The Sloan Digital Sky Survey is a project of the Astrophysical Research Consortium (ARC), a non-profit corporation incorporated in the State of Washington in 1984 for educational and research purposes. The members of ARC include the University of Chicago, the Institute for Advanced Study, Johns Hopkins University, New Mexico State University, Princeton University, the University of Washington, and Washington State University. ARC holds tax-exempt status with the U.S. Internal Revenue Service under Section 501(c)(3), and has been issued Employer Identification Number 91-1265806. ARC is a qualified recipient of federal grants, contracts, and cooperative agreements, and has received several such awards in support of SDSS and other projects. The Consortium has formal financial management and property control systems in full compliance with federal standards, as confirmed by annual audits under OMB Circular A-133.
In this chapter, we discuss the management structure under which the SDSS Project is being carried out. This subject is divided into nine parts:
. . . {16.1} Purpose and Principles
. . . {16.2} Resources
. . . {16.3} Budget
. . . {16.4} Schedule
. . . {16.5} Administration
. . . {16.6} Project Subtasks
. . . {16.7} Advisory Roles
. . . {16.8} Uses of the facility
. . . {16.9} Personnel
which we will address in turn.
The Project is focused on a single goal -- the production of the archive containing imaging and spectroscopic data. Project resources are devoted completely to the hardware, software, and personnel required to complete this task. The entire archive will be made public in a timely manner; this is the justification for requesting public funds.
To outline the management of the Project and its interaction with scientists, we define four groups of scientists:
Scientists holding positions at those institutions which have committed resources and scientists to the SDSS, i.e. the University of Chicago; the Institute of Advanced Study; the Johns Hopkins University; the Japanese Participation Group (a group of Japanese astronomers under the aegis of the University of Tokyo); Princeton University; the University of Washington; the astrophysics groups at the Fermi National Accelerator Laboratory; and the U.S. Naval Observatory. These groups are known hereafter as UC, IAS, JHU, JPG, PU, UW, FNAL, and USNO, respectively.
Scientists from other institutions, invited by the Director on the advice of the Science Advisory Committee (SAC) to participate in the Project because they provide special skills. These participants have full rights to use of the archive for a term approved by the SAC.
Scientists from ARC institutions not providing direct financial resources to the Project (New Mexico State University and Washington State University, hereafter NMSU and WSU, respectively).
Other scientists, the "public" or "community".
The focus on the archive is consistent with the following principles of the Project:
Funds to analyze and publish the results in journals must come from other sources. This proposal contains no such funds for scientists in any of the groups above.
No use of the telescope that does not contribute specifically to the archive for the North Polar Cap Survey or the Southern Deep Survey can take priority over this core survey, and any non-survey related use of the telescope can only proceed on a basis of strict non-interference with the Survey.
Projects not directly related to the main archive can only be carried out if incremental costs are provided from other sources.
The public archive will be distributed on a convenient medium, e.g., CD ROMs. The cost of producing copies (personnel, equipment, software) will be borne on a pro-rata basis by subscribers. The timescale for the distribution is discussed at the end of Section 16.8. We will seek separate funds in lieu of pro-rata charges, but of course cannot guarantee that we will be successful.
The Project is supervised by the Board of Governors of the Astrophysical Research Consortium (ARC). The institutional and human makeup of the Board is listed at the end of this section. Of the seven ARC member institutions, five are providing funds (the "funding institutions"). A generous grant from the Alfred P. Sloan Foundation was made to ARC in March, 1992. In recognition of this grant, the Project has been named the "Sloan Digital Sky Survey", referred to as SDSS.
The Sloan Foundation has committed $10M to the Project. The U.S. funding institutions (UC, IAS, JHU, PU, UW) have given a total of $4.6M to the construction, and are providing in-kind contributions of about $3M in direct staff work (postdocs) on software as well as the senior staff contributions noted below. FNAL is providing computer hardware and software to produce the archive through a Memorandum of Understanding (MOU) with ARC. No funds will change hands, but the anticipated cost to FNAL over ten years is about $10M. The JPG joined the Project in 1992. They have committed $6.0M to the Project, also through an MOU. NSF has committed $5.2M. The USNO expects to provide total funds and in-kind contributions of $4.2M.
The available resources total $42.6M, exclusive of the amount being requested here from NASA. The overall budget is $53.3M. The total does not include any part of the salaries of faculty or senior staff at any of the participating institutions. In the years 1992-1996, these institutions together contributed at least 10 FTEs per year to the Project at no charge. In 1997-2001, the amount of faculty time contributed will be at least 5 FTEs per year to direct service, though a much larger amount of faculty time will be spent on using and improving the archive. We are requesting $7M from NASA, or just under one-third of the operating cost (not counting faculty time). An additional $3.7M in fundraising by ARC will then allow completion of the Project.
Figure 16.1 shows the schedule milestones for key elements of the Project. The following text deals only with 1997 and later years, and is current as of December 1996. The symbols are as follows: D, design; P, procure; F, fabricate; I, integrate; Po, polish; T, subsystem test; S, system test; Co, commission; Ot, observatory test; Op, operate. The current status of the Project is described in Chapter 4.
Once the optics are installed, control system tests will begin, extending through April 1997. The photometric camera will be simultaneously fit and tested, so each CCD can be adjusted to proper tilt and position. The data acquisition system is integrated at the site and ready to receive data from the camera and the spectrograph. When tracking no longer affects image shape, the Photometric Survey will begin. On non-photometric nights, commissioning of the spectroscopic system will be carried out, by using the full fiber system and both spectrographs. The prime goal is to refine target selection for spectroscopy. By the first quarter of 1998, the full system will be commissioned and a significant amount of imaging data will be in hand, run through the pipelines, and placed in the science archive. With optimistic assumptions about weather and operational efficiencies, the Survey will be completed by July 1, 2002. Because only a portion of the currently unfunded costs are requested in this proposal, budget data in this document extend only through the end of 2001.
The polished common- and spectroscopic correctors will be mounted and on the mountain in January 1997. At that point, delivery of all telescope optics will be complete. The remaining deliverables required are the controls software, to be delivered and tested in late Spring 1997); the spectrographs (one is on the mountain and has been fit checked, the other follows in January 1997); the photometric camera (in final assembly, delivery to APO in Spring 1997); and the fiber cartridges (each consisting of a frame, 640 terminated fibers, and a slit head for insertion into the spectrographs). All the pieces for one cartridge are in hand; the remaining nine sets will be delivered at the rate of one per month. Only two cartridges are necessary through the first quarter of 1997.
Simulations will continue using level 1 software, including target selection using the Operational Data Base at FNAL and the loading of processed data into the Operational and Science Data Bases. Over the course of the spectroscopic commissioning, the level 1 code will be converted to final Survey code (level 2).
The funding institutions have agreed to certain principles of operation. It should be noted here that we are summarizing extensive agreements and that this proposal does not supersede those agreements. The following agreement on management was made in September 1989, accepted and approved by the ARC Board in November 1990, and revised November 26, 1996. The makeup of the ARC Board and the SDSS Advisory Council are given in Section 16.9.
Ultimate responsibility for all aspects of the SDSS, including approval of requests for outside funding, rests with the ARC Board of Governors, acting, in the first instance, through the SDSS Advisory Council. The Board appoints a Director and approves the annual budgets. The current Director and Principal Investigator of this proposal is Donald G. York (UC).
Project Schedule The Board is aided in all matters by the Advisory Council, consisting of members appointed by the Board. The Advisory Council meets at least three times per year. It was formerly chaired by J.P. Ostriker (Provost, PU) and is now chaired by J. Peoples (Director, FNAL). Fundraising activities are guided by this group, which works with the Director to initiate proposals or negotiate memoranda of understanding, as appropriate. The Director of the SDSS is appointed by the Board of Governors, and has executive authority for construction of the telescope and operation of the Survey. The Director is advised on scientific issues by the Science Advisory Committee (SAC) and prepares budgets for approval by the Board of Governors. The SAC consists of a representative of each Science Working Group (see below), and others appointed by the Director. It advises the Director, and the Board through the Director, on all scientific issues. It has primary responsibility for formulating policy regarding instrumentation, strategy, telescope scheduling, and publication. Its responsibilities include scientific review and prioritization of proposals from outside, and review of scientific issues arising in the Project. Working Groups have been formed to address specific fields: Large Scale Structure; Clusters of Galaxies; Galaxies; Quasars; Reddening (Galactic); Solar System; Southern Survey; Stars; and Serendipity. The function of these Groups is to consider carefully the complete flow of the data from the CCDs through to final analysis and publication from the point of view of their particular science interests. The working groups define requirements for equipment, observing time, analysis software, and archiving. The Chair of each Working Group is appointed by the Director for a fixed term, and will be responsible for insuring that the goals of the Working Group are achieved. Together with the other members of the Working Group, the Chair will allocate technical and scientific tasks, monitor the progress of projects, decide on matters related to publication, inform other members of the Survey of the progress of the Working Group, act as spokesperson for the Group in making presentations, and perform other tasks as agreed upon by the Chair and the Director. The Working Groups are responsible for defining Key Projects in their area and for marshaling the resources required to carry out scientific research and publishing the results. All funds from agencies, foundations, or the funding institutions are deposited with the ARC Secretary/Treasurer. All contracts and disbursement of funds are executed by the ARC Secretary/Treasurer or by agreement between ARC and an institution acting as agent for ARC. The ARC Secretary/Treasurer reports regularly on account status to the Board and Advisory Council, and initiates audits under OMB Circular A-133. ARC will charge no overhead for this activity. Limited administrative costs charged to the project are treated as direct costs. Agreements between ARC and the funding partners will be based on direct charges only. Other agreements, such as the one for site operations (NMSU), carry overhead at appropriate, federally-audited rates for that institution. Since ARC will cover these costs from other sources, no indirect costs are requested from NASA.
Management Chart
Figure 16.2 shows an overall management chart for the Project. The advisory structure is described below. Finances, including budgeting, reporting, bookkeeping, investments, institutional agreements with ARC, and contract negotiations are handled by Michael Evans. (UW), who reports directly to the ARC Secretary/Treasurer, Donald Baldwin, on these matters.
The Project Manager, Jeffrey Pier, directs all phases of construction and installation, and is on-site at APO half-time to coordinate scheduling for installation. The Project Manager is assisted by a Project Engineer and a Telescope Coordinator.
The Project Engineer (Walter Siegmund) has signature authority on all engineering drawings relating to mechanical parts of the Project (including site, telescope, and instrument issues). He assures that design reviews are ready, assists the Project Manager in conducting the reviews, and assures follow-up of any identified problems.
The camera is nearing construction completion at Princeton under the direction of Jim Gunn. Maki Sekiguchi of the JPG assists Gunn in design work, and managed production of some of the electrical and mechanical parts in Japan.
The spectrographs were designed and constructed under Paul Feldman at JHU. Alan Uomoto is Project Manager. Uomoto handles all procurements and scheduling, and is in charge of test and integration. The fiber system that guides light to the spectrographs depends on fibers fabricated, assembled into groups of 20, and tested by a vendor. Cartridges to hold the fibers between the plug plates and the spectrograph input are managed by Russell Owen (UW). Facilities to actually plug each plate, verify fiber/hole pairs, and move the cartridges to the telescope are managed by Paul Mantsch (FNAL). A machine verified to correctly drill plates exists at UW, and two outside vendors have been used in independent verification tests to assure a robust flow of plates to the site.
Figure 16.2 outlines the organization of the computing management for 1997 and beyond. All computing activities are centralized at FNAL. The computing manpower assigned to computing is divided into two categories: computing professionals in the on-line support group (OLS) at FNAL and scientists in both the Experimental Astrophysics Group at FNAL and at the other member institutions. The scientists working on software include faculty, research staff, and postdoctoral fellows. The overall computing effort is overseen by the Assistant Computing Coordinator, Brian Yanny, who reports directly to Steven Kent (Computing Coordinator).
Prior to summer 1996, two advisory structures existed: the Computing Implementation Advisory Committee (CIAC) and the Science Software Advisory Committee (SSAC), the former to deal with infrastructure and standards and the latter to deal with science software. Now that the level 1 code is being integrated and used for simulations, the data reduction equipment is in place at FNAL, and the infrastructure code, tools, operational database, and mass storage are in place, the advisory status has been consolidated into the group of pipeline coordinators, who meet weekly by phone and every six weeks in person. The software pipelines are the Photometric Pipeline, the Astrometric Pipeline, the Monitor Telescope pipeline, Final Calibration, Target Selection, Plate Specification, and the Spectroscopic Pipeline. Other computing tasks include the Science Archive construction and Survey Strategy (long-term records and planning related to sky coverage and Survey progress).
Revisions to pipeline or infrastructure code are integrated under the supervision of the Science Software Integration Manager, Chris Stoughton. Under the Computing Implementation and Integration Manager, and the daily management of the FNAL Computing Project Manager, the infrastructure code was written, the FNAL resources (tape drives, mass storage, reduction computers) were procured, and the Data Acquisition System at APO was procured and installed. The same structure will be used in maintaining and upgrading computing hardware and software through commissioning.
The Survey Director (Richard Kron) is responsible for coordinating the test year activities in preparation for observations, for the operations itself, for the integrity of the Survey (calibration and uniformity), and for the smooth running of the analysis software and archive activity. He will work closely with the Site Manager and Survey Operations Scientist at Apache Point on issues of staffing, Survey performance, and SDSS instrument maintenance. Likewise, he will work closely with FNAL staff to assure smooth running of the analysis activity, through the Project Scientist, the Data Processing Scientist, and the Plug Plate Production Manager. An Archive Director will also assist him in issues of archiving and distribution. The operation of the site and the employment and support issues will be directly handled by the Site Manager, Bruce Gillespie, through an ARC/NMSU operations agreement, analogous to that used for the ARC 3.5-meter telescope. Observers are now being hired for the SDSS. Maintenance of hardware and software will be supported by members of the construction or programming teams who will be retained for this purpose.
During instrument verification and testing activities, a standing Commissioning Executive Committee (CEC) meets weekly and carries out readiness reviews, progress reviews, and acceptance reviews for all subsystems and, in the end, for the overall spectroscopic and imaging systems in full operation with the operations team in place at both APO and FNAL. The group is chaired by Tom Nash (FNAL). To date, the group has held three readiness reviews (Monitor Telescope, Data Acquisition System, Data Reduction Software) and one progress review (Monitor Telescope). The readiness review for the photometric camera is scheduled for January 30, 1997. The spectrograph and telescope readiness reviews are expected to occur in February. These will be followed by progress reviews as necessary and acceptance reviews throughout 1997, with the final software acceptance review, for the level 2 software, near the end of November 1997.
In addition to the SAC and the Project Engineer, the Director is advised the Project Scientist, Jim Gunn. The Project Scientist monitors the system aspects of the entire Project in its design, construction, and operation phases and evaluates the scientific impact of changes or compromises made in the course of constructing the hardware and preparing the software. If not already on the SAC in another role, the Project Scientist will be present as an ex officio member at all SAC meetings.
Through the summer of 1996, the Project Scientist, Project Engineer, Project Manager, Survey Director, and Project Director formed a council that reviewed project status in monthly meetings (phone conferences or face-to-face, as progress warranted). This group was referred to as the Technical Oversight Group (TOG). It had several rotating positions to be filled by agreement to accommodate critical people at different stages of the Project, depending on where problems developed or better definition was required.
In October 1995, the Project Manager formed an installation task force (ITF) consisting of task leaders, to coordinate installation at the site. This group continues to meet, every four to six weeks, face-to-face.
By summer 1997, an instrumented telescope and associated software will be in place to carry out the Survey. Each year thereafter for at least five years, an incrementally larger archive will be in place.
The telescope will be used primarily to carry out observations for the Survey at the North Polar Cap in the relevant seasons and for the Deep Southern Survey in the Fall. If possible, good-seeing dark nights will be used to extend the Survey to lower Galactic latitudes to the extent feasible. If time is available for other purposes, on a strictly defined non-interference basis, it will be made available through competitive review.
Under the guidelines of the agreement with ARC for use of the site, ARC scientists can begin applying for other projects as soon as the Survey is underway, while non-ARC (group D) scientists can begin applying two years after the Survey begins. All scientists must provide incremental funding for additional projects, including all materials and media costs. Projects requiring funds to be obtained by separate proposal can get a letter of endorsement from the ARC Board, following science review by the SAC, and review by the Director for financial soundness and approval by the Board. The SAC review will include a member of the group C or group D scientists when proposals from each group are being discussed.
The nature of projects to be considered under this scheme are circumscribed by the manner in which the main Survey will be conducted. It will not, for example, be possible to accommodate other instruments or even filter changes, or, at the beginning, any projects which require completely moonless skies (though the last is expected to change as the Survey progresses). Basically, projects can be accommodated which use the Survey instrumentation and software exactly as it is used in the Survey, and, in accordance with the principles of operation above, only when the Survey cannot be done because of sky brightness or hour angle limitations.
Examples of projects which would be entertained include spectroscopic proposals (for stars, say) which can be done in slightly moonlit conditions; imaging proposals at lower latitude which might be similarly done; dark imaging proposals after the expected hour angle gaps between the North and the South develop; proposals for spectroscopy using fibers left over in low-density regions; or proposals for some small amount of imaging or spectroscopy in the South. The latter two depend, of course, on the development of the spectroscopy plan in the South and the serendipity program, but the advantage of opening the Survey in this way to innovative ideas from outside is fully recognized. An example of the sort of project we could entertain is described in Appendix B.
We cannot at this time offer intelligent estimates of how much time might be available, but it seems clear that as the Survey progresses and we understand the calibration better the amount will increase.
In Survey year 4, ARC will begin a process to decide whether to move the telescope to the Southern Hemisphere, or to terminate the activity upon completion of the North Polar Cap Survey. If the decision is to move, equipment will be moved to a new site in the Southern Hemisphere, providing funds can be identified. If the system is left in place, the ARC Board will decide whether to transfer control of the equipment or to operate the Survey instrument for general programs, possibly concurrently with a repeat of the imaging Survey. Proposals for support of the chosen route will then be made, with concurrence of our funding sources.
In what follows, the word "archive" refers to a limited-access data set for use in running the Survey (e.g., generating target lists for the fiber observations from the imaging data) and for use by Survey scientists in checking for completeness and maintaining quality control.
The Survey will be published for general use, at cost. Prior to publication, Group A and B scientists will have full access to the archive at all times. Group C scientists will have special access for specific projects (e.g., lists of clusters to obtain more redshifts), not for general perusal. Archival research proposals will be considered in the same way as are those for telescope time.
The current plan is for other scientists to obtain access through purchased media. The data will be published in usable form two years after completion of the first two years of the Survey. The results will be given to a stated level of completion and calibration accuracy, the best that can be done at the time. The second major release will be two years after completion of the entire Survey and will be complete to the stated goal of the proposal, or the best that can be done at that time. Interim releases of catalogs to some level of completeness will be possible if there is a demand and if sufficient funds are available to cover costs of the preparation and distribution activity and providing that there is not an adverse impact on the conduct and calibration of the Survey itself.
Here we discuss key participants in management and oversight functions.
The Principal Investigator of this proposal, Donald York, is the Project Director. He reports on a regular basis to the SDSS Advisory Council, and ultimately to the ARC Board of Governors. The project, and the Director's responsibilities, can be subdivided into three major categories: construction and commissioning, software development, and operations. The Director delegates these three functions on a daily basis to Jeffrey Pier, Steven Kent, and Richard Kron, respectively (Figure 16.2), with an upper level science advisory role played by Jim Gunn. For all of the above functions, York prepares budgets and reports the financial status of the project to the Advisory Council and the ARC Board of Governors.
The management and policy oversight of the Project is the responsibility of the ARC Board of Governors, acting in the first instance through the SDSS Advisory Council. The Board consists of experienced scientists and administrators, all of whom hold university positions. The two officers of the Board, listed first below, also hold the same title as officers of the formal corporate entity, ARC Inc.
Timothy Heckman, Professor of Physics and Astronomy, Johns Hopkins University: Chairman, Board of Governors, Astrophysical Research Consortium.
Donald Baldwin, Assistant Provost for Research, University of Washington: Secretary/Treasurer, Board of Governors, Astrophysical Research Consortium.
Allen I. Rowe, Associate Director for Finance and Administration, Institute for Advanced Study.
John N. Bahcall, Professor, School of Natural Sciences, Institute for Advanced Study.
Theodore Poehler, Vice Provost for Research, The Johns Hopkins University.
Rene Casillas, Dean, College of Arts and Sciences, New Mexico State University.
Rene Walterbos, Professor and Chairman, Department of Astronomy, New Mexico State University.
James E. Gunn, Professor, Department of Astrophysical Sciences, Princeton University.
Allen J. Sinisgalli, Associate Provost of Research and Project Administration, Princeton University.
Robert Rosner, Chairman, Department of Astronomy and Astrophysics, University of Chicago.
David N. Schramm, Vice President for Research; Professor, Department of Astronomy and Astrophysics, University of Chicago; Theoretical Astrophysical Group, Fermi National Accelerator Laboratory.
Leon J. Radziemski, Dean, Division of Science, College of Science and Arts, Washington State University.
Julie Lutz, Professor, Program in Astronomy, Washington State University.
Bruce Margon, Professor of Astronomy, University of Washington.
The Board is advised on all SDSS matters by the Advisory Council. The Council is chaired by John Peoples, FNAL. The Council consists of all the listed Board members except those from NMSU and WSU (R. Casillas, R. Walterbos, L. Radziemski, and J. Lutz), plus four additional members: Arthur Davidsen, Dean of Faculty of Arts and Sciences and Professor of Physics and Astronomy, Johns Hopkins University; Satoru Ikeuchi, Professor, Osaka University, (representing the JPG); E. Thomas Nash, Fermi National Accelerator Laboratory; and Kenneth Johnston, U.S. Naval Observatory.
The Science Advisory Committee (SAC) consists of a representative of each working group and others as appointed by the Director.
Alex Szalay, Large Scale Structure Working Group: Chair of SAC.
Neta Bahcall, Clusters of Galaxies Working Group.
Masataka Fukugita, Japan Promotion Group.
James Gunn (ex officio), Project Scientist.
Craig Hogan, Southern Survey Working Group.
Steven Kent, at large.
Richard Kron (ex officio), Survey Director.
Gillian Knapp, Reddening Working Group.
Bruce Margon, Serendipity Working Group.
Sadanori Okamura, Galaxy Working Group.
Thomas Quinn, Solar System Working Group.
Robert Rosner, Stars Working Group.
Donald Schneider, Quasars Working Group.
David Weinberg, at large.
Donald York (ex officio), Project Director.
Other key staff appear on the management chart.
The job of the working groups is to continuously review scientific areas in light of technical developments in the Project, considering the impact of technical decisions on the science. When the data come in, the members of these groups will organize themselves to carry out the key science of the project, though no participant is precluded from working individually. The following lists are of the participants by area. The main science interests of each individual are noted.
Alex Szalay, JHU, Co-Chair, observational cosmology, large-scale structure.
Josh Frieman, FNAL, Co-Chair, cosmology.
Neta Bahcall, PU, clusters of galaxies.
Francisco Castander, UC, clusters of galaxies.
Andrew Connolly, JHU, observational cosmology.
Arthur Davidsen, JHU, observational cosmology, QSOs.
Mamoru Doi, U. Tokyo, galaxies, galaxy evolution.
Nancy Ellman, Yale, galaxy evolution.
Masataka Fukugita, U. Tokyo, cosmology.
Jeremy Goodman, PU, binary galaxies and dynamics.
Richard Gott, PU, theoretical cosmology, galaxy formation.
James Gunn, PU, observational cosmology, galaxy formation.
Lam Hui, FNAL, cosmology.
Takashi Ichikawa, JPG, large-scale structure, properties of galaxies.
Gillian Knapp, PU, interstellar matter in galaxies.
Edward Kolb, FNAL/UC, particle physics in the early universe.
Richard Kron, UC/FNAL, observational cosmology, large-scale structure.
George Lake, UW, theoretical cosmology, computational astrophysics.
Donald Lamb, UC, gamma ray sources, neutron stars, theoretical astrophysics.
John Loveday, UC, large-scale structure.
Tim McKay, UMich, weak lensing, cosmic rays.
Avery Meiksin, UC, cosmology.
Jeff Munn, USNO, redshift surveys, large-scale structure.
Tom Nash, FNAL, particle physics.
Heidi Newberg, FNAL, supernovae.
Robert Nichol, UC, clustering of galaxies.
Jeremiah P. Ostriker, PU, theoretical cosmology.
John Peoples, FNAL (Director), particle physics.
Ruth Pordes, FNAL, instrumentation.
Mark Postman, STScI, clusters of galaxies.
William Press, Harvard, astrophysical theory.
Jean Quashnock, UC, cosmology.
Thomas Quinn, UW, N-body simulations, solar system.
Michael Richmond, PU, galaxies, supernovae.
Katsuhiko Sato, U.Tokyo, cosmology.
David Schramm, UC/FNAL, particle physics and cosmology.
Maki Sekiguchi, JPG, large-scale structure, cosmological parameters.
Kazuhiro Shimasaku, U.Tokyo, observational cosmology.
David Spergel, PU, dynamics of galaxies.
Chris Stoughton, FNAL, particle physics, QSOs.
Michael Strauss, PU, cosmology.
Chris Stubbs, UW, lensing, cosmology.
Istvan Szapudi, FNAL, cosmology.
Yasushi Suto, JPG, large-scale structure.
Max Tegmark, IAS, statistical astronomy.
Douglas Tucker, FNAL, large-scale structure.
Michael Turner, UC/FNAL, large-scale structure.
Michael Vogeley, STScI, large-scale structure.
David Weinberg, OSU, large-scale structure.
Neta Bahcall, PU, Chair, clusters of galaxies.
James Annis, FNAL, clusters of galaxies.
Francisco Castander, UC, clusters of galaxies.
Andrew Connolly, JHU, observational cosmology.
Mamoru Doi, JPG, evolution of galaxies and clusters.
Nancy Ellman, Yale, galaxy evolution.
Richard Gott, PU, theoretical cosmology, galaxy formation.
James Gunn, PU, observational cosmology, clusters.
Masaru Hamabe, U.Tokyo, structure and classification of galaxies.
Satoru Ikeuchi, JPG, theoretical cosmology, interstellar physics.
Gillian Knapp, PU, interstellar matter in galaxies.
Richard Kron, UC/FNAL, observational cosmology, large-scale structure.
George Lake, UW, theoretical cosmology, computational astrophysics.
John Loveday, UC, large-scale structure.
Robert Lupton, PU, statistical astronomy.
Tim McKay, UMich, weak lensing, cosmic rays.
Richard Miller, UC, dynamics of clusters, N-body calculations.
Robert Nichol, UC, clustering of galaxies.
Sadanori Okamura, JPG, dynamics and evolution of galaxies.
Michael Richmond, PU, galaxies, supernovae.
Thomas Quinn, UW, N-body calculations, solar system.
Mark Postman, STScI, clusters of galaxies.
Donald Schneider, IAS, high-z QSOs, clusters and cosmology.
Chris Stoughton, FNAL, particle physics, QSOs.
Michael Strauss, PU, cosmology.
Alex Szalay, JHU, observational cosmology, large-scale structure.
Max Tegmark, IAS, statistical astronomy.
Douglas Tucker, FNAL, large-scale structure.
Ed Turner, PU, gravitational lenses, dynamics of clusters.
J. Anthony Tyson, Lucent Technologies, gravitational astronomy, cosmology.
Michael Vogeley, STScI, large-scale structure.
David Weinberg, OSU, large-scale structure.
Sadanori Okamura, JPG, Co-Chair, dynamics and evolution of galaxies.
Michael Strauss, PU, Co-Chair, cosmology.
James Annis, FNAL, clusters of galaxies.
Neta Bahcall, PU, clusters of galaxies.
John Bakken, FNAL, instrumentation.
Francisco Castander, UC, clusters of galaxies.
Andrew Connolly, JHU, observational cosmology.
Mamoru Doi, JPG, evolution of galaxies and clusters.
Nancy Ellman, Yale, galaxy evolution.
Holland Ford, JHU, planetary nebulae, AGN.
Scott Friedman, JHU, observational astronomy.
Masataka Fukugita, JPG, cosmology.
Jeremy Goodman, PU, binary galaxies and dynamics.
James Gunn, PU, formation and dynamics of galaxies.
Masaru Hamabe, U.Tokyo, structure and classification of galaxies.
Doyal (Al) Harper, UC, infrared astronomy, star formation.
Timothy Heckman, JHU, active galaxies.
Shin-ichi Ichikawa, U.Tokyo, dynamics of galaxies and clusters.
Takashi Ichikawa, U.Tokyo, large-scale structure, properties of galaxies.
Satoru Ikeuchi, Osaka, theoretical cosmology, interstellar physics.
Steven Kent, FNAL, dynamics of galaxies, surface photometry.
Ed Kibblewhite, UC, automated faint surveys, adaptive optics.
Gillian Knapp, PU, interstellar matter in galaxies.
Richard Kron, UC/FNAL, faint galaxy surveys, photometry.
George Lake, UW, theoretical cosmology, computational astrophysics.
Donald Long, NMSU (APO), astronomical imaging, observatory operations.
John Loveday, UC, large-scale structure.
Robert Lupton, PU, statistical astronomy.
Tim McKay, UMich, weak lensing, cosmic rays.
Avery Meiksin, UC, cosmology.
Jeff Munn, USNO, redshift surveys, large-scale structure.
Donald Petravick, FNAL, instrumentation.
Ruth Pordes, FNAL, instrumentation.
Mark Postman, STScI, clusters of galaxies.
Thomas Quinn, UW, N-body calculations, solar system.
Michael Richmond, PU, galaxies, supernovae.
Maki Sekiguchi, U.Tokyo, large scale structure, observational parameters.
Kazuhiro Shimasaku, U.Tokyo, observational cosmology.
David Spergel, PU, dynamics of galaxies.
Chris Stoughton, FNAL, particle physics, QSOs.
Chris Stubbs, UW, lensing, cosmology.
Woody Sullivan, UW, radio astronomy, galaxies.
Yasushi Suto, U.Tokyo, large-scale structure.
Alex Szalay, JHU, observational cosmology, large-scale structure.
Max Tegmark, IAS, statistical astronomy.
Douglas Tucker, FNAL, large scale structure.
J. Anthony Tyson, Lucent Technologies, gravitational astronomy, cosmology.
Michael Vogeley, STScI, large-scale structure.
David Weinberg, OSU, large-scale structure.
Rosemary Wyse, JHU, stellar dynamics, stellar populations.
Naoki Yasuda, U.Tokyo, galaxies.
John Bahcall, IAS, Co-Chair, neutrino physics, QSOs.
Donald Schneider, Penn State, Co-Chair, high-z QSOs, clusters and cosmology.
Scott Anderson, UW, QSOs, X-ray sources.
Jim Annis, FNAL, clusters of galaxies.
Neta Bahcall, PU, clusters of galaxies.
Francisco Castander, UC, clusters of galaxies.
Arthur Davidsen, JHU, observational cosmology, QSOs.
Masataka Fukugita, U. Tokyo, cosmology.
Tim Heckman, JHU, active galaxies.
Richard Henry, JHU, cosmic background.
Lewis Hobbs, UC, interstellar medium, primordial abundances.
Craig Hogan, UW, cosmology.
Lam Hui, FNAL, cosmology.
Satoru Ikeuchi, Osaka, theoretical cosmology, interstellar physics.
Edward Jenkins, PU, interstellar and intergalactic medium.
Gillian Knapp, PU, interstellar matter in galaxies.
Arieh Konigl, UC, astrophysical jets, abundances, theoretical astrophysics.
Ronald Kollgaard, FNAL, X-ray source identification.
Julian Krolik, JHU, QSO physics.
Richard Kron, UC/FNAL, observational cosmology, large-scale structure.
John Loveday, UC, large-scale structure.
Bruce Margon, UW, AGN, high energy astrophysics.
Tim McKay, UMich, weak lensing, cosmic rays.
Avery Meiksin, UC, cosmology.
Warren Moos, JHU, plasma physics.
Jeff Munn, USNO, redshift surveys, large-scale structure.
Heidi Newberg, FNAL, supernovae.
Sadanori Okamura, U.Tokyo, dynamics and evolution of galaxies.
Jeremiah P. Ostriker, PU, intergalactic medium, QSO physics.
Michael Richmond, PU, galaxies, supernovae.
Kazuhiro Shimasaku, U.Tokyo, observational cosmology.
Chris Stoughton, FNAL, particle physics, QSOs.
Michael Strauss, PU, cosmology.
Chris Stubbs, UW, lensing, cosmology.
Edward Turner, PU, gravitational lenses, QSO physics.
Alan Uomoto, JHU, stellar astronomy, supernovae.
Brian Yanny, FNAL, intergalactic medium, globular clusters.
Donald York, UC, interstellar and intergalactic medium.
Gillian Knapp, PU, Chair, interstellar matter in galaxies.
Andrew Connolly, JHU, observational cosmology.
James Gunn, PU, observational cosmology.
Lewis Hobbs, UC, interstellar medium, primordial abundances.
Robert Nichol, UC, clusters of galaxies.
Michael Richmond, PU, galaxies, supernovae.
Michael Strauss, PU, cosmology.
Alex Szalay, JHU, observational cosmology, large-scale structure.
Alan Uomoto, JHU, stellar astronomy, supernovae.
Michael Vogeley, STScI, large-scale structure.
Bruce Margon, UW, Chair, AGN, high energy astrophysics.
Scott Anderson, UW, QSOs, X-ray sources.
Jim Annis, FNAL, clusters of galaxies.
Arthur Davidsen, JHU, observational cosmology, QSOs.
Paul Feldman, JHU, comets, planetary atmospheres.
Richard Gott, PU, theoretical cosmology, galaxy formation.
Robert Hindsley, USNO, astrometry.
Satoru Ikeuchi, JPG, theoretical cosmology.
Ed Kibblewhite, UC, automated faint surveys, adaptive optics.
George Lake, UW, theoretical cosmology, computational astrophysics.
Daniel Long, NMSU (APO), astronomical imaging, observatory operations.
Robert Lupton, UC, statistical astronomy.
Tim McKay, UMich, weak lensing, cosmic rays.
Avery Meiksin, UC, cosmology.
Heidi Newberg, FNAL, supernovae.
Robert Nichol, UC, clusters of galaxies.
Jeremiah P. Ostriker, PU, condensed matter, dark matter.
Bohdan Paczynski, PU, variable stars, supernovae, gravitational lenses.
Michael Richmond, PU, galaxies, supernovae.
Donald Schneider, Penn State, dwarf stars.
Maki Sekiguchi, U.Tokyo, large-scale structure, cosmological parameters.
Chris Stoughton, FNAL, particle physics, QSOs.
Michael Strauss, PU, cosmology.
Chris Stubbs, UW, lensing, cosmology.
Woodruff Sullivan, UW, radio astronomy, galaxies.
Paula Szkody, UW, variable stars.
Edward Turner, PU, QSOs, gravitational lenses.
John (Tony) Tyson, Lucent Technologies, gravitational astronomy, cosmology.
Alan Uomoto, JHU, stellar astronomy, supernovae.
Thomas Quinn, UW, Chair, N-body calculations, solar system.
Donald Brownlee, UW, solar system dust, meteorites.
Paul Feldman, JHU, comets, planetary atmospheres.
Greg Hennessy, USNO, astrometry.
Robert Hindsley, USNO, astrometry.
Donald Pascu, USNO, asteroids.
Michael Richmond, PU, galaxies, supernovae.
Walter Siegmund, UW, telescope engineering, asteroids.
Michael Strauss, PU, cosmology.
Pat Waddell, UW, telescopes.
Craig Hogan, UW, Chair, cosmology.
Scott Anderson, UW, QSOs, X-ray sources.
Jim Annis, FNAL, clusters of galaxies.
Francisco Castander, UC, clusters of galaxies.
Mamoru Doi, U.Tokyo, galaxies, galaxy evolution.
Josh Frieman, FNAL/UC, cosmology.
James Gunn, PU, observational cosmology, galaxies.
Greg Hennessy, USNO, astrometry.
Robert Hindsley, USNO, astrometry.
Steven Kent, FNAL/UC, dynamics of galaxies, surface photometry.
Gillian Knapp, PU, interstellar matter in galaxies.
Richard Kron, UC/FNAL, faint galaxy surveys, cosmology.
Jonathan Loveday, UC, large-scale structure.
Tim McKay, UMich, weak lensing, cosmic rays.
Avery Meiksin, UC, cosmology.
Heidi Newberg, FNAL, supernovae.
Robert Nichol, UC, clusters of galaxies.
Bohdan Paczynski, PU, stellar evolution, variable stars, supernovae.
Donald Petravick, FNAL, instrumentation.
Ruth Pordes, FNAL, instrumentation.
Michael Richmond, PU, galaxies, supernovae.
Robert Rosner, FNAL, Galactic X-ray sources, dynamics.
Donald Schneider, Penn State, QSOs, high z QSOs, dwarf stars.
Walter Siegmund, UW, telescope engineering, asteroids.
Allyn Smith, UMich, photometry, photometric standards.
Chris Stoughton, FNAL, particle physics, QSOs.
Michael Strauss, PU, cosmology.
Chris Stubbs, UW, lensing, cosmology.
Alex Szalay, JHU, observational cosmology, large-scale structure.
Paula Szkody, UW, variable stars.
Max Tegmark, IAS, statistical astronomy.
Alan Uomoto, JHU, stellar astronomy, supernovae.
Michael Vogeley, STScI, large-scale structure.
David Weinberg, OSU, large-scale structure.
Donald York, UC, interstellar and intergalactic medium.
Robert Rosner, UC, Chair, Galactic X-ray sources, dynamics.
Jim Annis, FNAL, clusters of galaxies.
John Bahcall, IAS, galactic structure, neutrino astronomy.
Kyle Cudworth, UC, star clusters, astrometry, stellar evolution.
Conard Dahn, USNO, stellar parallaxes.
Douglas Duncan, UC, primordial abundances, halo stars.
Masataka Fukugita, U.Tokyo, cosmology, photometric standards.
Hugh Harris, USNO, globular clusters.
Greg Hennessy, USNO, astrometry.
Robert Hindsley, USNO, astrometry.
Lewis Hobbs, UC, interstellar medium, primordial abundances.
Kenneth Johnston, USNO (Scientific Director), astrometry, VLBI.
Gillian Knapp, PU, late stages of stellar evolution.
Donald Lamb, UC, gamma ray sources, neutron stars, theoretical astrophysics.
Robert Lupton, PU, star clusters and low mass stars.
Bruce Margon, UW, AGN, high energy astrophysics.
Tim McKay, UMich, weak lensing, cosmic rays.
David Monet, USNO, astrometry.
Jeff Munn, USNO, redshift surveys, large scale structure.
Bohdan Paczynski, PU, stellar evolution, variable stars, supernovae.
Donald Petravick, FNAL, instrumentation.
Jeff Pier, USNO, RR Lyr stars, galactic structure.
Michael Richmond, PU, galaxies, supernovae.
Donald Schneider, Penn State, QSOs, dwarf stars.
Allyn Smith, UMich, photometry, photometric standards.
David Spergel, PU, star clusters, X-ray sources.
Ronald Stone, USNO, astrometry.
Chris Stoughton, FNAL, particle physics, QSOs.
Michael Strauss, PU, cosmology.
Paula Szkody, UW, variable stars.
James Truran, UC, stellar evolution, supernovae.
Alan Uomoto, JHU, stellar astronomy, supernovae.
Peter Vandervoort, UC, stellar dynamics.
Rosemary Wyse, JHU, stellar dynamics, stellar populations.
Norbert Zacharias, USNO, reference frames.