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                  SPACE SHUTTLE ENDEAVOUR

                          STS-67

                     MISSION PRESS KIT

                         MARCH 1995



PUBLIC AFFAIRS CONTACTS

For Information on the Space Shuttle

Ed Campion                 Policy/Management      202/358-1778
Headquarters, Wash., DC

Rob Navias                 Mission Operations     713/483-5111
Johnson Space Center,      Astronauts
Houston, TX

Bruce Buckingham           Launch Processing      407/867-2468
Kennedy Space Center, FL   KSC Landing Information

June Malone           External Tank/SRBs/SSMEs    205/544-0034
Marshall Space Flight Center
Huntsville, AL

Cam Martin            DFRC Landing Information    805/258-3448
Dryden Flight Research Center
Edwards, CA

     For Information on STS-67 Experiments & Activities

Don Savage                     ASTRO-2           202/358-1547
Headquarters, Wash., DC

Mike Braukus                   PCG               202/358-1979
Headquarters, Wash., DC

Tammy Jones                    GAS               301/286-5566
Goddard Space Flight Center
Greenbelt, MD

Jim Cast                       MACE, CMIX        202/358-1779
Headquarters, Wash., DC

Terri Hudkins                  SAREX             202/358-1977
Headquarters, Wash., DC


CONTENTS

GENERAL BACKGROUND
General Release                                      1
Media Services Information                           4
Quick-Look Facts                                     6
Shuttle Abort Modes                                  8
Summary Timeline                                     9
Payload and Vehicle Weights                         11
Orbital Events Summary                              12
Crew Responsibilities                               13

CARGO BAY PAYLOADS & ACTIVITIES
ASTRO-2                                             15
Get Away Special (GAS) Experiments                  33

IN-CABIN PAYLOADS
Commercial MDA ITA Experiments (CMIX)               35
Protein Crystal Growth (PCG) Experiments            39
Middeck Active Control Experiment (MACE)            43
Shuttle Amateur Radio Experiment (SAREX)            44

STS-67 CREW BIOGRAPHIES
Stephen S. Oswald , Commander (CDR)                 47
William G. Gregory, Pilot (PLT)                     47
John M. Grunsfeld, Mission Specialist-1 (MS-1)      48
Wendy B. Lawrence, Mission Specialist-2 (MS-2)0     48
Tamara E. Jernigan, Payload Commander/Mission
                    Specialist-3 (MS-3)             48
Samuel T. Durrance, Payload Specialist-1 (PS-1)     49
Ronald Parise, Payload Specialist-2 (PS-2)          49




RELEASE:  95-18

ASTRO TELESCOPES MAKE SECOND FLIGHT ON STS-67 MISSION


     This March, Space Shuttle Endeavor will conduct NASA's
longest Shuttle flight to date carrying unique ultraviolet
telescopes that will give astronomers a view of the universe
impossible to obtain from the ground.

     The mission, designated STS-67, also will see Endeavour's
crew perform a wide range of microgravity processing
experiments, continue efforts in understanding the structure
of proteins and study active control of flexible structures in
space.

     Launch of Endeavour is scheduled for March 2, 1995 at
approximately 1:37 a.m. EST from NASA's Kennedy Space Center's
Launch Complex 39-A.  Endeavour's flight will be 15 days, 13
hours, 32 minutes.  A 1:37 a.m. launch on March 2, would
result in a landing at Kennedy Space Center's Shuttle Landing
Facility on March 17, at 3:09 p.m. EST.

     The STS-67 crew will be commanded by Stephen S. Oswald
who will be making his third Shuttle flight.  William G.
Gregory, who will be making his first space flight, will serve
as pilot.  The three mission specialists aboard Endeavour will
include John M. Grunsfeld, Mission Specialist-1 (MS-1) who
will be making his first flight, Wendy B. Lawrence, Mission
Specialist-2 (MS-2) who will be making her first flight and
Tamara E. Jernigan, Payload Commander and Mission Specialist 3
(MS-3) who will be making her third flight.  Rounding out the
crew will be two payload specialists who flew on ASTRO-1
during the STS-35 mission in December 1990.  Samuel Durrance
will serve as Payload Specialist-1 (PS-1) and Ronald Parise
will serve as Payload Specialist-2.  Both Parise and Durrance
will be making their second space flight.

     The Astro Observatory, making its second flight aboard a
Space Shuttle, is a package of three instruments mounted on
the Spacelab Instrument Pointing System (IPS).  The Hopkins
Ultraviolet Telescope will conduct spectroscopy in the far
ultraviolet portion of the electromagnetic spectrum, allowing
scientists to learn what elements are present in targeted
celestial objects, as well as identify physical processes
taking place.

     The second instrument, the Ultraviolet Imaging Telescope,
will take wide-field photographs of objects in ultraviolet
light, recording the images on film for processing back on
Earth.  The third instrument, the Wisconsin Ultraviolet Photo-
Polarimeter Experiment, will measure the intensity of
ultraviolet light and its degree of polarization.  The
instrument will give astronomers clues to the geometry of a
star or the composition and structure of the interstellar
medium it illuminates.

     Simultaneous observations by these three telescopes will
complement one another as they provide different perspectives
on the same celestial objects.  These observations also will
complement those of ultraviolet instruments on other NASA
spacecraft, such as the Hubble Space Telescope, the
International Ultraviolet Explorer, and the Extreme
Ultraviolet Explorer -- all currently in operation.  By
combining research findings from these various instruments,
scientists hope to piece together the evolution and history of
the universe and learn more about the composition and origin
of stars and galaxies.

     The flight also will see the continuation of NASA's Get
Away Special (GAS) experiments program.  The project gives
individuals an opportunity to perform experiments in space on
a Shuttle mission.  Two GAS cans will be carried in the cargo
bay in support of a payload from the Australian Space Office.
The payload, coincidentally named Endeavour, is an Australian
space telescope that will take images in the ultraviolet
spectrum of violent events in nearby exploding galaxies.

     The third in a series of six Commercial MDA ITA
Experiments (CMIX) payloads will also fly aboard Endeavour.
CMIX-03 includes biomedical, pharmaceutical, biotechnology,
cell biology, crystal growth and fluids science
investigations.  These experiments will explore ways in which
microgravity can benefit drug development and delivery for
treatment of cancer, infectious diseases and metabolic
deficiencies.  These experiments also will include protein and
inorganic crystal growth, experiments on secretion of
medically important products from plant cells, calcium
metabolism, invertebrate development and immune cell
functions.

     Endeavour will carry two systems in Shuttle middeck
lockers to continue space-based research into the structure of
proteins and other macromolecules.  The study of proteins,
complex biochemicals that serve a variety of purposes in
living organisms, is an important aspect of this mission.
Determining the molecular structure of proteins will lead to a
greater understanding of how the organisms function.
Knowledge of the structures also can help the pharmaceutical
industry develop disease-fighting drugs.  The two systems are
the Vapor Diffusion Apparatus in which trays will be housed
within a temperature-controlled Thermal Enclosure System and
the Protein Crystallization Apparatus for Microgravity that
will be housed in a Single-locker Thermal Enclosure System.

     The Middeck Active Control Experiment is an experiment
designed to study the active control of flexible structures in
space.  In this experiment, a small, multibody platform will
be assembled and free-floated inside the Space Shuttle.  Tests
will be conducted on the platform to measure how disturbances
caused by a payload impact the performance of another nearby
payload which is attached to the same supporting structure.

     The STS-67 crew will take on the role of teachers as they
educate students in the United States and other countries
about their mission objectives.  Using the Shuttle Amateur
Radio Experiment-II, Shuttle Commander Stephen S. Oswald (call
sign KB5YSR), pilot William G. Gregory, (license pending),
mission specialists Tamara E. Jernigan (license pending) and
Wendy B. Lawrence (KC5KII) and Payload Specialists Ron Parise
(WA4SIR) and Sam Durrance (N3TQA) will talk with students in
26 schools in the U.S., South Africa, India and Australia
using "ham radio", about what it is like to live and work in
space.

     The STS-67 mission will be the 8th flight of Space
Shuttle Endeavour and the 68th flight of the Space Shuttle
system.

                - end general release-


MEDIA SERVICES INFORMATION

NASA Television Transmission

     NASA Television is available through Spacenet-2 satellite
system, transponder 5, channel 9, at 69 degrees West
longitude, frequency 3880.0 MHz, audio 6.8 Megahertz.

     The schedule for television transmissions from the
Orbiter and for mission briefings will be available during the
mission at Kennedy Space Center, FL; Marshall Space Flight
Center, Huntsville, AL; Dryden Flight Research Center,
Edwards, CA; Johnson Space Center, Houston; NASA Headquarters,
Washington, DC; and the NASA newscenter operation at Mission
Control-Moscow.  The television schedule will be updated to
reflect changes dictated by mission operations.

     Television schedules also may be obtained by calling
COMSTOR 713/483-5817.  COMSTOR is a computer data base service
requiring the use of a telephone modem.  A voice update of the
television schedule is updated daily at noon Eastern time.

Status Reports

     Status reports on countdown and mission progress, on-
orbit activities and landing operations will be produced by
the appropriate NASA newscenter.

Briefings

     A mission press briefing schedule will be issued prior to
launch.  During the mission, status briefings by a Flight
Director or Mission Operations representative and when
appropriate, representatives from the payload team, will occur
at least once per day.  The updated NASA television schedule
will indicate when mission briefings are planned.

Access by Internet

     NASA press releases can be obtained automatically by
sending an Internet electronic mail message to
[e-mail].  In the body of the message (not the subject
line) users should type the words "subscribe press-release"
(no quotes).  The system will reply with a confirmation via E-
mail of each subscription.  A second automatic message will
include additional information on the service.

     Informational materials also will be available from a
data repository known as an anonymous FTP (File Transfer
Protocol) server at ftp.pao.hq.nasa.gov under the directory
/pub/pao.  Users should log on with the user name "anonymous"
(no quotes), then enter their E-mail address as the password.
Within the /pub/pao directory there will be a "readme.txt"
file explaining the directory structure.

  The NASA public affairs homepage also is available via the
Internet.  The page contains images, sound and text (press
releases, press kits, fact sheets) to explain NASA activities.
It also has links to many other NASA pages.  The URL is:
http://www.nasa.gov/hqpao/hqpao_home.html

Access by fax

     An additional service known as fax-on-demand will enable
users to access NASA informational materials from their fax
machines.  Users calling [phone] may follow a series of
prompts and will automatically be faxed the most recent
Headquarters news releases they request.

Access by Compuserve

     Users with Compuserve accounts can access NASA press
releases by typing "GO NASA" (no quotes) and making a
selection from the categories offered.

STS-67 QUICK LOOK

Launch Date/Site:     March 2, 1995/KSC Pad 39A
Launch Time:          1:37 a.m. EST
Launch Window:        2 hours, 30 minutes
Orbiter:              Endeavour (OV-105) - 8th flight
Orbit/Inclination:    190 nautical miles/28.45 degrees
Mission Duration:     15 days, 13 hours, 32 minutes
Landing Time/Date     March 17, 1995
Landing Time:         3:09 p.m. EST
Primary Landing Site:    Kennedy Space Center, FL
Abort Landing Sites:     Return to Launch Site - KSC
            Transoceanic Abort Landing - Ben Guerir, Morocco
                                         Moron, Spain
            Abort Once Around - Edwards Air Force Base, CA

Crew:  Steve Oswald, Commander (CDR), Red Team
       Bill Gregory, Pilot (PLT), Red Team
       John Grunsfeld, Mission Specialist 1 (MS 1), Red Team
       Wendy Lawrence, Mission Specialist 2 (MS 2), Blue Team:
       Tammy Jernigan, Payload Commander, Mission
       Specialist -3 (MS 3), Blue Team
       Sam Durrance, Payload Specialist 1 (PS 1), Blue Team
       Ron Parise, Payload Specialist 2 (PS 2), Red Team

Extravehicular Crewmembers:  Jernigan (EV 1), Grunsfeld (EV 2)

Cargo Bay Payloads:   ASTRO-2
                      Getaway Special Canisters

Middeck Payloads:     MACE
                      PCG-STES
                      CMIX
                      PCG-TES

In-Cabin Payloads:    SAREX-II


Developmental Test Objectives/Detailed Supplementary
Objectives:

DTO 251:   Entry Aerodynamic Control Surfaces Test
DTO 254:   Subsonic Aerodynamics Verification
DTO 301D:  Ascent Structural Capability Evaluation
DTO 307D:  Entry Structural Capability
DTO 312:   External Tank Thermal Protection System Performance
DTO 319D:  Orbiter/Payload Acceleration and Acoustics Data
DTO 414:   APU Shutdown Test
DTO 667:   Portable In-Flight Landing Operations Trainer
                    (PILOT)
DTO 674:   Thermoelectric Liquid Cooling System Evaluation
DTO 700-8: Global Positioning System Developmental Flight Test
DTO 700-9: Orbiter Evaluation of TDRS Acquisition in Bypass
             Mode
DTO 805:   Crosswind Landing Performance
DSO 326:   Window Impact Observations
DSO 328:   In-Flight Urine Collection Absorber Evaluation
DSO 484:   Assessment of Circadian Shifting in Astronauts by
             Bright Light
DSO 487:   Immunological Assessment of Crewmembers
DSO 488:   Measurement of Formaldehyde Using Passive Dosimetry
DSO 603:   Orthostatic Function During Entry, Landing and
             Egress
DSO 604:   Visual-Vestibular Integration as a Function of
             Adaptation
DSO 605:   Postural Equilibrium Control During Landing/Egress
DSO 608:   Effects of Space Flight on Aerobic and Anaerobic
             Metabolism
DSO 614:   The Effect of Prolonged Space Flight on Head
             and Gaze Stability during Locomotion
DSO 624:   Pre and Postflight Measurement of Cardiorespiratory
             Responses to Submaximal Exercise
DSO 626:   Cardiovascular and Cerebrovascular Responses to
             Standing Before and After Space Flight
DSO 901:   Documentary Television
DSO 902:   Documentary Motion Picture Photography
DSO 903:   Documentary Still Photography


SPACE SHUTTLE ABORT MODES

     Space Shuttle launch abort philosophy aims toward safe
and intact recovery of the flight crew, Orbiter and its
payload. Abort modes for STS-67 include:

     *  Abort-To-Orbit (ATO) -- Partial loss of main engine
thrust late enough to permit reaching a minimal 105-nautical
mile orbit with the orbital maneuvering system engines.

     *  Abort-Once-Around (AOA) -- Earlier main engine
shutdown with the capability to allow one orbit of the Earth
before landing at Edwards Air Force Base, CA.

     *  TransAtlantic Abort Landing (TAL) -- The loss of one
or more main engines midway through powered flight would force
a landing at either Moron, Spain, or Ben Guerir, Morocco.

     *  Return-To-Launch-Site (RTLS) -- Early shutdown of one
or more engines, before the Shuttle has enough energy to reach
Moron or Ben Guerir, would result in a pitch around and thrust
back toward KSC until the Orbiter is within gliding distance
of the Shuttle Landing Facility.


MISSION SUMMARY TIMELINE

Flight Day One:
Launch/Ascent
OMS-2 Burn
Astro/Spacelab Activation
Instrument Pointing System Activation
Astro Observations

Flight Day Two:
Astro Observations

Flight Day Three:
Astro Observations
MACE Operations

Flight Day Four:
Astro Observations
MACE Operations

Flight Day Five:
Astro Observations

Flight Day Six:
Astro Observations
Off-Duty Time for MS 3 and PS 1

Flight Day Seven:
Astro Observations
MACE Operations
Off-Duty Time for MS 1 and PS 2

Flight Day Eight:
Astro Observations

Flight Day Nine:
Astro Observations
MACE Operations

Flight Day Ten:
Astro Observations
MACE Operations

Flight Day Eleven:
Astro Observations
Off-Duty Time for MS 3 and PS 1

Flight Day Twelve:
Astro Observations
MACE Operations
Off-Duty Time for MS 1 and PS 2

Flight Day Thirteen:
Astro Observations
Crew News Conference

Flight Day Fourteen:
Astro Observations
Flight Control System Checkout
Instrument Pointing System Stow Check and Redeployment

Flight Day Fifteen:
Astro/Spacelab Deactivation
Instrument Pointing System Stow
Cabin Stow

Flight Day Sixteen:
Deorbit Prep
Deorbit Burn
Entry
KSC Landing

PAYLOAD AND VEHICLE WEIGHTS

Vehicle/ Payload                                   Pounds

Orbiter (Endeavour) empty and 3 SSMEs             173,910

ASTRO-2 (Instruments and Support Equipment)        17,384

Getaway Special Canisters                           1,000

CMIX                                                   69

MACE (Middeck Active Control Experiment)              258

Protein Crystal Growth Experiment                     205

Shuttle Amateur Radio Experiment                       28

Detailed Test/Supplementary Objectives                171

Shuttle System at SRB Ignition                  4,520,531

Orbiter Weight at Landing                         217,683


               STS-67 ORBITAL EVENTS SUMMARY
             (Based on a March 2, 1995 Launch)

EVENT                    MET                TIME OF DAY (EST)

Launch                 0/00:00              1:37 a.m., Mar. 2

OMS-2                  0/00:51              2:28 a.m., Mar. 2

IPS Activation         0/03:15              4:52 a.m., Mar. 2

Crew News Conference  12/11:10             12:47 p.m., Mar. 14

FCS Checkout          13/11:45              1:22 p.m., Mar. 15

Deorbit Burn          15/12:25              2:02 p.m., Mar. 17

KSC Landing           15/13:32              3:09 p.m., Mar. 17



CREW RESPONSIBILITIES

Payloads and Activities      Prime               Backup
╩
ASTRO                      Jernigan              Grunsfeld,
                                              Durrance, Parise
Getaway Specials           Grunsfeld             Lawrence
MACE                       Oswald                Gregory
PCG                        Lawrence              Gregory
CMIX                       Gregory               Lawrence
SAREX                      Parise                Oswald



DTOs/ DSOs

DTO 251:   Entry Aerodynamics Test   Oswald        Gregory
DTO 312:   Tank TPS Performance      Grunsfeld     Lawrence
DTO 667:   PILOT                     Oswald        Gregory
DSO 484:   Circadian Shifting     Jernigan, Lawrence, Durrance
DSO 487:   Immunological Assessment      All
DSO 603C:  Entry Monitoring       Jernigan, Grunsfeld,
                                  Durrance, Parise
DSO 604:   Head/Eye Movement      Grunsfeld, Parise, Oswald
DSO 608:   Aerobic/Anaerobic      Oswald, Gregory, Lawrence
DSO 605:   Postural Equilibrium       Oswald, Gregory
DSO 614:   Head and Gaze Stability    Gregory, Grunsfeld
DSO 624:   Submaximal Exercise        Durrance, Parise
DSO 626:   Extended Stand Test        Jernigan, Grunsfeld,
                                      Durrance, Parise

Other Activities:
Photography/TV          Grunsfeld          Lawrence, Gregory
In-Flight Maintenance   Gregory          Lawrence, Oswald
Earth Observations      Grunsfeld            Lawrence
Medical                 Oswald               Jernigan


Astro-2

     A cluster of unique telescopes will turn the Space
Shuttle Endeavour into an Earth-orbiting ultraviolet
observatory.  This set of mechanized "eyes" will give
astronomers a view of the heavens impossible to obtain from
the ground.

     The mission, which will study some of the most energetic
events in the cosmos, builds on the experience and scientific
data obtained on the first Astro flight in 1990.  This second
mission will fill gaps in knowledge about ultraviolet
astronomy, expand and refine existing data, and help
astronomers better understand our dynamic universe.

     NASA's Marshall Space Flight Center in Huntsville, AL,
supervised development of the Astro observatory and manages
Astro missions for the Astrophysics Division of NASA's Office
of Space Science, Washington, DC.

Why Ultraviolet Astronomy?

     Since the earliest days of astronomy, people have used
the light from stars to test their understanding of the
universe.  However, the visible light that can be studied from
Earth is only a small portion of the radiation produced by
celestial objects.  Other forms of radiation -- like lower
energy infrared light and higher energy ultraviolet light and
X-rays -- are absorbed by the atmosphere and never reach the
ground.

     Seeing celestial objects in visible light alone is like
looking at a painting in only one color.  To fully appreciate
the meaning of the painting, viewers must see it in all of its
colors.

     Getting above the atmosphere with space instruments like
the Astro ultraviolet telescopes lets astronomers add some of
these "colors"  to their view of stars and galaxies.

     The universe of ultraviolet astronomy is strikingly
different from our familiar night sky. Most stars fade from
view, too cool to emit much ultraviolet radiation.  But very
young massive stars, some very old stars, glowing nebulae,
active galaxies, quasars and white dwarfs stand out when
observed with instruments sensitive to ultraviolet radiation.

      Before the advent of orbiting ultraviolet telescopes,
scientists had to be satisfied with rocket-borne ultraviolet
telescopes.  In fact, all three Astro telescopes are based on
prototypes flown separately on sounding rockets.  A typical
rocket flight might gather 300 seconds of data on a single
object.  During Astro-2, scientists expect their three
telescopes to gather hundreds of hours of data on a multitude
of celestial objects.


THE ASTRO TELESCOPES

     The Astro Observatory is a package of three instruments,
mounted on the Spacelab Instrument Pointing System.

     The Hopkins Ultraviolet Telescope (HUT), developed at The
Johns Hopkins University, Baltimore, MD, conducts spectroscopy
in the far ultraviolet portion of the electromagnetic
spectrum.  Spectroscopy allows scientists to learn what
elements are present in an object, as well as identify
physical processes taking place there.

     The Ultraviolet Imaging Telescope (UIT), developed by
NASA's Goddard Space Flight Center, Greenbelt, MD, takes wide-
field photographs of objects in ultraviolet light, recording
the images on film for processing back on Earth.

     The Wisconsin Ultraviolet Photo-Polarimeter Experiment
(WUPPE), developed at the University of Wisconsin at Madison,
measures the intensity of ultraviolet light and its degree of
polarization.  When light waves are polarized, or vibrate in a
preferred direction rather than randomly, they give
astronomers clues to the geometry of a star or the composition
and structure of the interstellar medium it illuminates.

     Simultaneous observations by the three telescopes
complement one another, as they provide different perspectives
on the same celestial objects.

     Astro-2 observations also complement those of ultraviolet
instruments on other NASA spacecraft, such as the Hubble Space
Telescope, the International Ultraviolet Explorer, and the
Extreme Ultraviolet Explorer -- all currently in operation.
By combining research findings from various instruments,
scientists hope to piece together the evolution and history of
the universe and learn more about the composition and origin
of stars and galaxies.

Astro-1

     The first flight of the Astro observatory took place in
December 1990 and lasted nine days.  In addition to the
ultraviolet telescopes, the observatory included an X-ray
instrument called the Broad-Band X-ray Telescope mounted on a
separate pointing system.

     During this mission the Astro team learned a number of
valuable lessons about operating a Shuttle-based astronomical
observatory in orbit -- lessons that will be put to good use
during the Astro-2 mission.

     The Astro-1 instruments captured the first views of many
celestial objects in extremely short ultraviolet wavelengths,
took the first detailed ultraviolet photographs of many
astronomical objects, and made the first extensive studies of
ultraviolet polarization.

     The end of 1994 saw more than 110 scientific articles
published on Astro-1 results by these four instrument teams.

     One of the first-covered Hopkins Ultraviolet Telescope
observations was designed to test a theory which had been
proposed about the nature of so-called "dark matter," -- a
substantial portion of the universe's mass that astronomers
have been unable to account for.   The observation effectively
disproved the theory, leaving the "missing mass" in the
universe as mysterious as ever.

     Successive papers reveal an impressively wide range of
scientific insights obtained by Astro-1.  Observations covered
everything from solar system objects, nearby interstellar
medium, distant quasars, star clusters, galaxies, individual
nebulae and stars.  Each observation helps to fill in gaps in
our understanding of the physics of these objects.

Astro-1 Results and Astro-2 Goals
     Many Astro-2 observations will build on discoveries from
Astro-1, while others will seek to answer additional questions
about the ultraviolet universe.

     * Stellar evolution.  Stars like Earth's Sun are the most
common type, emitting most of their radiation in visible
light.  But young stars being formed, and some old stars in
later stages of their evolution, shine brighter in ultraviolet
wavelengths.

     On Astro-1, UIT images identified rings of massive star
formation in several galaxies, and roughly half of the
instrument╒s science program on Astro-2 is devoted to studies
of star-forming galaxies.  A unique UIT contribution is the
identification of thousands of individual hot stars in other
galaxies for later study by NASA's Hubble Space Telescope.

     UIT also photographed globular clusters, where there are
often so many stars grouped together that it is impossible to
distinguish individual stars.  The ultraviolet images picked
out hot stars in late stages of evolution, where hydrogen has
been depleted from the cores and energy is provided by burning
helium.  By comparing photographs taken in different
wavelengths, scientists were able to measure the temperature
as well as brightness of the individual stars.

     Observing more globular clusters is a high priority for
the imaging telescope on Astro-2.  Astronomers will compare
the observations to theoretical predications, to help fill in
gaps in their knowledge about these late evolutionary stages.

     All three Astro-2 telescopes will study white dwarf
stars.  These are old stars in a transition phase -- former
giants which have shed their cool outer layers, leaving
dormant cores containing a Sun╒s worth of mass within a sphere
the size of Earth.  The hottest white dwarf stars, perhaps as
hot as 200,000 degrees Fahrenheit (110,000 degrees Celsius),
are very unstable and pulsate every five to ten minutes.

     * Spinning stars.  One of the surprises from Astro-1 were
observations of stars that are spinning very fast, called Be
stars.  A Be star is thought to be surrounded by a disk of gas
lost from the star.  WUPPE found that the amount of polarized
light coming from these stars was less than is seen in visible
light and less than expected in the ultraviolet, indicating
that some of the ultraviolet polarized light was being removed
by the gas in the disk around the star.  The wavelengths in
the ultraviolet where polarized light was missing told
astronomers that there are apparently atoms of gaseous iron in
the disks close to Be stars.  The WUPPE team will try to learn
more about the gaseous disks by viewing more Be stars during
Astro-2.

     * Cataclysmic variables.  Astro-1 ultraviolet telescopes
observed cataclysmic variables -- dual star systems which
occasionally increase dramatically in brightness as a dense
old star called a white dwarf pulls material from its
companion normal star.  One particularly interesting
observation was of a variable near the peak of its brightness,
which Astro-1 was able to view after a support network of
amateur astronomers using ground-based telescopes reported
seeing an outburst in progress.  Results from the Astro-1
observations did not match theoretical predictions, causing a
re-evaluation of current theories about this type of star
system.

     Scientists will use follow-up observations during Astro-2
to learn more about what triggers the sudden outbursts of
energy in cataclysmic variables, which can increase their
brightness 100 times or more.

     * Supernova remnants.  Supernova remnants are the ghosts
of dead stars, expanding gaseous nebulae created by stellar
explosions.  Observing the young remnants of a supernova╒s
explosion provides the only direct test of a process called
nucleosynthesis, whereby lighter elements are manufactured
into heavier elements in the centers of stars.  Observations
of old supernova remnants actually probe conditions in
interstellar space as the shock wave encounters clouds of
interstellar material.

     During Astro-1, all three ultraviolet telescopes observed
the Cygnus Loop, the remnant of an explosion some 40,000 years
ago.  Observations detected a much higher temperature and
therefore much greater velocity of its shock wave than had
been predicted.  The telescopes also studied the Crab Nebula,
a relatively young supernova remnant.

     Astro-2 observations will include the Cygnus Loop and
several other supernovas as well.

     * Galaxy morphology.  Galaxies come in a variety of
shapes and sizes, such as gigantic spirals like the Earth's
Milky Way, egg-shaped ellipticals and irregular shapes with no
preferred form.  Studying the shapes of galaxies in the
ultraviolet is a key to the study of galaxy evolution in the
early universe.

       Before Astro-1, there were only a handful of
ultraviolet pictures of nearby galaxies available.  UIT images
from that mission revealed that the shapes of galaxies seen in
ultraviolet wavelengths are strikingly different for their
familiar forms in visible light.  One UIT goal for Astro-2 is
the construction of an ultraviolet atlas of spiral galaxies.

     * Active galaxies.  Observations of active galaxies by
the Astro telescopes may help astronomers explain why the
cores of galaxies give off large amounts of high-energy
ultraviolet, X-ray and gamma-ray radiation.

     Most astronomers believe that the radiation is produced
by a massive black hole in the center of the galaxy,
surrounded by a torus, or doughnut-shaped cloud of material.
The WUPPE instrument on Astro-1 confirmed the existence of a
thick torus, while another instrument showed unexpectedly high
temperatures near it.  These results support the idea that
ultraviolet radiation is being absorbed by a disk of matter
spiraling into a massive black hole.

     Astro-2 observations will help confirm or refute this
picture of what is happening in the centers of active
galaxies.

     * Elliptical galaxies.  Astro-1 observations by both HUT
and UIT shed light on a 20-year-old mystery about the source
of faint, ultraviolet emissions in elliptical galaxies.  Such
galaxies are thought to consist almost entirely of old red
stars, which do not emit large amounts of ultraviolet light.
However, early astronomical satellites showed that these
elliptical galaxies increase in brightness at short
ultraviolet wavelengths.

     The Astro-1 studies ruled out some proposed explanations
for the ultraviolet emissions, and they found strong evidence
for a previously unknown stage of stellar evolution that
apparently is occurring in these galaxies.  During Astro-2,
both UIT and HUT will observe more elliptical galaxies to
confirm and extend these ideas.

     *  Interstellar dust.  On Astro-1, WUPPE used half a
dozen bright stars like flashlights to illuminate the
interstellar medium, literally shedding new light on the
chemical composition and physical nature of the "dust" between
stars in our Milky Way galaxy.  Surfaces of these dust grains
are thought to provide a safe haven for the formation of
molecules, clouds of which are the "womb" for the formation of
each generation of new stars.

     Astro-1 observations revealed that some parts of the
galaxy seem to have dust grains that may look like tiny hockey
pucks, while other parts seem to have a mixture of several
sizes, shapes and kinds of dust grains.  Previously,
astronomers had thought properties of this interstellar dust
were the same wherever the dust was found.  A major Astro-2
goal for WUPPE will be  to determine whether these different
types of dust grains form because conditions in some parts of
the galaxy are different than they are in other areas.

     *  Primordial intergalactic gas.  The primary Astro-2
goal for the Hopkins telescope is to detect the existence of
primordial intergalactic gas, an investigation it did not get
to perform on Astro-1.

     This helium gas in the vast space between galaxies is
thought to be left over from the "Big Bang," the primordial
fireball which marked the beginning of the universe.
Existence of the gas is a logical consequence of the "Big
Bang" theory.

     HUT will look for evidence of intergalactic helium by
observing the light of an extremely distant object called a
quasar, located behind the gas, much as a hazy mist can be
viewed when it is illuminated by the beam of a distant
flashlight.  Helium in the intervening gas would absorb light
of a specific frequency from the quasar, altering the chemical
signature the quasar could normally be expected to produce.

     A recent Hubble Space Telescope observation found
evidence of intergalactic helium in the spectrum of one
quasar.  However, HUT's spectral region permits looking at
more nearby quasars.  Positive results from Astro-2
observations would not only verify the Hubble findings, but
they could allow the density and ionization state of the gas
to be measured as well.

     *  Solar system objects.  HUT made several observations
of the planet Jupiter and its moon Io during Astro-1, studying
the dynamic nature of their relationship.  Io, the most
volcanically active body in the solar system, spews out
volcanic material into space, where it is ionized and swept up
by Jupiter's strong magnetic field.  Ultraviolet observations
permit a better understanding of the temperatures and
densities of the resulting plasma.  Scientists were able to
use HUT's more detailed spectra to reinterpret data gathered
by the Voyager spacecraft in the late 1970s.

     More studies of Jupiter will be performed during Astro-2.
The observations will help determine the importance to
Jupiter's atmosphere of extreme ultraviolet radiation from the
Sun.  The telescopes also will look for changes in the
planet's upper atmosphere resulting from recent impacts by
fragments of Comet Shoemaker-Levy 9.

ASTRO-2 INSTRUMENTS
Hopkins Ultraviolet Telescope (HUT)

Principal Investigator:     Dr. Arthur F. Davidsen
                            The Johns Hopkins University
                            Baltimore, MD

     The Hopkins Ultraviolet Telescope conducts spectroscopy
in the far ultraviolet portion of the electromagnetic
spectrum.  During Astro-2, it will study a wide variety of
objects, ranging from our own solar system and galactic
neighborhood to very distant objects near the edge of the
observable universe.

     The instrument team's highest priority for Astro-2 is the
search for intergalactic helium thought to be left over from a
primordial fireball that marked the birth of the universe
about 10 to 20 billion years ago.  HUT astronomers will
attempt to analyze light shining through this gas by observing
distant quasars.

     The portion of the spectrum observed by the Hopkins
telescope, coupled with the instrument's sensitivity, enables
it to see a slice of the ultraviolet universe which other
observatories are unable to detect.  HUT's spectral region
covers wavelengths shorter than those observed by the Hubble
Space Telescope and the International Ultraviolet Explorer and
longer than the Extreme Ultraviolet Explorer satellite.

     HUT uses a 36-inch (0.9 meter) mirror, located in the
back of the telescope tube, to focus ultraviolet light from
astronomical objects into a spectrograph set in the middle of
the telescope.  The spectrograph "spreads" ultraviolet light
into a spectrum which can be studied in detail, in much the
same way as a prism separates visible light into a rainbow of
colors.  It then measures the brightness of the light at each
wavelength.

     By analyzing how the brightness varies across the
wavelengths, scientists can determine the elements present in
the object, the relative amounts of each element, and the
temperature and density of the object.  From this, astronomers
can gain a better understanding of the physical processes
occurring in or near the object being studied.

     HUT was designed and built by Johns Hopkins University
astrophysicists and engineers at the university's Applied
Physics Laboratory in Laurel, MD.  More than two dozen
faculty, staff and students from Johns Hopkins currently are
involved in the project.

     During Astro-1, HUT made numerous observations of active
galactic nuclei, quasars, cataclysmic variables, nebulae,
supernova remnants, solar system objects and other
astronomical objects, many of which had never been studied
before in the energy range unique to HUT.

     The telescope has been improved significantly for Astro-
2, and the science team expects it to be about three times
more sensitive to the far ultraviolet spectrum than it was on
its first mission.  This will allow them to obtain higher
quality spectra and to observe fainter objects.  The primary
mirror has been coated with silicon carbide, which is much
more reflective to far ultraviolet light than the iridium
coating on the original HUT mirror.  The spectrograph grating
also has been coated with silicon carbide.

     Each time the Astro-2 telescopes point for a new
observation, astronauts and ground controllers will use
visible-light images on HUT's closed circuit TV camera to
identify the desired targets and to verify that the telescope
is pointing accurately.

     Spectra from the observations will be downlinked to the
HUT science team in Huntsville, where Johns Hopkins scientists
will record the data.  About 60 days after landing all of the
science and engineering data will be sent to Baltimore.
Scientists there will continue the detailed process of
analyzing their collected information.



Hopkins Ultraviolet Telescope (HUT)

Telescope Optics:     Silicon carbide-coated parabolic mirror
Aperture:             36 inches (90 centimenters)
Focal Ratio:                f/2
Guide TV Field of View:     10 arc-minutes
Spectral Resolution:        3.0 Angstroms
Wavelength Range:           830 to 1860 Angstroms
            (limited sensitivity in 500 to 750 Angstrom range)
Magnitude Limit:            16
Detector:     Prime Focus Rowland Circle Spectrograph with
                    microchannel plate intensifier
                    and electronic diode array detector
Weight:         1,736 pounds (789 kilograms)
Dimensions:     44 inches (1.1 meter) diameter
                12.1 feet (3.7 meters) length


Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE)

Principal Investigator:     Dr. Arthur D. Code
                            University of Wisconsin
                            Madison, WI

     The Wisconsin Ultraviolet Photo-Polarimeter Experiment
(WUPPE) measures the polarization and intensity of ultraviolet
radiation from celestial objects.

     Photometry is the measurement of the intensity
(brightness) of the light, while polarization is the
measurement of the orientation (direction) of the vibrating
light wave.

     Light is made up of electric and magnetic waves that
vibrate from side to side, up and down, and diagonally.  The
polarization of light is a measure of how much more the waves
vibrate in one direction than the others.

     Usually, light waves vibrate randomly, thus are said to
be unpolarized.  The waves become polarized when they
encounter a particular object or force which causes them to
vibrate in a preferred direction.  For example, polarization
occurs when light is emitted in the presence of a magnetic
field or when it passes through clouds of dust grains aligned
by an interstellar magnetic field.  The light from a comet's
tail is reflected sunlight that becomes polarized when it is
scattered by the ice and dust particles left in the comet's
wake.  This is similar to the way that polarized sunglasses
reduce the glare of scattered light.

     Determining the amount and direction of polarization and
how these change with wavelength can tell scientists what
caused the light waves to vibrate in a preferred direction ╤
indicators of a celestial object's geometry and other physical
conditions, or about the reflecting properties of tiny
particles in the interstellar medium along the radiation's
path.

     The primary processes responsible for polarization within
individual celestial objects are enhanced in observations of
hotter, more energetic ultraviolet radiation.  The background
clutter common in visible light studies is greatly reduced,
which is important since polarization of the interstellar
medium usually is not as strong in ultraviolet as in visible
wavelengths.

     Natural light also can become polarized when it passes
through a cloud containing dust grains aligned by an
interstellar magnetic field.  From this scientists learn about
the kinds of grains and can map out the magnetic fields in
space.

     The Wisconsin Ultraviolet Photo-Polarimeter Experiment
was built by scientists, engineers and students at the
University of Wisconsin-Madison's Space Astronomy Lab in the
1980s.

     Before the Astro-1 flight, only one single measurement of
ultraviolet polarization had ever been made.  WUPPE
observations from Astro-1 gave astronomers the first
measurements of the ultraviolet polarization of many types of
astronomical objects.  The instrument provided detailed
spectral data on the polarization of some three dozen stars,
interstellar clouds and galaxies, and ultraviolet spectra of
an additional 20 stellar objects.

     A major Astro-2 goal for WUPPE is to follow up on Astro-1
observations of the interstellar medium.  The science team
hope to learn more about the causes of polarization and the
nature of "dust" grains in the space between stars.  They also
will follow up on observations of active galaxies and rapidly
spinning stars.

     The WUPPE telescope examines ultraviolet radiation from
1,400 Angstroms (around the mid-point of the far ultraviolet
range) to 3,200 Angstroms (slightly shorter wavelengths than
blue visible light ).  This is an area that has not been
readily studied, especially for stars that are too bright for
Hubble's Faint Object Spectrograph and for nebulae too large
for Hubble's smaller spectrograph openings.

     The telescope is a classical Cassegrain-type, meaning
that light enters the tube and strikes a large, parabolic
mirror near the back.  The light then is reflected forward to
a smaller, secondary mirror near the front of the telescope,
which focuses the light back through a hole in the center of
the large mirror.  The secondary mirror can be adjusted in
precise increments to refocus the telescope, to allow it to
look at objects slightly offset from those other Astro
instruments are studying, and to perform rapid small
corrections to the telescope╒s pointing direction.

     Behind the primary mirror, the beam passes through an
ultraviolet spectrograph, a device which spreads out the
radiation by wavelengths.  A beam-splitting prism divides the
resulting spectrum into two perpendicular planes of
polarization, and the two spectra are recorded simultaneously
on two separate detectors.  Comparison of the two spectra is
then used to study the polarization of the ultraviolet light
as a function of wavelength.

Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE)
Telescope Optics:        Cassegrain system
Aperture:                20 inches (50 centimeters)
Focal Ratio:             f/10
Spectral Resolution:     6 Angstroms
Wavelength Range:        1,400 to 3,200 Angstroms
Magnitude Limit:         16
Detectors:     Spectropolarimeter with dual electronic diode
                         array detectors
Weight:         981 pounds (446 kilograms)
Dimensions:     28 inches (70 centimeters) diameter
                12.14 feet (3.7 meters) length


Ultraviolet Imaging Telescope (UIT)

Principal Investigator:     Theodore P. Stecher
                            NASA Goddard Space Flight Center
                            Greenbelt, MD

     The Ultraviolet Imaging Telescope makes deep, wide-field
photographs of objects in ultraviolet light.  This type of
imagery is a primary means for recognizing fundamentally new
phenomena or important examples of known astrophysical objects
in ultraviolet wavelengths.  Before Astro-1, very few
ultraviolet images had been made and those that were available
were taken during brief rocket flights.

     The Ultraviolet Imaging Telescope observes a field of
view two-thirds of a degree across, an area larger than the
full Moon.  This is considered "wide field" for astronomers;
each UIT photo covers an area more than 250 times the size of
the Hubble Space Telescope's Wide Field/Planetary Camera,
though at lower angular resolution and sensitivity.  For many
galaxies or star clusters, this is large enough to encompass
the entire object in a single photo frame.  In addition, the
UIT suffers much less interference from visible light, since
it is provided with "solar blind" detectors.

     Images made in the ultraviolet spectrum clearly show the
dynamic events taking place beyond our world.  The clutter of
objects which produce most of their radiation in visible light
disappears.  Hot stars leap into prominence, the spiral arms
of distant galaxies snap into clearer resolution, and the
material hidden between the stars comes into view.

     UIT's wide-field images are ideal for investigating
astronomical questions such as the shapes of nearby galaxies
as revealed in ultraviolet light, the properties of massive
hot stars, the evolution of low-mass stars, and the nature of
interstellar dust and gas.  UIT galaxy-wide images are sky
surveys that can locate bright ultraviolet stars for further
more detailed study by the Hubble Space Telescope.

     The Ultraviolet Imaging Telescope was developed at NASA's
Goddard Space Flight Center, Greenbelt, MD.  During Astro-1,
UIT obtained a large number of images, including clusters of
young, hot massive stars; globular clusters containing old
stars, some of which are unusually hot; spiral galaxies rich
with star-forming activity; and smaller "irregular" galaxies
that can experience sudden bursts of star formation.  Astro-2
will continue the important work of imaging the ultraviolet
sky.

     UIT is a powerful combination of telescope, image
intensifier and camera.  Unlike data from the other Astro
instruments, which will be electronically transmitted to the
ground, UIT images will be recorded directly on very sensitive
astronomical film.  The film will be processed and analyzed
after Endeavour returns to Earth.

     Light is reflected from a 15-inch (38-centimeter) primary
mirror, at the middle of the telescope tube, to a secondary
mirror near the front.  The secondary mirror is linked to an
image motion compensation system, which adjusts it slightly as
necessary to offset any motion or jitter in the spacecraft.
This is critical since any motions would blur the resulting
photographs.

     Reflected from the secondary mirror, the light passes
through filter wheels containing six filters each.  These
different filters allow specific wavelengths of the
ultraviolet spectrum to be selected.  By comparing two images
of the same area with different filters, the UIT team can
measure the temperature as well as the brightness of every
object in the field.

     The light then enters one of the telescope's two image
intensifier/film transport units.  The image intensifiers
amplify and convert the ultraviolet light into a visible image
that can be recorded on astronomical film.  Each unit contains
1,000 film frames.

     A 30-minute exposure can record a blue star of 25th
magnitude, about 100 million times fainter than the faintest
visible light star which could be seen by the naked eye on a
clear, dark night.  Developed after the mission, each frame of
film is digitized to form an array of 2,048 x 2,048 picture
elements, called pixels, for computer analysis.  This analysis
produces quantitative information about the objects whose
images appear on the film.



Ultraviolet Imaging Telescope (UIT)
Telescope Optics:       Ritchey-Chretien
Aperture:               15 inches (38 centimeters)
Focal Ratio:            f/9
Field of view:          40 arc-minutes
Angular Resolution:     2 arc-seconds
Wavelength Range:       1,200 to 3,200 Angstroms
Magnitude Limit:        25
Detectors:     Two image intensifiers with 70-millimeter film,
                   1,000 frames each, IIaO
astronomical film
Weight:                 1,043 pounds (474 kilograms)
Dimensions:             32 inches (81 centimeters) diameter
                        12.1 feet (3.7 meters) length


The Astro-2 Mission
     Like Astro-1, the Astro-2 observatory will be housed
inside the Shuttle's payload bay, with astronomers serving as
payload specialists operating the telescopes from the aft
flight deck of the Shuttle.  As the Shuttle Endeavour orbits
220 miles above Earth, a large contingent of scientists and
engineers will guide the mission from NASA's Spacelab Mission
Operations Control Center at Marshall Space Flight Center in
Huntsville.

     The ultraviolet telescope assembly rests on two Spacelab
pallets in Endeavour's cargo bay.  The Shuttle and Spacelab
systems provide power, pointing and communications links for
the observatory.

     The telescopes are mounted on the Instrument Pointing
System (IPS), which was part of the Spacelab equipment
developed for NASA by the European Space Agency.  It has been
used twice before, on Spacelab 2 in 1985 and on Astro-1 in
late 1990.

     The IPS furnishes a stable platform, keeps the telescopes
aligned, and provides various pointing and tracking
capabilities to the telescopes.  During Astro-1 the IPS had
some difficulties locking onto guide stars properly, although
an alternate technique allowed the astronauts to manually
point the IPS and track targets.  In general, the astronauts
were able to provide pointing stability of about 2 to 3 arc
seconds or better.  However, in "optical hold", the IPS should
be able to achieve sub-arc-second stability.  A special task
team put together by mission management at Marshall has
extensively modified and tested the IPS software and made
other improvements to ensure the IPS works properly for Astro-
2.

     Marshall's image motion compensation system, designed to
eliminate jitter caused by crew motions and thruster firings
during observations, will refine pointing and stability even
further for the photo-polarimeter and the imaging telescope.
When the system senses unwanted motion in the instruments, it
sends signals which adjust the telescopes' mirrors to reduce
jitter. This is particularly important for UIT to maintain the
quality of its imagery, since the pictures are recorded on
film and a single exposure can last as long as 30 minutes.

     After launch, the plan calls for a roughly 20-hour
checkout period, though fine-tuning the observatory could take
somewhat longer.  Observations will begin immediately after
checkout is complete and continue throughout the mission, with
only brief interruptions for activities such as waste-water
dumps and Shuttle tests.

     The night launch will allow the Shuttle Endeavour to pass
through the so-called South Atlantic Anomaly, where high-
energy radiation dips closer to the Earth than usual, mainly
on the daylit side of its orbit.  High energy particles affect
instrument operation and increase the background levels in
electronic detectors. The "natural" background, such as
scattered light and ultraviolet residual airglow emissions, is
also higher on the daylit side.  The nighttime launch
therefore preserves orbital night passes ╤ when Earth is
between the Shuttle and the Sun ╤ for observations of the
faintest, and often highest priority, astronomical targets.
Brighter targets will be observed during the day.

     The mission timeline, a detailed "blueprint" of the
flight's science activities, is divided into two-orbit (three-
hour) blocks.  One of the three telescope teams will have
priority for the entire time block and will select the
observations during that period.  Generally, the other two
telescopes will observe the same object or something nearby,
though some targets may be too bright for the imaging
telescope to view.

     The seven-member Astro-2 crew will be split into two 12-
hour shifts, so astronomical observations can continue around
the clock.

     To begin an observation, an Orbiter crew member will
maneuver the Shuttle's payload bay to point toward the
celestial object being studied.

     The two science crew members on each shift, a NASA
mission specialist and a payload specialist (an astronomer
chosen from among the experiment teams), will have the option
of using a pre-programmed, automatic sequence to maneuver the
Instrument Pointing System and lock onto guide stars, or they
may choose to acquire the target manually using a joystick-
type device.  Generally, the mission specialist will be
responsible for pointing the telescope assembly, and the
payload specialist will control the actual instrument set-ups
and observations.

     Astronomers on each instrument team will receive
telescope data at Spacelab control and adjust their
observations as needed to obtain the best possible results.
If the data reveal something unexpected, or if an unforeseen
astronomical event occurs (like the cataclysmic variable
outburst during Astro-1), the instrument teams will work with
Marshall payload controllers to develop changes in the
timeline.  This allows the investigators to explore the
unexpected and take advantage of science opportunities that
may arise during the mission.

Guest Investigators

     One new feature for Astro-2 is "community involvement."
Although each of the instruments was developed by a team of
scientists and engineers at a particular university or
government facility, "guest investigators"  also will use the
Astro telescopes for their own observations.  In 1993 NASA
solicited proposals from the general astronomical community
for participation in the observatory's second flight.  After
scientific and technical peer review, NASA selected ten
proposals for inclusion into the scientific program.  This has
produced an even broader range of observations that will be
attempted and scientific investigations that will be carried
out.

Astro-2 principal guest investigators and their experiments
are:

The Near UV Properties of Galaxies Which Have Low Optical
Surface Brightness (UIT)
Dr. Gregory D. Bothun
University of Oregon
Eugene, OR

Ultraviolet Extinction and Polarization of Interstellar Dust
in the Large Magellanic Cloud (HUT, WUPPE)
Dr. Geoffrey C. Clayton
University of Colorado
Boulder, CO

O-VI Emission and Broad-Band UV Spectra of Symbiotic Systems
(HUT, WUPPE)
Dr. Brian R. Espey
The Johns Hopkins University
Baltimore, MD

Investigations of Lyman Line Profiles in Hot DA White Dwarfs
(HUT)
Dr. David S. Finley
EUREKA Scientific, Inc.
Oakland, CA

An Ultraviolet Survey/Atlas of Spiral Galaxies (UIT)
Dr. Wendy L. Freedman
Carnegie Institution of Washington
Pasadena, CA

Astro-2 Observations of the Moon (UIT)
Dr. George R. Gladstone
Southwest Research Institute
San Antonio, TX

HUT Observations of the Lyman Continuum in Starburst Galaxies
(HUT)
Dr. Claus H. Leitherer
Space Telescope Science Institute
Baltimore, MD

Far UV Observations of Interstellar Shocks (HUT)
Dr. John C. Raymond
Smithsonian Institution Astrophysical Observatory
Cambridge, MA

The Extended Atmospheres of Wolf-Rayet Stars (HUT, WUPPE)
Dr. Regina E. Schulte-Ladbeck
University of Pittsburgh
Pittsburgh, PA

A Reconnaissance of O3 Spectra in the 900-1200 Angstrom Region
(HUT)
Dr. Nolan R. Walborn
Space Telescope Science Institute
Baltimore, MD

Astro-2 Management Team

Headquarters, Washington, DC
Program Manager                       James McGuire
Program Scientist                     Dr. Robert Stachnik

Marshall Space Flight Center
Mission Manager                       Dr. Robert Jayroe
Mission Scientist                     Dr. Charles Meegan
Deputy Mission Scientist              Dr. Eugene Urban
Assistant Mission Scientist           Dr. John Horack
Chief Engineer                        David Jacobson
Assistant Mission Manager             Stuart Clifton
Lead Payload Operations Director      Lewis Wooten



GET AWAY SPECIAL (GAS)

    The Get Away Special (GAS) project is managed by NASA's
Goddard Space Flight  Center, Greenbelt, MD.  NASA began
flying these small self-contained payloads in 1982.  The
project gives an individual an opportunity to perform
experiments in space on a Shuttle mission.  Students,
individuals and people from private industry have taken
advantage of this unique project.  Space is available for
upcoming flights, and GAS presents an educational opportunity
for students.  There is one experiment in two payloads on this
flight.  Following is a brief description of the payloads.

G-387 & G-388
Customer:  Australian Space Office, Depart. of Industry
Science & Technology Customer Manager:  Dr. John S. Boyd,
Deputy Executive Director, Australian Space Office, NASA
Technical Manager:  Charlie Knapp

    Endeavour, an Australian space telescope, is very
significant to the Australian space program as it makes its
second flight aboard Space Shuttle Endeavour on mission STS-
67.  The telescope previously flew in January 1992.

    Coincidentally, the Australian payload has the same name
as the Shuttle Endeavour.  Both were named after the sailing
ship which the Captain James Cook commanded during an
expedition to explore the Pacific Ocean.  In doing so he
discovered the eastern coast of Australia and pioneered the
way for the first settlement in Australia by Europeans.

    Endeavour is the most significant space payload built by
the Australian space industry in more than two decades.  This
is the program on which many Australian engineers learned
their space skills.  This is particularly true for Auspace,
the prime contractor for this project.  More than 200
Australian companies also contributed to this pioneering space
project.  The Australian Space Office of the Department of
Industry Science and Technology, which administers the
Australian space program, provided the funds for the Endeavour
program.

    Outside the influence of the Earth's atmosphere, Endeavour
will take images in the ultraviolet spectrum of targets which
include star-forming regions, nearby galaxies and violent
galactic events.  Such images cannot be taken from ground-
based telescopes because the radiation at these wavelengths is
absorbed by the Earth's atmosphere.  The Australian Space
Telescope is housed in two GAS canisters that are mounted on
the side of the Shuttle cargo bay and are interconnected by
means of a cable harness.  One of the canisters is fitted with
a Motorized Door Assembly which protects the payload during
launch and opens to allow observations to be made.  This
canister houses the telescope, the detector and the control
computer.

    Endeavour is a 100 mm binocular reflecting telescope.  One
side of the telescope allows all the light from celestial
targets to enter the other side allows only light in a narrow
spectral band.  Thus, by the subtraction of the two signals,
the narrow band image can be studied in detail as the brighter
background is removed.

    The detector is a very sensitive photon counting array
which comprises an image tube, a fiber optic image dissector
and charged coupled arrays.  The detector counts individual
photons, the smallest indivisible packet of light to obtain
maximum efficiency at the low light level produced by these
distant galaxies.

    The second canister contains the battery to supply
electrical power to the payload and video cassette recorders
to record the images for processing on the ground after
landing.  The telescope has a field-of-view of two degrees and
relies on the Shuttle for pointing.  Shuttle motion during
exposures can be removed by subsequent ground image
processing.

    The managing director of Auspace, Mr. T. Stapinski, said
"Endeavour is a very important space project for Auspace.  It
is a very complex payload of over 180 kg. (396 lbs.) and we
learned a lot during its manufacture and testing.

    "The expertise learned on Endeavour has enabled Auspace
engineers to make major contributions on other electro-optical
space instrumentation such as the Along Track Scanning
Radiometer for the European Remote Sensing satellite.  The
Flight of Endeavour is very important as it will demonstrate
the capability of the Australian space industry to produce top
quality space hardware."

COMMERCIAL MDA ITA EXPERIMENTS (CMIX-03)

Overview

     The third in a series of six commercial experiments,
known as CMIX, will fly aboard Endeavour during STS-67.  CMIX-
03 includes biomedical, pharmaceutical, biotechnology, cell
biology, crystal growth and fluids science investigations.

     These experiments will explore ways in which microgravity
can benefit drug development and delivery for treatment of
cancer, infectious diseases and metabolic deficiencies.  These
experiments also will include protein and inorganic crystal
growth, secretion of medically important products from plant
cells, calcium metabolism, invertebrate development and immune
cell functions.

     CMIX represents an innovative dual agreement program
between NASA Headquarters and the University of Alabama in
Huntsville (UAH) Consortium for Materials Development in Space
(CMDS). UAH is one of NASA's eleven Centers for the Commercial
Development of Space (CCDS).  The goals of the program are to
provide increased access to space for NASA's CCDS
investigators and their industry affiliates and to facilitate
private sector utilization of space.  Through a subsequent
agreement between UAH and Instrumentation Technology
Associates (ITA), of Exton, PA, ITA provides flight hardware
to UAH for its associated investigators and industry
affiliates in exchange for flight opportunities.  ITA markets
both the flight opportunity and hardware as a turnkey
commercial service to both domestic and international users.

     On STS-67, UAH and ITA will fly more than 30 individual
experiment investigations totaling some 400 samples on CMIX-
03.

     The most significant UAH CMDS/NASA CCDS experiments on
this mission deal with microgravity research into aging,
multi-drug resistance and neuro-muscular development.

     The most significant ITA commercial experiments on this
flight involve the growth of urokinase protein crystals as the
first step for use in developing an inhibitor drug to combat
breast cancer metasis, and the microencapsulation of drugs as
a drug delivery system for cancer therapy.


UAH CMDS Experiments

     Experiments being conducted by the UAH CMDS and
collaborating scientists on the STS-67 CMIX-03 payload include
aging, multi-drug effects on cells, neuro-muscular
development, gravity sensing and calcium metabolism,
production of plant cell products, and protein crystal growth.
Some of the data expected from the CMIX-03 microgravity
experiments can be used by industry to understand processes
which can enhance the quality of life on Earth, and contribute
to the health and welfare of the increasing numbers of persons
spending time in space.

Aging

     Evidence from previous microgravity experiments indicates
that gravity affects single cells.  No matter what effect any
environmental factor produces on living systems, it begins
with single cells or a group of single cells acting together.
Microgravity appears to slow cell growth.  How this affects
the aging process will be tested using human lymphocytes.


Multi-drug Resistance

     The broad objective of drug resistance experiments is to
gain an understanding of the role of gravity and effect of
microgravity on cell membranes.  Drugs must cross cell
membranes to be effective;  however, many drugs lose their
effectiveness after several years of use because patients
develop multi-drug resistance.  Researchers believe that the
mechanisms of multi-drug resistance may be more easily
understood for cells in microgravity where cellular metabolism
is slowed.

Neuro-muscular Development

     There are a number of diseases which result from faulty
nerve-muscle interactions and these disorders are a target for
pharmaceutical and biotechnology industry research.  The
development of nerve tissue is influenced by the communication
between nerve and muscle cells and depends on membrane
interactions.  Previous flight experiments have shown that
microgravity slows the growth and development of these cells
and significantly alters the cytoskeleton.  Frog cells will be
flown as a model to investigate development of membrane
associated interactions.

Gravity Sensing and Calcium Metabolism

     Calcium is known to regulate many cellular activities
leading to growth, differentiation, and transduction of
signals from the cell membrane to produce genetic responses.
The UAH investigation will fly an experiment using the
Bioprocessing Modules to evaluate the development of gravity
in understanding calcium dynamics in cells and has economical
value in the area of calcium and bone metabolism.


Production of Plant Cell Products

     Pharmaceutical products from plants have been used for
treatment of various types of cancer.  These plant products
include vinblastin and taxol.  Cultured cells from soy bean
plants will be flown in the MDA minilabs to assess the effect
of microgravity on growth, development and production of
secondary metabolites.  These cells, grown in ground-based
tests, produce a product with strong anti-colon cancer
activity.  Preliminary evidence suggests that microgravity may
provide an advantage for higher production of this material.

Protein Crystal Growth

     Protein crystal growth experiments will be flown to gain
information on the specific structure and growth
characteristics of selected economically important proteins.
Information will be used to develop more complex experiments
on future missions.


Commercial ITA Experiments

     The private sector commercial experiments on CMIX-03
utilizing the ITA hardware have three main thrusts: biomedical
research involving the growth of protein crystals for cancer
research;  the microencapsulation of drugs;  and an ITA-
sponsored student space education program.

Urokinase Breast Cancer Experiment

     The most significant commercial experiment on the CMIX-03
payload is an experiment to grow large protein crystals of
urokinase for breast cancer research.  Urokinase is an enzyme
which is present when breast cancer spreads (cancer
metastasis).  ITA, with its team of scientists and engineers,
will dedicate 60 to 90 space experiments to the growth of
large protein crystals of at least 100 microns for analysis.
Small urokinase protein crystals have been grown on the CMIX-
01 (STS-52) and CMIX-02 (STS-56) Shuttle flights.  The
crystals were not large enough for analysis.  Urokinase
protein crystals grown on the ground are not large enough for
analysis.  If a 100+ micron protein crystal can be obtained on
the CMIX-03 mission, the three-dimensional structure will be
determined in the laboratories of crystallographers.  A cancer
research center has agreed to try to develop and test drugs to
inhibit urokinase and hence breast cancer metastasis.

     The scientists and engineers on the research team believe
that the chance of achieving their goal of large urokinase
crystals is enhanced because the STS-67 mission is twice as
long (16 days) as the previous CMIX missions and the growth
rate is believed to be linear.  In addition, the hardware has
been modified to provide two temperatures and four separate
crystal growth techniques.


Microencapsulation of Drugs

     The second major commercial thrust is experiments
involving the encapsulation of drugs or living cells for new
medical therapies.   This series of commercial
microencapsulation experiments will continue the studies
conducted on STS-52 (CMIX-01) and STS-56 (CMIX-02) wherein an
antitumor drug (cis-platinum) was co-encapsulated with a
radiocontrast medium into spherical, multilayer liquid
microcapsules.  This is a commercial joint venture with the
Institute for Research, Houston, TX.

     The objectives of the Microgravity Encapsulation of Drugs
(MED) are for experiments on microcapsules to enable testing
against tumors in mice as a necessary step towards clinical
studies in cancer patients.

     Another separate group of microencapsulation experiments
involves the mixing of polymer solutions which ultimately may
be used to encapsulate pancreatic islet cells to facilitate
transplantation into diabetic patients.

Student Space Education Program

     The third major thrust involves school students as part
of ITA's Student Space Education Program to increase awareness
and interest in science and space technology.  ITA is donating
a portion of its hardware and personnel on every CMIX mission
to flying student experiments as a "hands-on" experience for
students.  To date, some 400 students and 30 teachers from
seven states have participated in this private sector-
sponsored program for students to conduct Space Shuttle
microgravity experiments on the CMIX payload.

CMIX-03 Payload Hardware

     The CMIX-3 hardware consists of four Materials Dispersion
Apparatus (MDA) Minilabs, two of which will contain
experiments developed by the UAH CMDS and its industry
affiliates.  Additional hardware to fly on this mission
includes ITA's Liquids Mixing Apparatus and UAH's
BioProcessing Modules.  The other two MDA'S, commercially
marketed by ITA, will contain experiments developed by ITA's
customers, international users, and university research
institutions.

     Dr. Marian Lewis, of the UAH/CMDS, is the Project Manager
for the CMIX Program and Mr. John M. Cassanto, President of
ITA, is the Program Manager for the commercial half of the
CMIX payload.


Protein Crystal Growth Experiments

     The STS-67 mission will carry two systems in Shuttle
middeck lockers to continue space-based research into the
structure of proteins and other macromolecules.  Vapor
Diffusion Apparatus trays will be housed within a temperature-
controlled Thermal Enclosure System, which fills the area
normally occupied by two lockers.  The Protein Crystallization
Apparatus for Microgravity will be housed in a Single-locker
Thermal Enclosure System.

     Proteins are important, complex biochemicals that serve a
variety of purposes in living organisms.  Determining the
molecular structure of proteins will lead to a greater
understanding of how the organisms function.  Knowledge of the
structures also can help the pharmaceutical industry develop
disease-fighting drugs.

     X-ray crystallography currently offers the best route to
determine the three-dimensional structure of macromolecules,
particularly proteins.  In this technique, researchers grow
crystals of purified proteins, then collect X-ray diffraction
data on the crystals.  The three-dimensional structure is then
determined by analysis of this data.  Unfortunately, crystals
grown in the gravity environment of Earth often have internal
defects that make such analysis difficult or impossible.

     As demonstrated on Space Shuttle missions since 1985,
some protein crystals grown in space ╤ away from gravity's
distortions ╤ are larger and have fewer defects.  The
experiments help develop techniques and methods to improve the
protein crystallization process on Earth as well as in space.

     Both systems will grow crystals using the vapor diffusion
method, which has been highly effective in previous Shuttle
experiments.  In vapor diffusion, water evaporates from a
protein solution and is absorbed by a more concentrated
reservoir solution contained in a wicking material.  As the
protein concentration rises, the protein crystals form.

Vapor Diffusion Apparatus Experiments
Dr. Larry DeLucas
University of Alabama at Birmingham
Birmingham, AL

     This investigation continues a very successful series of
space-based protein crystal growth experiments, which has
produced some of the highest-quality crystals of several
proteins.  Previous experiments have helped determine the
structures of porcine elastase, used to study emphysema;
gamma-interferon, which stimulates the immune system and is
used to treat cancer and viral diseases; and Factor D,
important in understanding the body╒s defenses against
infection.

     On STS-67, the Vapor Diffusion Apparatus experiments will
be contained in a Thermal Enclosure System (TES), which is the
size of two mid-deck lockers.  The TES, set at 72 degrees
Fahrenheit (22 degrees Celsius), will contain four vapor
diffusion apparatus trays, each containing 20 individual
crystallization chambers.  Each experiment chamber includes a
double-barreled syringe containing protein solution in one
barrel and precipitant solution in the other.  A reservoir of
concentrated precipitant solution is contained in the wicking
material lining the experiment chamber.

     To activate the experiments at the beginning of the
mission, a crew member will turn a ganging mechanism on the
side of each tray to push the syringe pistons forward and
extrude the protein droplets onto the syringe tip.  During the
course of the experiments, water molecules will migrate from
the drops through the vapor space to the more concentrated
reservoirs, increasing the protein and precipitant
concentrations in the drops.  The increased concentration in
the drops will initiate crystal growth.  At the end of the
mission, the experiments will be deactivated by drawing the
protein drops and crystals back into the syringes.

     [Vapor Diffusion Apparatus Experiments Graphic]

Protein Crystallization Apparatus for Microgravity
Dr. Daniel Carter
Marshall Space Flight Center
Huntsville, AL

     The Protein Crystallization Apparatus for Microgravity
(PCAM) is the second test of a new design for growing large
quantities of protein crystals in orbit.  It first flew aboard
STS-63 in February 1995.  The apparatus holds more than six
times as many samples as are normally accommodated in the same
amount of space.

     A controlled-temperature enclosure occupying a single
Shuttle mid-deck locker, called the Single-locker Thermal
Enclosure System (STES), will hold six cylinders containing a
total of 378 samples ╤ one of the largest quantities in any
single protein crystal growth experiment to date.  In most
experiments of this type, a single locker accommodated a
maximum of 60 samples.  The STES will maintain temperatures at
72 degrees Fahrenheit (22 degrees Celsius).

     Each cylinder contains nine trays held in position by
guide rods and separated from each other by bumper plates with
springs. The trays are sealed by an adhesive elastomer. Each
tray holds seven sample wells, surrounded by a donut-shaped
reservoir with a wicking material to absorb the protein
carrier solution as it evaporates.

     To start the experiment, a crew member will open the
front of the thermal enclosure, then rotate a shaft on the end
of the cylinder with a ratchet from an orbiter tool kit.  This
will allow diffusion to start and protein crystal growth to
begin.  Near the end of the mission, a crew member will rotate
the shaft in the opposite direction to stop diffusion.

     A few of the candidate proteins for this flight of the
PCAM are human cytomegalovirus assemblin (a factor in virus
duplication), parathyroid hormone antagonist (a controlling
factor in bone growth), pseudoknot 26 (a potential HIV
inhibitor), human antithrombin III (a blood clotting factor),
and an HIV protease/drug complex (a factor in viral
replication).

MIDDECK ACTIVE CONTROL EXPERIMENT

     The Middeck Active Control Experiment (MACE) is designed
to study the active control of flexible structures in space.
In this experiment, a small, multibody platform will be
assembled and free-floated inside the Space Shuttle.  Tests
will be conducted on the platform to measure how disturbances
caused by a payload impacts the performance of another nearby
payload which is attached to the same supporting structure.

     MACE consists of three separate hardware elements: The
Multibody Platform, the Experiment Support Module, and the Ku-
Band Interface Unit.  The Multibody Platform consists of a
long flexible polycarbonate structure.  A two axis gimballing
payload is located at either end, and a three-axis torque
wheel/rate gyro platform is located in the center. By swapping
out certain components, the platform can be reconfigured into
more complex geometries, thereby increasing the complexity of
the control problem. Actuators consisting of 7 motors and two
piezoelectric bending elements and sensors, consisting of rate
gyros, strain gauges, and encoders, are distributed along the
structure to  facilitate active control. The Experiment
Support Module contains all the electronics necessary to
conduct the experiment.  The Ku-Band Interface Unit allows
downlink and uplink of data from the middeck.

     On-orbit, the astronaut will set-up the test article and
attach it to the Experiment Support Module. A series of tests
will be performed by using a hand-held terminal for selecting
and controlling programmed test protocols. The astronaut will
monitor the experiment and videotape its operation. At the end
of each test day, the astronaut will select several of the
test result data files for downlink via the Ku-Band Interface
System. The MACE ground team will use this data to adjust the
test protocols during the mission. These new protocols will be
later uplinked and run on the hardware. MACE is expected to
take 44 hours of on-orbit time.  Mission Commander Steve
Oswald and Pilot William Gregory will operate the hardware on
orbit.

     MACE is an IN-STEP (In-Space Technology Experiments
Program) experiment, sponsored by NASA's Office of Space
Access and Technology, that was developed by the Massachusetts
Institute of Technology in collaboration with Payload Systems,
Inc., NASA's Langley Research Center, and Lockheed Missiles
and Space Company.  The experiment will provide a fundamental
understanding of the effects of microgravity on the
interaction between the dynamics of structures and attached
payloads and validate control strategies and algorithms that
will be applicable to a wide range of future space missions.


Shuttle Amateur Radio EXperiment (SAREX)

     Students from 26 schools in the U.S., South Africa, India
and Australia will have a chance to speak via amateur radio
with astronauts aboard Endeavour during the STS-67 mission.
Ground-based amateur radio operators ("hams") will be able to
contact the Shuttle through automated computer-to-computer
amateur (packet) radio links.  There also will be voice
contacts with the general ham community as time permits.

     Shuttle Commander Stephen S. Oswald (call sign KB5YSR),
pilot William G. Gregory, (call sign KC5MGA), mission
specialists Tamara E. Jernigan (call sign KC5MGF) and Wendy B.
Lawrence (KC5KII) and Payload Specialists Ron Parise (WA4SIR)
and Sam Durrance (N3TQA)  will talk with the students.

     Students in the following schools will have the
opportunity to talk directly with orbiting astronauts for
approximately 4 to 8 minutes:

*  Brewton Elementary School, Brewton, AL (WD4SBV)
*  Watson Elementary School, Huntsville, AR (W5TM)
*  Fullbright Avenue Elementary, Canoga Park, CA (W6SD)
*  Tri City Christian Schools, Vista, CA (KK6FX)
*  Plymouth Center School, Plymouth, CT (KD1OY)
*  Bishop Planetarium & South Florida Museum,
          Bradenton, FL (KB4SYV)
*  Renfroe Middle School, Decatur, GA (KM4LS)
*  Pearl City High School, Pearl City, HI (AH6IO)
*  Waihe'e Elementary School, Wailuku, HI (KH6HHG)
*  Highland Park H.S., Highland Park, IL (W9MON)
*  Kentucky Tech, Montgomery County Area Vocational
           Education Center, Mt. Sterling, KY  (WD4EUD)
*  U.S. Naval Academy, Annapolis, MD (W3ADO)
*  Lutherville Elementary/Ridgely Middle School,
           Lutherville, MD (WA3GOV)
*  Silver Spring/Burtonsville Schools, Silver
           Spring, MD (N3CJN)
*  William Bryant Elementary, Blue Springs, MO  (WA0NKE)
*  Plank Road South School, Webster, NY  (KB2JDS)
*  Lockport H.S., Lockport, NY  (N2IQL)
*  Saint Peters School, Greenville, NC
*  Washington Senior H..S., Washington C.H., OH (N8MNB)
*  Bethany Middle School, Bethany, OK  (KB5KIJ)
*  Tarkington Middle School, Cleveland, TX  (N5AF)
*  Chisum Jr./Sr. H.S., Paris, TX  (KA5CJJ)
*  J.J. Fray Elementary School, Rustburg, VA (K4HEX)
*  Group of Scholars from South Africa, South Africa (ZS5AKV)
*  Little Lillys English School, Bangalore, India  (VY2RMS)
*  Cobram Secondary College, Cobram, Australia  (VK3KLN)


     The radio contacts are part of the SAREX project, a joint
effort by NASA, the American Radio Relay League (ARRL), and
the Radio Amateur Satellite Corp.

     The project, which has flown on 15 previous Shuttle
missions, is designed to encourage public participation in the
space program and support the conduct of educational
initiatives to demonstrate the effectiveness of communications
between the Shuttle and low-cost ground stations using amateur
radio voice and digital techniques.

     Several audio and digital communication services have
been developed to disseminate Shuttle and SAREX-specific
information during the flight.

     The ARRL ham radio station (W1AW) will include SAREX
information in its regular voice and teletype bulletins.

     The amateur radio station at the Goddard Space Flight
Center, (WA3NAN), will operate around the clock during the
mission, providing  SAREX information, retransmitting live
Shuttle air-to-ground audio, and retransmitting many SAREX
school group contacts.

     Information about orbital elements, contact times,
frequencies and crew operating schedules will be available
during the mission from NASA ARRL (Steve Mansfield, 203/666-
1541) and AMSAT (Frank Bauer, 301/286-8496).  AMSAT will
provide information bulletins for interested parties on the
Internet and amateur packet radio.

     Current Keplerian elements to track the Shuttle are
available from the NASA Spacelink computer information system,
computer bulletin board system (BBS) [phone] or via the
Internet: spacelink.msfc.nasa.gov., and the ARRL BBS (203)
666-0578.  The latest element sets and mission information are
also available via the Johnson Space Center (JSC) ARC BBS or
the Goddard Space Flight Center (GSFC) BBS.  The JSC number is
[phone], 9600 Baud or less.  The GSFC BBS is available
via Internet.  The address is wa3nan.gsfc.nasa.gov.


STS-67 SAREX Frequencies

     Routine SAREX transmissions from the Space Shuttle may be
monitored on a worldwide downlink frequency of 145.55 MHz.

The voice uplink frequencies are (except Europe):
144.91 MHz
144.93
144.95
144.97
144.99


The voice uplink frequencies for Europe only are:
144.70
144.75
144.80

     Note:  The astronauts will not favor any one of the above
frequencies.  Therefore, the ability to talk with an astronaut
depends on selecting one of the above frequencies chosen by
the astronaut.

     The worldwide amateur packet frequencies are:

     Packet downlink          145.55 MHz
     Packet uplink            144.49 MHz

     The Goddard Space Flight Center amateur radio club
planned HF operating frequencies are:

     3.860 MHz          7.185 MHz
     14.295            21.395
     28.650


STS-67 CREW BIOGRAPHIES

     Stephen S. Oswald, 43, will lead STS-67's seven-member
crew, serving as Commander. This is his third space flight.

     Selected as an astronaut in 1985.  Oswald was born in
Seattle, WA, but considers Bellingham, WA, to be his hometown.
He received a bachelor of science degree in aerospace
engineering from the U.S. Naval Academy in 1973 and was
designated as a naval aviator in September 1974.  Following
training in the A-7 aircraft, he flew the Corsair-II aboard
the USS Midway from 1975-1977. In 1978, he attended the U.S.
Naval Test Pilot School at Patuxent River, MD. Upon
graduation, he remained at the Naval Air Test Center
conducting flying qualities, performance and propulsion flight
tests on the A-7 and F/A-18 aircraft through 1981.

     Oswald resigned from active Navy duty and joined
Westinghouse Electric Corp. as a civilian test pilot.  During
1983-1984, he was involved in developmental flight testing of
various airborne weapons systems for Westinghouse, including
the F-16C and B-1B radars.  He has logged over 6,000 flight
hours in 40 different aircraft.

     Oswald joined NASA in 1984 as an aerospace engineer and
instructor pilot. Since being selected as an astronaut, he has
served as Pilot for STS-42 and STS-56, flown in January 1992
and April 1993, respectively.  The International Microgravity
Laboratory-1, the primary payload on STS-42, included major
microgravity experiments conducted over the eight-day flight
in Discovery's Spacelab module.  STS-56 was the second
Atmospheric Laboratory for Applications and Science mission.
This nine-day flight also included the deployment and
retrieval of the SPARTAN spacecraft.  With the completion of
his second mission, Oswald has logged more than 400 hours in
space.

     William G. Gregory (Lt. Col., USAF), 37, will serve as
Pilot for STS-67. This is his first shuttle mission.

     Born in Lockport, NY., Gregory received a bachelor of
science degree in engineering science from the Air Force
Academy in 1979, a master of science degree in engineering
mechanics from Columbia University in 1980 and a master of
science degree in management from Troy State University in
1984.

     Between 1981 and 1986, Gregory served as an operational
fighter pilot flying the D and F models of the F-111.  In this
capacity, he served as an instructor pilot at RAF Lakenheath,
U.K., and Cannon Air Force Base, NM.  He attended the USAF
Test Pilot  School in 1987.  Between 1988 and 1990, Gregory
served as a test pilot at Edwards Air Force Base, flying the
F-4, A-7D and all five models of the F-15.  He has accumulated
more than 3,500 hours of flight time in more than 40 types of
aircraft.  Gregory was selected for the astronaut corps in
1990.

     John M. Grunsfeld, Ph.D., 36, also will be making his
first space flight on STS-67.  Grunsfeld will serve as Mission
Specialist 1.

     Grunsfeld was born in Chicago, IL, and received a
bachelor of science degree in physics from the Massachusetts
Institute of Technology in 1980.  He earned a master of
science degrees and a doctor of philosophy degree in physics
from the University of Chicago in 1984 and 1988, respectively.

     Grunsfeld has held a variety of academic positions at
institutions including the University of Chicago, California
Institute of Technology and the University of Tokyo/Institute
of Space and Astronautical Science.  His research has covered
X-ray and gamma-ray astronomy, high energy cosmic ray studies,
and development of new detectors and instrumentation.  He also
has studied binary pulsars and energetic X-ray and gamma ray
sources using NASA's Compton Gamma Ray Observatory, X-ray
astronomy satellites, radio telescopes and optical telescopes.
Grunsfeld was selected as an astronaut in 1992.

     Wendy B. Lawrence, Commander (Select), USN, will serve as
flight engineer and will carry the designation Mission
Specialist 2 during her first shuttle flight.

     Lawrence, 35, was born in Jacksonville, FL, and received
a bachelor of science degree in ocean engineering from the
U.S. Naval Academy in 1981.  She earned a master of science
degree in ocean engineering from the Massachusetts Institute
of Technology and the Woods Hole Oceanographic Institution in
1988.

     Lawrence was designated as a naval aviator in July 1982
and has more than 1500 hours of flight time.  She also has
conducted more than 800 shipboard landings in six different
types of helicopters.  While stationed at Helicopter Combat
Support Squadron SIX, she was one of the first two female
helicopter pilots to make a long deployment to the Indian
Ocean as part of a carrier battle group.  In October 1990, she
reported to the U.S. Naval Academy where she served as a
physics instructor.  Lawrence is a member of the astronaut
class of 1992.

     Tamara E. Jernigan, Ph.D., 35, will serve as the Payload
Commander and Mission Specialist 3 during her third space
flight.

     Born in Chattanooga, TN, Jernigan received a bachelor of
science degree with honors in physics in 1981, and a master of
science degree in engineering science in 1983, both from
Stanford University.  She earned a master of science degree in
astronomy from the University of California-Berkeley in 1985
and earned her doctorate in space physics and astronomy from
Rice University in 1988.

     After graduating from Stanford, Jernigan served as a
research scientist in the  Theoretical Studies Branch at
NASA's Ames Research Center from June 1981 to July 1985.  Her
research interests have included the study of bipolar outflows
in regions of star formation, gamma ray bursts and shock wave
phenomena in the interstellar medium.

     Selected as an astronaut candidate in 1985, Jernigan has
held a wide variety of technical assignments including
software verification in the Shuttle Avionics Integration
Laboratory, operations coordination on secondary payloads,
spacecraft communicator for five shuttle flights, lead
astronaut for flight software development, and chief of the
Astronaut Office Mission Development Branch.

     Jernigan's first shuttle flight was STS-40 in June 1991,
a nine-day mission called Spacelab Life Sciences-1, the first
mission dedicated to investigating how the human body adapted
to microgravity.  Her second mission, STS-52 in October 1992,
was a 10-day flight during which crew members deployed the
Laser Geodynamics Satellite and operated the U.S. Microgravity
Payload-1.  Jernigan has logged about 455 hours in space.

     Samuel T. Durrance, Ph.D., 51, will be returning to space
for a second time as one of two payload specialists for the
ASTRO-2 mission.  He first flew in that capacity on the ASTRO-
1 mission aboard Columbia on the STS-35 flight in December
1990.  Durrance will carry the designation Payload Specialist
1.

     Durrance was born in Tallahassee, FL, but considers
Tampa, to be his hometown.  He earned a bachelor of science
and mater of science degrees in physics from California State
University, Los Angeles, in 1972 and 1974, respectively.  He
then received a doctor of philosophy degree in astrogeophysics
from the University of Colorado in 1980.

     Durrance is a Principal Research Scientist in the
Department of Physics and Astronomy at Johns Hopkins
University, Baltimore, MD.  He is co-investigator for the
Hopkins Ultraviolet Telescope, one of the instruments flying
as part of the ASTRO Observatory.

     Durrance has made International Ultraviolet Explorer
satellite observations of Venus, Mars, Jupiter, Saturn and
Uranus.  He has directed a program to develop adaptive optics
instrumentation resulting in the design and construction of
the Adaptive Optics Coronagraph, which is now being used at
the Palomar Observatory in California.  In addition, he
participated in the design construction, calibration and
integration of the Hopkins Ultraviolet Telescope and the ASTRO
Observatory.  His main astronomical interests are in the
origin and evolution of planets, both in our own solar system
and around other stars.

     Ronald Parise, Ph.D., rounds out the STS-67 crew as
Payload Specialist 2. Parise will be making his second space
flight, having first flown during the ASTRO-1 mission in
December 1990.

     Parise, 43, was born in Warren, OH, and received his
bachelor of science degree in physics with minors in
mathematics, astronomy and geology from Youngstown State
University in 1973.  He received a master of science degree
and a doctor of philosophy degree in astronomy from the
University of Florida in 1977 and 1979, respectively.

     Parise currently is a senior scientist in the Space
Observatories Department of Computer Sciences Corporation in
Silver Spring, MD.  He also is a member of the research team
for the Ultraviolet Imaging Telescope, one of the ASTRO-2
instruments.  Parise has been involved in all aspects of
flight hardware development, electronic systems design and
mission planning activities for the Ultraviolet Imaging
Telescope.  He has studied the circumstellar material in
binary star systems using the Copernicus satellite as well as
the International Ultraviolet Explorer.  His current research
involves the study of the later stages of the evolution of low
mass stars in globular clusters.


                  -END STS-67 PRESS KIT-