiquement différentes.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Imagen mosaica de radar de resoluci├│n completa de la regi├│n Lavinia de Venus geol├│gicamente diversa.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Detailliertes Radar-Mosaik von verschiedenen geologischen Laviniaregionen der Venus.</text>
<text> MAGELLAN PROJECT OFFICE P-37601 2/19/91 This is a Magellan full-resolution radar mosaic of the Lavinia region of Venus. The mosaic is centered at 50 degrees south latitude, 345 degrees east longitude, and spans 540 kilometers (338 miles) north to south and 900 kilometers (563 miles) east to west. As with all Magellan images acquired thus far, the illumination of the radar is from the left-hand side of the image. This area shows a diverse set of geologic features. The bright area running from the upper right to the lower left is interpreted as part of a belt of ridges, formed by compression and thickening of the upper layers of the planet. The areas between ridges suggest flooding by radar dark (and thus presumably) smoother lavas. The varied textures of the lavas can be seen in the mottled appearance of the plains which are cut by the ridges; brighter, rougher flows are also quite common. The particularly bright flows in the lower right corner are the northern extension of Mylitta Fluctus. The bright ridges adjacent to Mylitta Fluctus at the bottom center of the image also appear to have been affected by the volcanic activity. Some of these bright features have been interpreted as down-dropped areas roughly 5 kilometers (3 miles) wide. This would imply a region of extension where the crust has been pulled apart and thus was more easily flooded by the later lava flows. The thinner fractures running from the upper left seem to end at the ridge belt in the center of this mosaic. These thinner fractures are a continuation of a pattern seen throughout much of Lavinia and suggest a pattern of compression over a very large region. At the bottom of the image, overlying the ridges, is an impact crater 10-15 kilometers (6-10 miles) in diameter. The double or overlapped crater structure and asymmetrical ejecta pattern suggests that the incoming body broke up shortly before it hit, leaving closely-spaced craters. The placement of the crater on top of the ridges implies it is younger than the ridges; in fact, the crater may be one of the youngest features in this image.</text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Pleine résolution radar mosaïque de régions Lavinia de Vénus géologiquement différentes.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Imagen mosaica de radar de resoluci├│n completa de la regi├│n Lavinia de Venus geol├│gicamente diversa.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Detailliertes Radar-Mosaik von verschiedenen geologischen Laviniaregionen der Venus.</text>
<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37296 12/14/90 Dark Halos Revealed Around Impact Craters: New Geologic Clocks for Venus? This Magellan image mosiac located in the Lavinia region shows the crater Carson, a 38 km (23 mile) diameter crater. The image is centered at about 24 degrees south latitude, 344 degrees longitude. Impact craters in the Magellan data are frequently surrounded by radar-dark halos. Several of these halos were noted to have a hyperbolic shape, extending hundreds of kilometers to the west of the craters. Five of these dark halos were also seen extending out from craters in Magellan emissivity data. Magellan emissivity data, derived from the altimeter data, provides information about the porosity (soil versus solid rock) and the composition of the surface. The darkness in the emissivity data indicates a very smooth surface, leading to the interpretation that these halos may be thick, smooth sediment deposits formed by the 'crushing' blow of the atmosphere associated with the incoming projectile that formed the impact crater. But why are only about 5% of the craters surrounded by these halos? On the surface of most planets, the population of impact craters can be used to obtain both relative and absolute surface ages. On Venus, as on Earth, there are relatively few craters, making relative age dating (comparing one region of the planet to another) statistically difficult. The number of craters on Venus indicates that the surface may be only about 400 million years old. The dark halos may indicate the very youngest craters on the planet- where the harsh conditions on Venus have not yet caused these dark halos to 'roughen up' and disappear. The halos could possibly be used as 'geologic clocks.' Volcanic flows or tectonic structures cutting one of these halos are interpreted to have occurred even more recently than the craters. This image shows such a situation, where flows associated with the crater cut across the halo, indicating a very young age. Scientists are continuing to identify these halos in the Magellan data, and use them to understand the geologic evolution of the surface. </text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Mosaïque Magellan de Crater Carson dans la région Lavinia montrant des halos inexpliqués.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Mosaico desde Magallanes del cráter Carson en la región Lavinia que muestra auréolas inexplicadas.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Magellan-Mosaik des Kraters Carson in der Laviniaregion mit unerklärten Höfen.</text>
<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37296 12/14/90 Dark Halos Revealed Around Impact Craters: New Geologic Clocks for Venus? This Magellan image mosiac located in the Lavinia region shows the crater Carson, a 38 km (23 mile) diameter crater. The image is centered at about 24 degrees south latitude, 344 degrees longitude. Impact craters in the Magellan data are frequently surrounded by radar-dark halos. Several of these halos were noted to have a hyperbolic shape, extending hundreds of kilometers to the west of the craters. Five of these dark halos were also seen extending out from craters in Magellan emissivity data. Magellan emissivity data, derived from the altimeter data, provides information about the porosity (soil versus solid rock) and the composition of the surface. The darkness in the emissivity data indicates a very smooth surface, leading to the interpretation that these halos may be thick, smooth sediment deposits formed by the 'crushing' blow of the atmosphere associated with the incoming projectile that formed the impact crater. But why are only about 5% of the craters surrounded by these halos? On the surface of most planets, the population of impact craters can be used to obtain both relative and absolute surface ages. On Venus, as on Earth, there are relatively few craters, making relative age dating (comparing one region of the planet to another) statistically difficult. The number of craters on Venus indicates that the surface may be only about 400 million years old. The dark halos may indicate the very youngest craters on the planet- where the harsh conditions on Venus have not yet caused these dark halos to 'roughen up' and disappear. The halos could possibly be used as 'geologic clocks.' Volcanic flows or tectonic structures cutting one of these halos are interpreted to have occurred even more recently than the craters. This image shows such a situation, where flows associated with the crater cut across the halo, indicating a very young age. Scientists are continuing to identify these halos in the Magellan data, and use them to understand the geologic evolution of the surface. </text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Mosaïque Magellan de Crater Carson dans la région Lavinia montrant des halos inexpliqués.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Mosaico desde Magallanes del cráter Carson en la región Lavinia que muestra auréolas inexplicadas.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Magellan-Mosaik des Kraters Carson inder Laviniaregion mit unerklärten Höfen.</text>
<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37296 12/14/90 Dark Halos Revealed Around Impact Craters: New Geologic Clocks for Venus? This Magellan image mosiac located in the Lavinia region shows the crater Carson, a 38 km (23 mile) diameter crater. The image is centered at about 24 degrees south latitude, 344 degrees longitude. Impact craters in the Magellan data are frequently surrounded by radar-dark halos. Several of these halos were noted to have a hyperbolic shape, extending hundreds of kilometers to the west of the craters. Five of these dark halos were also seen extending out from craters in Magellan emissivity data. Magellan emissivity data, derived from the altimeter data, provides information about the porosity (soil versus solid rock) and the composition of the surface. The darkness in the emissivity data indicates a very smooth surface, leading to the interpretation that these halos may be thick, smooth sediment deposits formed by the 'crushing' blow of the atmosphere associated with the incoming projectile that formed the impact crater. But why are only about 5% of the craters surrounded by these halos? On the surface of most planets, the population of impact craters can be used to obtain both relative and absolute surface ages. On Venus, as on Earth, there are relatively few craters, making relative age dating (comparing one region of the planet to another) statistically difficult. The number of craters on Venus indicates that the surface may be only about 400 million years old. The dark halos may indicate the very youngest craters on the planet- where the harsh conditions on Venus have not yet caused these dark halos to 'roughen up' and disappear. The halos could possibly be used as 'geologic clocks.' Volcanic flows or tectonic structures cutting one of these halos are interpreted to have occurred even more recently than the craters. This image shows such a situation, where flows associated with the crater cut across the halo, indicating a very young age. Scientists are continuing to identify these halos in the Magellan data, and use them to understand the geologic evolution of the surface. </text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Mosaïque Magellan de Crater Carson dans la région Lavinia montrant des halos inexpliqués.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Mosaico desde Magallanes del cráter Carson en la región Lavinia que muestra auréolas inexplicadas.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Magellan-Mosaik des Kraters Carson inder Laviniaregion mit unerklärten Höfen.</text>
<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-36644 MGN-12 9/17/90 On September 15, 1990, the Magellan spacecraft started radar operations for its mapping mission at Venus. This image is taken from the first set of radar data collected in the normal operating mode. These fault-bounded troughs were imaged by Magellan on orbit 147 on September 15, 1990. The image is of part of the Lavinia Region of Venus at 60 degrees south latitude, 347 degrees east longitude. The image is 28 kilometers (17 miles) wide and 75 kilometers (46 miles) long. This region is at the intersection of two tectonic trends. An extensive set of east-west trending fractures extends to the west (left) and a second set extends down to the south-southeast (lower right). The lines of pits suggest some igneous or volcanic activity accompanying the faulting. The prominent trough trending diagonally across the image is 5 kilometers (3.1 miles) wide and is 100 to 200 meters (300 to 600 feet) deep. </text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Carte radar Magellan de la région Lavinia de Vénus.</text>
</content>
<content>
<layer>background</layer>
<id>31</id>
<text>Imagen mosaica de radar de la regi├│n Lavinia de Venus.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Magellans Radaraufnahme der Venus-Laviniaregion</text>
<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-36547 MGN-6 8/23/90 This three-dimensional representation of brightness variations in a Magellan radar image of Golubkina crater enhances the structural features of the crater. Golubkina is 34 km (20.4 miles) in diameter, and is located at about 60.5 degrees north latitude, 287.2 degrees east longitude. Golubkina is characterized by terraced inner walls and a central peak, typical of large impact craters on the Earth, Moon and Mars. The terraced inner walls form at late stages in the formation of an impact crater, due to collapse of the initial cavity formed by the meteorite impact. The central peak forms due to rebound of the inner crater floor. </text>
</content>
<content>
<layer>background</layer>
<id>29</id>
<text>Vue en 3D de la brillance dans image radar Magellan du cratère Golubinka.</text>
</content>
<content>
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<text>Vista tridimensional de resplandor en imagen radar desde Magallanes del cráter Golubinka.</text>
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<id>30</id>
<text>3D-Ansicht der Helligkeit des Golubinka Kraters, -Magellan Radaraufnahme.</text>
<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-36711 MGN-17 9/25/90 One of the most useful Magellan standard data products is the full resolution mosaic, the F-MIDR (Full-Resolution Mosaicked Image Data Record). These products are mosaics of about 500 km (300 mile) segments of 30 or more individual image strips. This is a partial F-MIDR made from orbits 376 to 399, obtained between September 15 and September 18, 1990, part of the first orbits in which the Magellan flight team operated the radar system in the mapping mode. The mosaic is centered at 27 degrees south latitude, 339 degrees longitude, in the Lavinia region of Venus. Three large impact craters with diameters ranging from 37 kilometers (23 miles) to 50 kilometers (30 miles) can be seen located in a region of fractured plains. The craters show many features typical of meteorite impact craters, including rough, radar-bright ejecta, terraced inner walls and central peaks. Numerous domes of probable volcanic origin can be seen in the southeastern corner of the mosaic. The domes range in diameter from 1-12 kilometers (0.6-7 miles), and some have central pits typical of volcanic shields or cones. Resolution of the Magellan data is about 120 meters (400 feet). </text>
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<text>Pleine résolution mosaïque de trois larges cratères dans la région Lavinia de Vénus.</text>
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<text>Mosaico de resolución completa de tres cráteres de impacto en la región Lavinia de Venus.</text>
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<text>Detailliertes Mosaik von drei großen Aufschlagskratern in Venus' Laviniaregion.</text>
<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37264 12/5/90 This Magellan image covers a region 77 kilometers (46 miles) wide and 85 kilometers (51 miles) high. This image shows part of a long, open channel at 76.5 degrees north latitude, 335 degrees longitude in the Vires-akka Chasma, about 100 kilometers (60 miles) north of Freyja Montes, in the Denitsa Region of Venus. The channel ranges in width from less than 1 kilometer (3300 feet) to 4 kilometers (2.4 miles). The portion of the channel visible in this scene is over 120 kilometers (72 miles) long. Longitudinal scour features are visible within the channel, particularly where it makes abrupt turns. The channel may have been carved by very low viscosity lavas that were able to remain fluid over great distances and thermally erode pre-existing terrain due to the extreme temperatures at Venus' surface. </text>
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<text>Image Magellan d'un canal ouvert au nord de Freyja Montes, dans la région Denitsa de Vénus.</text>
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<text>Imagen desde Magallanes de cauce abierto al norte de los Freyja Montes, en la regi├│n Denitsa de Venus.</text>
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<text>Magellan-Bild: offener Kanal n├╢rdlich von Freyja Montes -Denitsaregion der Venus.</text>
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<text>¶b Freyja Montes •_√‰•¥∂}¿WπD™∫ Magellan πœπ≥, ¶b™˜¨P Denitsa ¶a∞œ.</text>
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<text> MAGELLAN PROJECT OFFICE P-37651 2/25/91 This mosaic of Magellan data in the Fortuna region of Venus, centered at 49 degrees north latitude, 2 degrees longitude, shows two coronae. Coronae are large circular or oval structures first identified in Soviet radar images of Venus. The structure on the left, Bahet Corona, is about 230 kilometers (138 miles) long and 150 kilometers (90 miles) across. A portion of Onatah Corona, over 350 kilometers (210 miles) in diameter, can be seen on the right of the mosaic. Both features are surrounded by a ring of ridges and troughs, which in places cut more radially-oriented fractures. The centers of the features also contain radial fractures as well as volcanic domes and flows. Coronae are thought to form due to the upwelling of hot material from deep in the interior of Venus. The two coronae may have formed at the same time over a single upwelling, or may indicate movement of the upwelling or the upper layers of the planet to the west over time. A 'pancake' dome, similar to low-relief domes see in the southern hemisphere, is located just to the southwest of Bahet. Resolution of the Magellan data is about 120 meters (400 feet). Jet Propulsion Laboratory California Institute of Technology National Aeronautics and Space Administration Pasadena, Calif. 91109</text>
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<text>Mosaïque Magellan de la région Fortuna de Vénus montrant deux Coronae, des structures ovales.</text>
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<text>Mosaico Magallanes de la regi├│n Fortuna de Venus que muestra dos Coronae, estructuras ovales.</text>
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<text>Magellan-Mosaik der Venus-Fortunaregion mit zwei Koronae, ovale Strukturen.</text>
<text> MAGELLAN PROJECT OFFICE P-37651 2/25/91 This mosaic of Magellan data in the Fortuna region of Venus, centered at 49 degrees north latitude, 2 degrees longitude, shows two coronae. Coronae are large circular or oval structures first identified in Soviet radar images of Venus. The structure on the left, Bahet Corona, is about 230 kilometers (138 miles) long and 150 kilometers (90 miles) across. A portion of Onatah Corona, over 350 kilometers (210 miles) in diameter, can be seen on the right of the mosaic. Both features are surrounded by a ring of ridges and troughs, which in places cut more radially-oriented fractures. The centers of the features also contain radial fractures as well as volcanic domes and flows. Coronae are thought to form due to the upwelling of hot material from deep in the interior of Venus. The two coronae may have formed at the same time over a single upwelling, or may indicate movement of the upwelling or the upper layers of the planet to the west over time. A 'pancake' dome, similar to low-relief domes see in the southern hemisphere, is located just to the southwest of Bahet. Resolution of the Magellan data is about 120 meters (400 feet). Jet Propulsion Laboratory California Institute of Technology National Aeronautics and Space Administration Pasadena, Calif. 91109</text>
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<text>Mosaïque Magellan de la région Fortuna de Vénus montrant deux Coronae, des structures ovales.</text>
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<text>Mosaico Magallanes de la regi├│n Fortuna de Venus que muestra dos Coronae, estructuras ovales.</text>
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<text>Magellan-Mosaik der Venus-Fortunaregion mit zwei Koronae, ovale Strukturen.</text>
<text> MAGELLAN PROJECT OFFICE P-37651 2/25/91 This mosaic of Magellan data in the Fortuna region of Venus, centered at 49 degrees north latitude, 2 degrees longitude, shows two coronae. Coronae are large circular or oval structures first identified in Soviet radar images of Venus. The structure on the left, Bahet Corona, is about 230 kilometers (138 miles) long and 150 kilometers (90 miles) across. A portion of Onatah Corona, over 350 kilometers (210 miles) in diameter, can be seen on the right of the mosaic. Both features are surrounded by a ring of ridges and troughs, which in places cut more radially-oriented fractures. The centers of the features also contain radial fractures as well as volcanic domes and flows. Coronae are thought to form due to the upwelling of hot material from deep in the interior of Venus. The two coronae may have formed at the same time over a single upwelling, or may indicate movement of the upwelling or the upper layers of the planet to the west over time. A 'pancake' dome, similar to low-relief domes see in the southern hemisphere, is located just to the southwest of Bahet. Resolution of the Magellan data is about 120 meters (400 feet). Jet Propulsion Laboratory California Institute of Technology National Aeronautics and Space Administration Pasadena, Calif. 91109</text>
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<text>Mosaïque Magellan de la région Fortuna de Vénus montrant deux Coronae, des structures ovales.</text>
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<text>Mosaico Magallanes de la regi├│n Fortuna de Venus que muestra dos Coronae, estructuras ovales.</text>
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<text>Magellan-Mosaik der Venus-Fortunaregion mit zwei Koronae, ovale Strukturen.</text>
<text> MAGELLAN PROJECT OFFICE P-38102 4/5/91 Arachnoids, among the more remarkable features found on Venus, are seen on radar-dark plains in this Magellan image mosaic in the Fortuna region. The image is centered at about 40 degrees north latitude, 18 degrees longitude. Arachnoids are circular to ovoid features with concentric rings and a complex network of fractures extending outward. The top image is a mosaic of Magellan radar images with a resolution of 120 meters. The MGN image is illuminated from the left at an angle of 35 degrees off vertical. The bottom image was obtained by the Soviet Venera 15/16 radar system. The Venera image has a resolution of about 1.5 kilometers (.9 mile). The bottom image is illuminated from the right side at an angle of 10 degrees off vertical. This image illustrates the importance of multiple mapping angles for some areas. Notice in the top image, the bright, irregular lava flows, just to the left of bottom center. The rough lava surface is bright at the Magellan incidence angle. The lava flows are not detected in the Venera image at the higher incidence angle which is less sensitive to roughness variations. However, the high angle Venera image reveals the topography which is not easily seen at the Magellan incidence angle. In the image, the arachnoids range in size from approximately 50 kilometers (29.9 miles) to 230 kilometers (137.7 miles) in diameter. Since arachnoids are similar in form but generally smaller than coronae (circular volcanic structures surrounded by a set of ridges and grooves as well as radial lines), one theory concerning their origin is that they are a precursor to coronae formation. The radar-bright lines extending for many kilometers may have been caused by an upwelling of magma from the interior of the planet which pushed up the surface to form "cracks." Radar-bright lava flows are present in the central part of this image, also indicative of volcanic activity in this area. Some of the fractures cut across these flows, indicating that the flows occurred before the fractures appeared; such relations between different structures provides good relative age dating of events. At present, arachnoids are found only on Venus. Jet Propulsion Laboratory California Institute of Technology National Aeronautics and Space Administration Pasadena, Calif. 91109 </text>
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<text>Mosaïque Magellan d'arachnoids, de fractures volcaniques, dans la région Fortuna de Vénus.</text>
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<text>Mosaico desde Magallanes de aracnoides, fracturas volcánicas, en la región Fortuna de Venus.</text>
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<text>Magellan-Mosaik von Arachnoiden und vulkanischen Br├╝chen in Venus' Fortunaregion.</text>
<text> MAGELLAN PROJECT OFFICE P-37501 1/21/91 Arachnoids, one of the more remarkable features found on Venus, are seen on radar-dark plains in this Magellan image mosaic in the Fortuna region. The image is centered at about 40 degrees north latitude, 18 degrees longitude. As the name suggests, arachnoids are circular to ovoid features with concentric rings and a complex network of fractures extending outward. In this image, the arachnoids range in size from approximately 50 kilometers (29.9 miles) to 230 kilometers (137.7 miles) in diameter. Since arachnoids are similar in form but generally smaller than coronae (circular volcanic structures surrounded by a set of ridges and grooves as well as radial lines), one theory concerning their origin is that they are a precursor to coronae formation. The radar-bright lines extending for many kilometers may have been caused by an upwelling of magma from the interior of the planet which pushed up the surface to form "cracks." Radar-bright lava flows are present in the central part of this image, also indicative of volcanic activity in this area. Some of the fractures cut across these flows, indicating that the flows occurred before the fractures appeared; such relations between different structures provides good relative age dating of events. At present, arachnoids are found only on Venus and can now be more closely studied with the high resolution (120 meter/0.07 mile) radar imagery from Magellan. Jet Propulsion Laboratory California Institute of Technology National Aeronautics and Space Administration Pasadena, Calif. 91109 </text>
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<text>Mosaïque Magellan d'arachnoids, de fractures volcaniques, dans la région Fortuna de Vénus.</text>
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<text>Mosaico desde Magallanes de aracnoides, fracturas volcánicas, en la región Fortuna de Venus.</text>
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<text>Magellan-Mosaik von Arachnoiden und vulkanischen Br├╝chen in Venus' Fortunaregion.</text>
<text> MAGELLAN PROJECT OFFICE P-37501 1/21/91 Arachnoids, one of the more remarkable features found on Venus, are seen on radar-dark plains in this Magellan image mosaic in the Fortuna region. The image is centered at about 40 degrees north latitude, 18 degrees longitude. As the name suggests, arachnoids are circular to ovoid features with concentric rings and a complex network of fractures extending outward. In this image, the arachnoids range in size from approximately 50 kilometers (29.9 miles) to 230 kilometers (137.7 miles) in diameter. Since arachnoids are similar in form but generally smaller than coronae (circular volcanic structures surrounded by a set of ridges and grooves as well as radial lines), one theory concerning their origin is that they are a precursor to coronae formation. The radar-bright lines extending for many kilometers may have been caused by an upwelling of magma from the interior of the planet which pushed up the surface to form "cracks." Radar-bright lava flows are present in the central part of this image, also indicative of volcanic activity in this area. Some of the fractures cut across these flows, indicating that the flows occurred before the fractures appeared; such relations between different structures provides good relative age dating of events. At present, arachnoids are found only on Venus and can now be more closely studied with the high resolution (120 meter/0.07 mile) radar imagery from Magellan. Jet Propulsion Laboratory California Institute of Technology National Aeronautics and Space Administration Pasadena, Calif. 91109 </text>
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<text>Mosaïque Magellan d'arachnoids, de fractures volcaniques, dans la région Fortuna de Vénus.</text>
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<text>Mosaico desde Magallanes de aracnoides, fracturas volcánicas, en la región Fortuna de Venus.</text>
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<id>30</id>
<text>Magellan-Mosaik von Arachnoiden und vulkanischen Br├╝chen in Venus' Fortunaregion.</text>
<text> MAGELLAN PROJECT OFFICE P-37501 1/21/91 Arachnoids, one of the more remarkable features found on Venus, are seen on radar-dark plains in this Magellan image mosaic in the Fortuna region. The image is centered at about 40 degrees north latitude, 18 degrees longitude. As the name suggests, arachnoids are circular to ovoid features with concentric rings and a complex network of fractures extending outward. In this image, the arachnoids range in size from approximately 50 kilometers (29.9 miles) to 230 kilometers (137.7 miles) in diameter. Since arachnoids are similar in form but generally smaller than coronae (circular volcanic structures surrounded by a set of ridges and grooves as well as radial lines), one theory concerning their origin is that they are a precursor to coronae formation. The radar-bright lines extending for many kilometers may have been caused by an upwelling of magma from the interior of the planet which pushed up the surface to form "cracks." Radar-bright lava flows are present in the central part of this image, also indicative of volcanic activity in this area. Some of the fractures cut across these flows, indicating that the flows occurred before the fractures appeared; such relations between different structures provides good relative age dating of events. At present, arachnoids are found only on Venus and can now be more closely studied with the high resolution (120 meter/0.07 mile) radar imagery from Magellan. Jet Propulsion Laboratory California Institute of Technology National Aeronautics and Space Administration Pasadena, Calif. 91109 </text>
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<text>Mosaïque Magellan d'arachnoids, de fractures volcaniques, dans la région Fortuna de Vénus.</text>
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<text>Mosaico desde Magallanes de aracnoides, fracturas volcánicas, en la región Fortuna de Venus.</text>
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<text>Magellan-Mosaik von Arachnoiden und vulkanischen Br├╝chen in Venus' Fortunaregion.</text>
<text> MAGELLAN PROJECT OFFICE P-38088 4/5/91 This is a 225 meter per pixel Magellan radar image mosaic of Venus, centered at 47 degrees south latitude, 25 degrees east longitude in the Lada region. The scene is approximately 550 kilometers (341 miles) east-west by 630 kilometers (391 miles) north-south. The mosaic shows a system of east-trending radar- bright and dark lava flows encountering and breaching a north- trending ridge belt (left of center). Upon breaching the ridge belt, the lavas pool in a vast, radar-bright deposit (covering approximately 100,000 square kilometers [right side of image]). The source caldera for the lava flows, named Ammavaru, lies approximately 300 kilometers (186 miles) west of the scene. Jet Propulsion Laboratory California Institute of Technology National Aeronautics and Space Administration Pasadena, Calif. 91109 </text>
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<text>Image radar Magellan mosaïque de Vénus montrant des coulées et étangs de lave.</text>
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<text>Imagen mosaica de radar desde Magallanes tomada de Venus que muestra corrientes y pozas.</text>
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<text>Magellan Radarbild-Mosaik der Venus, das Lavafl├╝sse und Poole darstellt.</text>
<text> MAGELLAN PROJECT OFFICE P-38088 4/5/91 This is a 225 meter per pixel Magellan radar image mosaic of Venus, centered at 47 degrees south latitude, 25 degrees east longitude in the Lada region. The scene is approximately 550 kilometers (341 miles) east-west by 630 kilometers (391 miles) north-south. The mosaic shows a system of east-trending radar- bright and dark lava flows encountering and breaching a north- trending ridge belt (left of center). Upon breaching the ridge belt, the lavas pool in a vast, radar-bright deposit (covering approximately 100,000 square kilometers [right side of image]). The source caldera for the lava flows, named Ammavaru, lies approximately 300 kilometers (186 miles) west of the scene. Jet Propulsion Laboratory California Institute of Technology National Aeronautics and Space Administration Pasadena, Calif. 91109 </text>
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<text>Image radar Magellan mosaïque de Vénus montrant des coulées et étangs de lave.</text>
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<text>Imagen mosaica de radar desde Magallanes tomada de Venus que muestra corrientes y pozas.</text>
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<text>Magellan Radarbild-Mosaik der Venus, das Lavafl├╝sse und Poole darstellt.</text>
<text> MAGELLAN PROJECT OFFICE P-38088 4/5/91 This is a 225 meter per pixel Magellan radar image mosaic of Venus, centered at 47 degrees south latitude, 25 degrees east longitude in the Lada region. The scene is approximately 550 kilometers (341 miles) east-west by 630 kilometers (391 miles) north-south. The mosaic shows a system of east-trending radar- bright and dark lava flows encountering and breaching a north- trending ridge belt (left of center). Upon breaching the ridge belt, the lavas pool in a vast, radar-bright deposit (covering approximately 100,000 square kilometers [right side of image]). The source caldera for the lava flows, named Ammavaru, lies approximately 300 kilometers (186 miles) west of the scene. Jet Propulsion Laboratory California Institute of Technology National Aeronautics and Space Administration Pasadena, Calif. 91109 </text>
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<text>Image radar Magellan mosaïque de Vénus montrant des coulées et étangs de lave.</text>
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<text>Imagen mosaica de radar desde Magallanes tomada de Venus que muestra corrientes y pozas.</text>
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<text>Magellan Radarbild-Mosaik der Venus, das Lavafl├╝sse und Poole darstellt.</text>
<text> MAGELLAN PROJECT OFFICE P-38088 4/5/91 This is a 225 meter per pixel Magellan radar image mosaic of Venus, centered at 47 degrees south latitude, 25 degrees east longitude in the Lada region. The scene is approximately 550 kilometers (341 miles) east-west by 630 kilometers (391 miles) north-south. The mosaic shows a system of east-trending radar- bright and dark lava flows encountering and breaching a north- trending ridge belt (left of center). Upon breaching the ridge belt, the lavas pool in a vast, radar-bright deposit (covering approximately 100,000 square kilometers [right side of image]). The source caldera for the lava flows, named Ammavaru, lies approximately 300 kilometers (186 miles) west of the scene. Jet Propulsion Laboratory California Institute of Technology National Aeronautics and Space Administration Pasadena, Calif. 91109 </text>
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<text>Image radar Magellan mosaïque de Vénus montrant des coulées et étangs de lave.</text>
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<text>Imagen mosaica de radar desde Magallanes tomada de Venus que muestra corrientes y pozas.</text>
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<text>Magellan Radarbild-Mosaik der Venus, das Lavafl├╝sse und Poole darstellt.</text>
<text> MAGELLAN PROJECT OFFICE P-38088 4/5/91 This is a 225 meter per pixel Magellan radar image mosaic of Venus, centered at 47 degrees south latitude, 25 degrees east longitude in the Lada region. The scene is approximately 550 kilometers (341 miles) east-west by 630 kilometers (391 miles) north-south. The mosaic shows a system of east-trending radar- bright and dark lava flows encountering and breaching a north- trending ridge belt (left of center). Upon breaching the ridge belt, the lavas pool in a vast, radar-bright deposit (covering approximately 100,000 square kilometers [right side of image]). The source caldera for the lava flows, named Ammavaru, lies approximately 300 kilometers (186 miles) west of the scene. Jet Propulsion Laboratory California Institute of Technology National Aeronautics and Space Administration Pasadena, Calif. 91109 </text>
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<text>Image radar Magellan mosaïque de Vénus montrant des coulées et étangs de lave.</text>
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<text>Imagen mosaica de radar desde Magallanes tomada de Venus que muestra corrientes y pozas.</text>
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<text>Magellan Radarbild-Mosaik der Venus, das Lavafl├╝sse und Poole darstellt.</text>
<text> MAGELLAN PROJECT OFFICE P-38088 4/5/91 This is a 225 meter per pixel Magellan radar image mosaic of Venus, centered at 47 degrees south latitude, 25 degrees east longitude in the Lada region. The scene is approximately 550 kilometers (341 miles) east-west by 630 kilometers (391 miles) north-south. The mosaic shows a system of east-trending radar- bright and dark lava flows encountering and breaching a north- trending ridge belt (left of center). Upon breaching the ridge belt, the lavas pool in a vast, radar-bright deposit (covering approximately 100,000 square kilometers [right side of image]). The source caldera for the lava flows, named Ammavaru, lies approximately 300 kilometers (186 miles) west of the scene. Jet Propulsion Laboratory California Institute of Technology National Aeronautics and Space Administration Pasadena, Calif. 91109 </text>
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<text>Image radar Magellan mosaïque de Vénus montrant des coulées et étangs de lave.</text>
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<text>Imagen mosaica de radar desde Magallanes tomada de Venus que muestra corrientes y pozas.</text>
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<text>Magellan Radarbild-Mosaik der Venus, das Lavafl├╝sse und Poole darstellt.</text>
<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37786 MGN-34 3/5/91 Thirty-six orbits of full-resolution data from the northern edge of central Alpha Regio are shown in this image. The image width is about 600 kilometers (375 miles). The bright lineated terrain is a series of troughs, ridges, and faults that are oriented in many directions. The lengths of these features generally range from 10 kilometers (6.3 miles) to 50 kilometers (31.3 miles). The topographic elevation within Alpha Regio varies over a range of 4 kilometers (2.5 miles). Local topographic lows, whose outlines are generally controlled by structures within the central region, are relatively radar-dark and filled with volcanic lavas. Source vents for this volcanism appear as bright spots within the smooth plains units. A distinct example of late-stage deformation of Alpha is the narrow band of southwest-northeast trending faults that disrupt older terrain between -20 degrees and -22 degrees latitude. Another interesting feature is the 35 kilometers (21.9 miles) diameter volcanic edifice located at the upper right of the image. The center of the volcano is a local topographic low and its western edge appears to be breached. </text>
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<text>Images du versant nord du centre d'Alpha Regio durant 36 orbites.</text>
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<text>Imágenes del límite norteño de la Alpha Regio central durante 36 órbitas.</text>
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<text>Bilder der nördlichen Kante des zentralen Alpha Regio während des 36-Orbits</text>
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<text>Alpha Regio §§§fl¶b 36 ≠”≠yπD™∫•_√‰√‰Ωtπœπ≥.</text>
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<text>㇠êØ</text>
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<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37786 MGN-34 3/5/91 Thirty-six orbits of full-resolution data from the northern edge of central Alpha Regio are shown in this image. The image width is about 600 kilometers (375 miles). The bright lineated terrain is a series of troughs, ridges, and faults that are oriented in many directions. The lengths of these features generally range from 10 kilometers (6.3 miles) to 50 kilometers (31.3 miles). The topographic elevation within Alpha Regio varies over a range of 4 kilometers (2.5 miles). Local topographic lows, whose outlines are generally controlled by structures within the central region, are relatively radar-dark and filled with volcanic lavas. Source vents for this volcanism appear as bright spots within the smooth plains units. A distinct example of late-stage deformation of Alpha is the narrow band of southwest-northeast trending faults that disrupt older terrain between -20 degrees and -22 degrees latitude. Another interesting feature is the 35 kilometers (21.9 miles) diameter volcanic edifice located at the upper right of the image. The center of the volcano is a local topographic low and its western edge appears to be breached. </text>
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<text>Images du versant nord du centre d'Alpha Regio durant 36 orbites.</text>
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<text>Imágenes del límite norteño de la Alpha Regio central durante 36 órbitas.</text>
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<id>30</id>
<text>Bilder der nördlichen Kante des zentralen Alpha Regio während des 36-Orbits.</text>
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<text>Alpha Regio §§§fl¶b 36 ≠”≠yπD™∫•_√‰√‰Ωtπœπ≥.</text>
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<text>㇠êØ</text>
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card_5272.xml
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<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37786 MGN-34 3/5/91 Thirty-six orbits of full-resolution data from the northern edge of central Alpha Regio are shown in this image. The image width is about 600 kilometers (375 miles). The bright lineated terrain is a series of troughs, ridges, and faults that are oriented in many directions. The lengths of these features generally range from 10 kilometers (6.3 miles) to 50 kilometers (31.3 miles). The topographic elevation within Alpha Regio varies over a range of 4 kilometers (2.5 miles). Local topographic lows, whose outlines are generally controlled by structures within the central region, are relatively radar-dark and filled with volcanic lavas. Source vents for this volcanism appear as bright spots within the smooth plains units. A distinct example of late-stage deformation of Alpha is the narrow band of southwest-northeast trending faults that disrupt older terrain between -20 degrees and -22 degrees latitude. Another interesting feature is the 35 kilometers (21.9 miles) diameter volcanic edifice located at the upper right of the image. The center of the volcano is a local topographic low and its western edge appears to be breached. </text>
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<text>Images du versant nord du centre d'Alpha Regio durant 36 orbites.</text>
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<text>Imágenes del límite norteño de la Alpha Regio central durante 36 órbitas.</text>
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<text>Bilder der nördlichen Kante des zentralen Alpha Regio während des 36-Orbits.</text>
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<id>32</id>
<text>Alpha Regio §§§fl¶b 36 ≠”≠yπD™∫•_√‰√‰Ωtπœπ≥.</text>
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<text>㇠êØ</text>
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<text>JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION PASADENA, CALIF. 91109 PHOTO CAPTION MAGELLAN P-37786 MGN-34 3/5/91 Thirty-six orbits of full-resolution data from the northern edge of central Alpha Regio are shown in this image. The image width is about 600 kilometers (375 miles). The bright lineated terrain is a series of troughs, ridges, and faults that are oriented in many directions. The lengths of these features generally range from 10 kilometers (6.3 miles) to 50 kilometers (31.3 miles). The topographic elevation within Alpha Regio varies over a range of 4 kilometers (2.5 miles). Local topographic lows, whose outlines are generally controlled by structures within the central region, are relatively radar-dark and filled with volcanic lavas. Source vents for this volcanism appear as bright spots within the smooth plains units. A distinct example of late-stage deformation of Alpha is the narrow band of southwest-northeast trending faults that disrupt older terrain between -20 degrees and -22 degrees latitude. Another interesting feature is the 35 kilometers (21.9 miles) diameter volcanic edifice located at the upper right of the image. The center of the volcano is a local topographic low and its western edge appears to be breached. </text>
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<text>Images du versant nord du centre d'Alpha Regio durant 36 orbites.</text>
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<text>Imágenes del límite norteño de la Alpha Regio central durante 36 órbitas.</text>
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<text>Bilder der nördlichen Kante des zentralen Alpha Regio während des 36-Orbits.</text>
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<id>32</id>
<text>Alpha Regio §§§fl¶b 36 ≠”≠yπD™∫•_√‰√‰Ωtπœπ≥.</text>
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<text>MAGELLAN PROJECT OFFICE P-38143 4/19/91 This crater, partly flooded by volcanic lavas, was mapped by Magellan on September 20, 1990 during orbits 411 through 418. It is located in the Lavinia region of Venus at 59.5 degrees south latitude and 354.5 east longitude. It is one of the very few impact craters that has been documented by Magellan to be actually in the process of elimination by volcanic resurfacing, and with a diameter of 63 kilometers (39 miles), it is the largest of these craters. The large, trough-like depression on the southwest (lower left) side is a rille or channel through which lava once flowed. A remnant of rough radial ejecta is preserved outside the crater's southeast rim. The presence of partly lava-flooded craters, such as this, are important to our understanding of the rate of resurfacing on Venus by volcanism. Resolution of the Magellan data is about 120 meters (400 feet). Alcott, the name proposed for this crater, honors Louisa May Alcott, American author (1832-1888). Proposed names for all features on planetary bodies are provisional until formally adopted by the International Astronomical Union. Jet Propulsion Laboratory California Institute of Technology National Aeronautics and Space Administration Pasadena, Calif. 91109 </text>
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<text>Vue d'un cratère, partiellement inondé avec de la lave volcanique, dans la région Lavinia de Vénus.</text>
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<text>Vista de un cráter, parcialmente inundado de lava, en la región Lavinia de Venus.</text>
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<id>30</id>
<text>Sicht auf einen Krater, z.T. mit vulkanischer Lava geflutet. -Venus Lavinaregion.</text>
<text>MAGELLAN PROJECT OFFICE P-38143 4/19/91 This crater, partly flooded by volcanic lavas, was mapped by Magellan on September 20, 1990 during orbits 411 through 418. It is located in the Lavinia region of Venus at 59.5 degrees south latitude and 354.5 east longitude. It is one of the very few impact craters that has been documented by Magellan to be actually in the process of elimination by volcanic resurfacing, and with a diameter of 63 kilometers (39 miles), it is the largest of these craters. The large, trough-like depression on the southwest (lower left) side is a rille or channel through which lava once flowed. A remnant of rough radial ejecta is preserved outside the crater's southeast rim. The presence of partly lava-flooded craters, such as this, are important to our understanding of the rate of resurfacing on Venus by volcanism. Resolution of the Magellan data is about 120 meters (400 feet). Alcott, the name proposed for this crater, honors Louisa May Alcott, American author (1832-1888). Proposed names for all features on planetary bodies are provisional until formally adopted by the International Astronomical Union. Jet Propulsion Laboratory California Institute of Technology National Aeronautics and Space Administration Pasadena, Calif. 91109 </text>
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<id>29</id>
<text>Vue d'un cratère, partiellement inondé avec de la lave volcanique, dans la région Lavinia de Vénus.</text>
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<id>31</id>
<text>Vista de un cráter, parcialmente inundado de lava, en la región Lavinia de Venus.</text>
</content>
<content>
<layer>background</layer>
<id>30</id>
<text>Sicht auf einen Krater, z.T. mit vulkanischer Lava geflutet. -Venus Lavinaregion.</text>
<text>MAGELLAN PROJECT OFFICE P-38143 4/19/91 This crater, partly flooded by volcanic lavas, was mapped by Magellan on September 20, 1990 during orbits 411 through 418. It is located in the Lavinia region of Venus at 59.5 degrees south latitude and 354.5 east longitude. It is one of the very few impact craters that has been documented by Magellan to be actually in the process of elimination by volcanic resurfacing, and with a diameter of 63 kilometers (39 miles), it is the largest of these craters. The large, trough-like depression on the southwest (lower left) side is a rille or channel through which lava once flowed. A remnant of rough radial ejecta is preserved outside the crater's southeast rim. The presence of partly lava-flooded craters, such as this, are important to our understanding of the rate of resurfacing on Venus by volcanism. Resolution of the Magellan data is about 120 meters (400 feet). Alcott, the name proposed for this crater, honors Louisa May Alcott, American author (1832-1888). Proposed names for all features on planetary bodies are provisional until formally adopted by the International Astronomical Union. Jet Propulsion Laboratory California Institute of Technology National Aeronautics and Space Administration Pasadena, Calif. 91109 </text>
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<content>
<layer>background</layer>
<id>29</id>
<text>Vue d'un cratère, partiellement inondé avec de la lave volcanique, dans la région Lavinia de Vénus.</text>
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<id>31</id>
<text>Vista de un cráter, parcialmente inundado de lava, en la región Lavinia de Venus.</text>
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<content>
<layer>background</layer>
<id>30</id>
<text>Sicht auf einen Krater, z.T. mit vulkanischer Lava geflutet. -Venus Lavinaregion.</text>
<text>This image shows a portion of the Akna Mountains, which form the western edge of Lakshmi Planum. The crater Wanda has a diameter of 22 km. While the crater does not seem deformed by tectonic activity, material from adjacent mountain areas appear to have collapsed into it. The ridge of mountains to the west of Wanda is about 8 km in width. The image is about 200 km long and 125 km wide. It is centered at 71.5N lat., 324 east long.</text>
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<text>Montagnes Akna qui forment le versant ouest de Lakshmi Planum comprenant le cratère Wanda.</text>
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<content>
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<text>Cordillera Akna que forma el límite occidental del Planum Lakshmi inclusive del cráter Wanda.</text>
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<content>
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<id>30</id>
<text>die Akna-Berge, die die westliche Kante des Lakshmi Planum mit dem Krater Wanda bilden.</text>
<text>••••••••••••Arcade GamesThe Best of Internet Arcade Games CD-ROM contains over 600 MB of Windows and DOS games from the Internet. The most popular PC arcade and video games are on this CD. Included are shareware* versions and demos for DOS: Doom by iD Software, Descent by Parallax Software, Flying Carpet by Bullfrog Productions, Heretic by iD & Raven Software, Dark Forces by LucasArts, Ltd, Quarantine by Gametek & Imagexcel, Blake Stone by Jam Productions & Apogee, Tie Fighter by LucasArts, Ltd., Wolfenstein-3D by iD & Apogee, Wacky Wheels by Apogee Software, and Mutant Space Bats of Doom by Pop Software. For Windows, the following are among the top hits on the CD-ROM: Missile Command, Asteroids, Tetris, Video Poker, NCC-1701 Star Trek, Checkers, Chess, MahJongg, and Entombed demo by Impulse Softwart.••••••••••••BlowfishBlowfish OS/2 CD-ROM is a large collection of shareware* and freeware utility programs for IBM’s OS/2 operating system.The Blowfish OS/2 disc includes system and file management utilities, text editors and programming tools and other programs and files for OS/2. The CD-ROM comes with a viewer which lets the user browse through the files with an easy to use graphical interface and then copy files onto the hard drive. All of the files are uncompressed and ready to use and have been categorized for quick and easy access.A special feature of the CD-ROM is the inclusion of Hippix software, which is an OS/2 implementation of many of the Posix commands and libraries like awk, diff, mv, sort, fflush, kill, write, etc. (Posix is an IEEE standard that comprises many of the commands and utilities that Unix® systems contain.)••••••••••••Clip Art Palette The C\lip Art Palette CD-ROM contains more than 1800 high quality, royalty free computer graphics collected from some of the best sites on the Internet. The images are provided in PICT, TIFF, EPS and BMP formats and the disk includes a Windows viewer. The viewer allows users to view pictures in bitmap mode, to view the interface in other languages and has menus for ‘help’ and ‘select categories’.The clip art on this disk can be imported or pasted into word processing, graphics and desktop publishing programs like Microsoft Word, WordPerfect, QuarkXPress, Pagemaker, CorelDRAW and others. The disk also contains a copy of Adobe Printshop Tryout for Macintosh and Windows users. The trial version is fullly functional, except that the ‘save’ and ‘print’ functions have been disabled.••••••••••••Fonts & FacesThis disc offers a broad selection of TrueType fonts and typefaces for Windows and Macintosh computers. The fonts have been divided into four categories: traditional, display, script and picture.Traditional Fonts:Made up of fonts from or based on the five basic families, Old Style, Transitional, Modern, Egyptian and Contemporary. From the antique feel of Garamond and Caslon to the modern sans serif style of Helvetica and Avante Garde. (note: we can change these names later if necessary). Serif type faces that are appropriate for long blocks of text; the serifs make the type more readable, guiding the reader's eye comfortably to the next word. The sans serifs work well with headlines and titles and are also good for documents where you don't want the text to interfere with the message, i.e. spreadsheets, graphs, etc.Display Fonts: Decorative fonts designed to attract the eye and set a mood come under this category. Display fonts are good for headlines, titles, posters and creating contrast between headings and the body text.Script Fonts:Fonts that imitate handwriting, from the wide brush style to delicate and spidery. Good for invitations or formal documents.Picture Fonts: These are fonts that typically carry meaning without being phonetic. Examples include Zingbat and Symbol.••••••••••••FontAsia TextProFonts and word processing programs for Japanese, Korean, Chinese and other Asian languages.This CD-ROM is scheduled to ship in June 1995.••••••••••••HyperStacksHyperStacks CD-ROM is a collection of over 1000 HyperCard stacks. HyperStacks CD-ROM includes public domain and shareware* games, personal organizers, books, and educational stacks, many incorporating graphics, animation, audio, and video. There are also some HyperCard-based tools as well as sample scripts and code for the advanced Macintosh user. The stacks on the CD-ROM have been culled from Macintosh libraries at several sites on the Internet, which is the immense network of computers connecting universities and research institutes around the world.HyperStacks CD-ROM is priced at $29.95 and is available directly from Pacific HiTech and leading retail outlets.*Shareware programs require separate payment to the author if found userful.••••••••••••Info-Mac 5Info-Mac V is amazing assortment of public domain and shareware* files downloaded in December 1994 from the Internet site at Stanford University's Info-Mac archive, the most up-to-date and comprehensive collection of Macintosh software available. Featuring a new, easy to use interface and containing over 1 GB of all-new material, this latest edition of the popular Info-Mac CD is indexed with FreeText, EasyView and OnLocation for instant access. Brief descriptions of each of the programs on the disc allow users to survey the vast amount of information quickly and efficiently. All of the files have been indexed, virus-checked and uncompressed, so that many of the files can be run directly from the CD-ROM. The disc saves users the considerable time and expense of selecting and downloading files themselves.The 20,000 files on the two disc set include about 2000 programs. Among them, users will find countless useful applications, desk accessories, games, virus-detection programs, commercial demos, graphics, sounds, Quicktime movies, fonts, HyperCard stacks, source code samples, and Internet periodicals.A previous release of the Info-Mac CD-ROM was listed in the “Top 50 CD-ROMs” feature in MacUser magazine (date) as one of the best bargains around. It has been featured in several reviews by leading magazines like MacUser and CD-ROM World, and has won acclaim as the top Macintosh public domain/shareware CD-ROM. The latest release, composed entirely of new files and updated versions, promises to be an even bigger success. Priced at $49.95, it compares favorably with competing discs in the $100 range.*Shareware programs require separate payment to the author if found userful.••••••••••••JupiterJupiter Impact CD-ROM will allow you to experience the explosive excitement of a comet striking our galaxy's largest planet. The Jupiter Impact CD-ROM documents the Shoemaker-Levy Comet's collision with Jupiter during the summer of 1994, from the comet's discovery and fiery approach to its explosion with the planet's surface and aftermath of its impact.Hundreds of photographs, images and educational information from the Internet's NASA archive, Hubble Space Telescope and observatories around the world commemorate the historic event. In addition, several movies, video clips, and simulations will let you watch this spectacular event unfold from the safety of your computer screen.The images are in GIF, BMP and PICT formats with graphics viewers for both Macintosh® and Windows™ users. The video is in MPEG and Quick Time formats.••••••••••••Linux Dev KitLinux Developers' Kit contains tools and software for the Linux operating system, a POSIX-based multi-tasking operating system for PCs with 386, 486 or Pentium processors.The most important Linux archives on the Internet are contained in this set. It comes complete with all of the tools needed to connect to the Internet through SLIP, PPP, or Term.The multi-disc set features the Slackware, Bogus, SLS, Debian, and MCC installation packages; Japanese Extensions to Linux; and all of the documentation available for Linux. It also features a complete mirror of Sunsite.unc.edu and over half of Tsx-11.mit.edu. There is very little duplication between the two archives.Because the Linux development community is actively updating the Linux operating system and applications for it, keeping up to date with the latest developments can be a challenge. Pacific HiTech offers a subscription service that provides users with the latest major updates as they occur. The subscription price is $12.95 per update. The regular price for the multi-disc set is $19.95. For LInux newcomers, it is recommended that you purchase the companion book, Linux Installation Guide, by Matt Welsh, available from Pacific HiTech at $12.95.••••••••••••Linux Runtime SystemThe Linux Run Time System CD-ROM contains an uncompressed, "ready to run" Linux system compiled with useful applications from the Linux archives that can be executed directly from the disc. Included on the CD are the following: Andrew Text Processing system, GCC, G++, X-Windows, games (including Doom), Tcl/Tk, Perl, POV-Ray, Radiance, Rayshade, libraries and documentation.••••••••••••MacGamesAll of the games on MacGames CD-ROM have been selected from Stanford University’s Sumex-Aim Info-Mac archive, the foremost repository of Macintosh public domain and shareware* software on the Internet. MacGames CD-ROM includes Bolo, arcade games, word games, commercial demos and card games. The friendly Pacific HiTech user-interface lets you find what you’re looking for with speed and ease. Since the programs have been uncompressed, many can be run directly form the CD. With several hundred of the most recent top Macintosh games available, there is something for everyone who likes having fun on their Macintosh.MacWorld USA distributed a special free version of the disc with their January 1995 issue, and MacWorld UK featured the disc on the cover of their 1994 Christmas issue.*Shareware programs require separate payment to the author if found userful.••••••••••••MacSourceMacSource CD-ROM is a collection of over 640 MB of tools and source code for Macintosh programmers.A programming and development disc, MacSource CD-ROM, includes samples in C, Pascal, and other programming languages. In also contains programming tools, utilities, information on Macintosh software and hardware, and related technical documentation. Most of the software included on the disc is in the public domain, although there are some shareware* programs and utilities.The data was gathered from leading Macintosh sites on the Internet, the world-wide network of computers connecting research labs, universities and government agencies. Designed specifically for Macintosh programmers and developers, the disc is the most up-to-date and comprehensive CD-ROM of its kind on the market. Given the current lack of such Macintosh CD-ROM titles, it should be a welcomed by the programming community as an invaluable resource.MacSource CD-ROM is priced at $29.95 and is available directly from Pacific HiTech and leading retail outlets.*Shareware programs require separate payment to the author if found userful.••••••••••••MPEGIAThe MPEGIA CD-ROM is the first collection of MPEG movies from the Internet to be produced on CD-ROM. (MPEG has become a standard for cross-platform digital compressed video. )Categories of movies on this CD-ROM include Astronomy, Nature, Digital Simulations, Mathematics, People and Geography. Some MPEGs contain only video, but many contain audio and video within the same package. Also on the MPEGIA CD-ROM are included shareware* and freeware MPEG viewers for all popular computer platforms (DOS, Windows, Macintosh, Unix/X11).All of the files on the CD-ROM are also available on PHT’s Internet site (ftp.pht.com).*Shareware programs require separate payment to the author if found userful.••••••••••••Norman Bosworth Vol 1The Norman Bosworth Photography Series is a two volume collection of royalty free photographs for graphic artists, desktop publishers and multi-media professionals, who need high quality images. The images are in 300dpi and 72dpi resolutions and are in TIFF, BMP and PICT formats. Graphics viewers for both Macintosh® and Windows™ users are provided on these hybrid disks.Volume One: Light of Days contains background images, desert scenery, seascapes, people, mountains, leaves, fireworks, buildings, deep canyons and sunsets. One hundred photographs in TIFF, BMP, and PICT formats in 300 dpi and 72 dpi resolution are included.The Norman Bosworth images can be used in print and digital publications, video presentations or multimedia works on a royalty-free basis with the exception that they cannot be used as a primary commercial object in any derivative products.••••••••••••Norman Bosworth Vol 2The Norman Bosworth Photography Series is a two volume collection of royalty free photographs for graphic artists, desktop publishers and multi-media professionals, who need high quality images. The images are in 300dpi and 72dpi resolutions and are in TIFF, BMP and PICT formats. Graphics viewers for both Macintosh® and Windows™ users are provided on these hybrid disks.Volume Two: Desert Sculptures brings you stunning imagery from Arches and Bryce Canyon national parks in the Great American Southwest Desert. Images of graceful curving arches, wind-blown buttes, jutting pinnacles, swirling sandstone and desert plants make up this CD-ROM. Mr. Bosworth has used his talent to capture nature's stark masterpieces of wind, rain and time. A valuable addition to any photography collection.The Norman Bosworth images can be used in print and digital publications, video presentations or multimedia works on a royalty-free basis with the exception that they cannot be used as a primary commercial object in any derivative products.••••••••••••NTIANTIA is a CD-ROM containing a broad selection of programs and utilities for Windows NT.This is the first Windows NT public domain and shareware* collection on CD-ROM, with hundreds of useful programs and utilities from the NTIA site on the Internet. As a special feature, it also contains Hippix™ for NT -- POSIX-compliant commands and libraries for Windows NT. (Posix is an IEEE standard that comprises many of the commands and utilities that Unix® systems contain.) All of these programs can also be found at NITA (NT Internet Archive) at ftp.pht.com.*Shareware programs require separate payment to the author if found userful.••••••••••••Paper CD Vol 1The Paper CD Series is a collection of fine paper backgrounds on CD-ROM. Volume One is Fiber Paper.All of the backgrounds are from high quality drum-scanned images. These images can be used for background graphics in desktop publishing and for multimedia presentations. There are 20 papers on each disc. There are currently five volumes in the series: Fiber Paper, Speckled Paper, Cloud Paper, Stardust Paper, and Wheat Paper. The approximately 600 MB of graphical data on each disc is royalty-free. A friendly user-interface for viewing and copying the images is included as well as both Windows and Macintosh versions of Adobe Photoshop™ Tryout. The images are in TIFF format, at 300 dpi, with dimensions of 2610 x 3570 and 900 x 900, which will allow for high-quality printing at 150 lines per inch. Image sizes of 640 x 480 at 72 dpi in PICT and BMP formats are included for multimedia presentations. Each disc in the series has a retail price of $39.95 per disc.••••••••••••Paper CD Vol 2The Paper CD Series is a collection of fine paper backgrounds on CD-ROM. Volume Two is Speckled Paper.All of the backgrounds are from high quality drum-scanned images. These images can be used for background graphics in desktop publishing and for multimedia presentations. There are 20 papers on each disc. There are currently five volumes in the series: Fiber Paper, Speckled Paper, Cloud Paper, Stardust Paper, and Wheat Paper. The approximately 600 MB of graphical data on each disc is royalty-free. A friendly user-interface for viewing and copying the images is included as well as both Windows and Macintosh versions of Adobe Photoshop™ Tryout. The images are in TIFF format, at 300 dpi, with dimensions of 2610 x 3570 and 900 x 900, which will allow for high-quality printing at 150 lines per inch. Image sizes of 640 x 480 at 72 dpi in PICT and BMP formats are included for multimedia presentations. Each disc in the series has a retail price of $39.95 per disc.••••••••••••Paper CD Vol 3The Paper CD Series is a collection of fine paper backgrounds on CD-ROM. Volume Three is Cloud Paper.All of the backgrounds are from high quality drum-scanned images. These images can be used for background graphics in desktop publishing and for multimedia presentations. There are 20 papers on each disc. There are currently five volumes in the series: Fiber Paper, Speckled Paper, Cloud Paper, Stardust Paper, and Wheat Paper. The approximately 600 MB of graphical data on each disc is royalty-free. A friendly user-interface for viewing and copying the images is included as well as both Windows and Macintosh versions of Adobe Photoshop™ Tryout. The images are in TIFF format, at 300 dpi, with dimensions of 2610 x 3570 and 900 x 900, which will allow for high-quality printing at 150 lines per inch. Image sizes of 640 x 480 at 72 dpi in PICT and BMP formats are included for multimedia presentations. Each disc in the series has a retail price of $39.95 per disc.••••••••••••Paper CD Vol 4The Paper CD Series is a collection of fine paper backgrounds on CD-ROM. Volume Four is Stardust Paper.All of the backgrounds are from high quality drum-scanned images. These images can be used for background graphics in desktop publishing and for multimedia presentations. There are 20 papers on each disc. There are currently five volumes in the series: Fiber Paper, Speckled Paper, Cloud Paper, Stardust Paper, and Wheat Paper. The approximately 600 MB of graphical data on each disc is royalty-free. A friendly user-interface for viewing and copying the images is included as well as both Windows and Macintosh versions of Adobe Photoshop™ Tryout. The images are in TIFF format, at 300 dpi, with dimensions of 2610 x 3570 and 900 x 900, which will allow for high-quality printing at 150 lines per inch. Image sizes of 640 x 480 at 72 dpi in PICT and BMP formats are included for multimedia presentations. Each disc in the series has a retail price of $39.95 per disc.••••••••••••Paper CD Vol 5The Paper CD Series is a collection of fine paper backgrounds on CD-ROM. Volume Five is Wheat Paper.All of the backgrounds are from high quality drum-scanned images. These images can be used for background graphics in desktop publishing and for multimedia presentations. There are 20 papers on each disc. There are currently five volumes in the series: Fiber Paper, Speckled Paper, Cloud Paper, Stardust Paper, and Wheat Paper. The approximately 600 MB of graphical data on each disc is royalty-free. A friendly user-interface for viewing and copying the images is included as well as both Windows and Macintosh versions of Adobe Photoshop™ Tryout. The images are in TIFF format, at 300 dpi, with dimensions of 2610 x 3570 and 900 x 900, which will allow for high-quality printing at 150 lines per inch. Image sizes of 640 x 480 at 72 dpi in PICT and BMP formats are included for multimedia presentations. Each disc in the series has a retail price of $39.95 per disc.••••••••••••PHT IllustrationsPHT Illustrations CD-ROM is a collection of 100 royalty-free original illustrations. These images can be used for high quality, creative background graphics in desktop publishing and multimedia presentations. Categories include Animals, Art, Food, Landscapes and Space. The images are in 300dpi and 72dpi resolutions and are in TIFF, BMP and PICT formats. The disc is in hybrid format with viewers for both Windows™ and Macintosh®, and has Windows and Macintosh versions of Adobe Photoshop Tryout. This CD-ROM is easy to use and suitable for professional graphic artists and home computer dabblers alike. The PHT Illustrations may be used in print and digital publications, video presentations or multimedia works on a royalty free basis with the exception that the images cannot be used as a primary commercial object in any derivative products.••••••••••••PIAThe PIA CD-ROM contains over 100 programs for the Power Macintosh.PHT's PIA CD-ROM is the first-ever public domain and shareware* disc devoted solely to the Power Mac. All of the programs on the CD have been taken from the Internet and are current as of March 1995. Included on the CD-ROM are demos of some of the best commercial programs available for the Power Mac. These programs can also be found now at PIA (PowerMac Internet Archive) at ftp.pht.com.*Shareware programs require separate payment to the author if found userful.••••••••••••SpaceViewSpace View is a collection of astronomical images from the Internet. A large portion of the data on the CD-ROM is from the NASA Internet archive. Each image includes a detailed description of the image, makes note of areas of special interest and explains how the data/image was obtained. The disk also includes a categorical index, allowing the user to select from general topics like: Earth, Moon, Venus, Saturn, Eclipses. The Space View interface is available in English, Japanese, Chinese, French, German and Spanish.••••••••••••UMichThis CD-ROM contains thousands of shareware* and freeware programs from the University of Michigan’s Macintosh archive. UMich has applications, games, utilities, graphics and science programs , as well as source code samples and development tools. The disk also includes a top-level directory listing which categorizes its files and programs by type.*Shareware programs require separate payment to the author if found userful.••••••••••••Visual ProgrammingThe disk contains an extensive collection of shareware* and freeware source code and programming utilities for creating Windows programs with Visual Basic and Visual C++. The disk provides Windows applications programmers and developers with hundreds of useful programs, taken primarily from the CICA archive at Indiana State University.This disc is scheduled to ship June 1995.*Shareware programs require separate payment to the author if found userful.••••••••••••WIAThis disk contains thousands of freeware and shareware* applications, games, file utilities and general utilities for Windows. WIA includes database, spreadsheet and word processing utilities and examples, as well as source sode and programming utilities.This CD-ROM is scheduled to ship early June of 1995.*Shareware programs require separate payment to the author if found userful.••••••••••••X11X11R6 CD-ROM contains the free windowing system for Unix® developed at MIT.This CD-ROM is the source for the server and all contributing programs from ftp.x.org and sunsite,unc.com. In addition to the entire X11R6 Window System source code, nearly all of the sunsite.unc.edu/pub/X11 tree containing 450 MB of source code for X11 applications is included. Documentation for the X11R6 package is found under the R6 distribution tree and most of the applications in this disk contain read me files as well. Directory listings of all the files in this collection are contained in 'Is-IR' and 'find.files,' allowing users to quickly find specific files.</text>
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<script>on colorMeAddColor colorCard,irisOpen,90-- go next card-- setLang 5go cd 3 -- Skip the card 2 (which is English SpaceViewMenu)end colorMe</script>