V O L 2 2 I S S U E 0 3

Space Telescope Science Institute

Getting so Much The caption for this figure is located on page 3.

Better all the Time Figure 1:

B. Margon, [email protected]

here is, alas, no special nomenclature for a 15th anniversary. value to the public. The program has been responsible for a large number

It is five years short of the vigenary date, or perhaps can be of famous, widely circulated Hubble images. Even with this past high expressed as the sum of the decennial and quinquennial years. standard, the Heritage team, led by Keith Noll, outdid themselves for But for Hubble Space Telescope, the passage of April 25, 2005, this special occasion with two new multicolor images surely destined to exactly 15 years after the deployment of the satellite from the become iconic: a wide-field exposure of M51 (the Whirlpool Galaxy) with TShuttle Discovery, could not be allowed to pass unnoted for lack of a its companion NGC 5195, and a large section of M16 (the Eagle Nebula), name. It is unusual for any high-technology scientific experiment to remain centered about 10 arcminutes away from the already famous image from

productive and in the forefront of both the discipline and the public for such the Wide Field and Planetary Camera 2 (WFPC2). The huge number of 2 0 0 5 an extended time interval, and certainly extraordinary for its productivity pixels and wide field of view of ACS, compared with its predecessor Hubble and fame to continually increase with age for such a lengthy time. Yet by cameras, enabled breathtaking results for both images. most metrics, this is indeed the case for Hubble. Therefore, a variety of Thanks to frantic work by John Stoke and colleagues in the Institute’s celebrations and commemorative activities seemed more than justified Office of Public Outreach, the two new Heritage images were released to this spring. Multiple events and opportunities occurred for the public, for the public in a particularly dramatic form, namely as 4 × 6 foot prints— the astronomical community, and for the Hubble family. predistributed, but embargoed against display until the anniversary day— A centerpiece of the celebration was the release of two new images to more than 100 museums, planetariums, and related informal science obtained by the Advanced Camera for Surveys (ACS) under the aegis of education venues across the nation, plus a few abroad. A variety of ancillary the Hubble Heritage program. Heritage images utilize a small, annually explanatory materials (lithographs, PowerPoint files, reviewed grant of the Institute Director’s Discretionary time to obtain DVDs) accompanied the giant, hundred-million-pixel Continued

page  S U M M E R exposures of targets deemed to be of the greatest interest and educative prints. The recipient institutions ranged from the DIRECTOR’S PERSPECTIVE

Hubble’s Future S. Beckwith, [email protected]

n April 2005, Hubble received a new lease on life at the Senate confirmation hearing for Michael Griffin as the NASA Administrator. In response to a question by Senator Pryor, Griffin spoke eloquently on Hubble’s contribution to science and indicated his interest in re-examining the question of servicing Hubble following the return to flight of the space shuttle. In testimony to the House Science Committee on June 28, he stated his intention to recommend another servicing mission to Hubble, if the first two space shuttle flights meet their technical goals.

He has already directed the Hubble project team at Goddard to start Hubble has also played an important role in building public support for preparing for the next servicing mission, SM4, assuming use of a space astronomy. It is certainly the world’s most recognized telescope and is shuttle, as in the past. NASA has internally identified December 2007 as perhaps the world’s most recognized scientific instrument. Following a a launch date for planning purposes. successful servicing mission, the continuing stream of interesting science Griffin has promised that the Science Missions Directorate will not pay from Hubble should make it easier to maintain support for additional public for the shuttle costs, as some feared; those will come from the same investment in astronomical research—a cause that all readers of this budget line that normally funds the space shuttle program. Newsletter will surely support. We will need that support to weather the A new feature of SM4 is NASA’s requirement that the mission include inevitable crises that will occur as new projects could run into technical the installation of a de-orbit module for the end of Hubble’s life. This and financial difficulty. requirement is a prudent use of NASA’s resources, because it obviates In the seven years I have been associated with the Hubble program, I the need for a separate robotic mission in the future, which would be at have become increasingly aware of the emotional appeal it has to people great cost to the Science Missions Directorate. NASA policy states that whose daily lives are otherwise disconnected from questions about the Hubble must be safely de-orbited at the end of its mission; this requires universe. I have met people from all walks of life who have been touched the assistance of a propulsion system to guide its re-entry into the by the work astronomers do. Making the most of Hubble’s science atmosphere. NASA had planned to develop a robotic mission that would opportunities should help maintain their support for the foreseeable autonomously mount the propulsion system. Equipping Hubble with a de- future. W orbit module during SM4 has the potential to save hundreds of millions of dollars that would have been spent on a robotic mission. A successful SM4 will bring several additional benefits beyond the savings to the science budget. The longer life for Hubble’s science program and the enhanced quality and scope enabled by the new instruments will benefit Hubble’s users. The extra years of science will be popular with the public, whose support for servicing has been unwavering since the cancellation of SM4 on January 16, 2004. Servicing Hubble will also be a wonderful way to show the utility of the space shuttle following its return to flight, a benefit to the human spaceflight program.

 world famous (e.g., the Rose Center, Museum of Natural History in New York and the Exploratorium in San Francisco), to the perhaps not so famous (the Hitchcock Nature Center of Pottawattamie County, Honeycutt, Iowa), to the heartwarming (U.S. Navy youth centers in Guam and Iceland). My personal favorite case is the print circulating in rural Alaska by dogsled, under the sponsorship of the Alaskan Express Freight Sled Expedition, formerly known as the Iditarod.

Figure 2: The Hubble Heritage Image of M51 (the Whirlpool Nebula) and its interacting companion NGC 5195. This is a montage of six pointings obtained with the Hubble ACS, superposing data from B, V, I, and Hα filters.

In a somewhat more traditional unveiling, the Smithsonian National Air and Space Museum (NASM) on the Mall in Washington DC accepted the large Heritage Whirlpool image for permanent display in an April 25th ceremony attended by more than 100 government, scientific, and industry leaders, including the new NASA Administrator, Dr. Michael Griffin. The event included a brief new IMAX film, produced collaboratively by the Institute’s Office of Public Outreach and the IMAX Corporation. The film pans slowly through the two ACS images. The 60-foot screen and the hundred-million-pixel scenes seemed well matched! A variety of other new Hubble images joined the NASM collection as part of this ceremony. The large ACS Whirlpool image, dramatically backlit, now graces the entrance to the permanent “Explore the Universe” astronomy exhibit, which, fittingly enough, has long employed small, ground-based images of M51 as the repeating icon for that collection. The 24 orbits of observing time invested in the M51 images, although less than 1% of the time available to General Observers (GOs) in Cycle 13, was still substantial by Heritage standards. Figure 1: (Cover Image) Therefore, the Institute was anxious that the data serve double duty—by having its value for the scientific community optimized to every extent possible. Certainly it is not every day that an entire A 3 arcmin wide section of the Eagle nearby face-on spiral is imaged on 0.05 arcsec pixels to limiting B magnitude of 27! Rob Kennicutt Nebula, M16, obtained with the Hubble of Steward Observatory kindly served as a “science advocate” during the time the observations ACS. This Heritage image is a montage were configured, and the Institute announced the upcoming public release of the data (also on the of two pointings, superposing data from anniversary date), together with the details of the observation, well prior to the Cycle 14 proposal B, V, I, [O III], and Ha filters. The field deadline. The community was invited to propose Archival Research programs to analyze these of the other, very famous image of this unique data for publication, and provided the opportunity for normal GO object from WFPC2 is about 10 arcmin proposals to supplement the Heritage data with additional exposures, as distant and thus does not overlap these Continued well. (No special Hubble time was allocated; these proposals competed in page 4 new data. the normal Cycle 14 peer review process with all other programs.)

 This research component of the anniversary program succeeded well beyond our expectations. 15th Anniversary from page 3 Nineteen proposals to utilize the M51 Heritage data for scientific analysis were received in Cycle 14, and the peer review process selected five of them, four archival, and one for acquisition of new data. The latter program will result in Near Infrared Camera and Multi-Object Spectrometer (NICMOS) H and WFPC2 U images to complement the unique ACS data set. Less than one-half year after the Heritage data were obtained, nature cooperated with our hope that the observations would prove to be scientifically unique as well as of public interest: the bright supernova SN 2005cs appeared in M51, and the ACS images have already proven fundamental in the identification of the progenitor star and studies of the nearby environment. Finally, the Institute, as well as the NASA Goddard Space Flight Center—home of the pers Hubble Project—each had their own internal Pa anniversary celebrations. The Institute’s ceremony included a variety of talks on the Institute’s outreach efforts for the milestone, the scientific significance of the two Heritage

# Refereed images, retrospectives of Hubble’s greatest scientific achievements, and projections of its scientific future. At Goddard, a group of NASA and Institute scientists and engineers, whose collective Hubble experience easily Publication Year exceeds a century, reviewed and reminisced, capped with comments from astronomer/ Figure 3: Refereed papers based on Hubble data. astronaut John Grunsfeld, the only person to both observe with Hubble and also visit it (twice) on-orbit. Candidly, we were unsure quite what to expect in the way of public response to this event, which is so important to all who have worked on Hubble. After all, although the two Heritage images are beautiful and scientifically significant, a 15th birthday is not exactly “news,” especially in these turbulent times. The media’s response to the various 15th anniversary events was, in fact, nothing short of overwhelming. According to statistics compiled by Goddard and the Institute, more than 660 press accounts of the event appeared, and television recorded an astounding Nielsen audience of just under 50 million in the April 24–26 interval. Even the U.S. Congress was captivated: on April 28, House Resolution 251 was introduced to the floor, “Congratulating all of the individuals and organizations on the 15th anniversary of the launch of the Hubble Space Telescope that have helped make Hubble one of the most important astronomical instruments in history.” The public clearly adores Hubble and its results. Nevertheless, as astronomers, our currency is surely not the Nielsen rating, impressive though it is, but rather the results appearing in refereed journals. In this regard, Hubble remains just as impressive in year 15 (see Figure 3). In 2004, more refereed papers from Hubble data appeared than in any year since launch, capping a virtually perfect, continuous rise in this statistic. Among its other extraordinary properties, Hubble is, as the Beatles said about school, “getting so much better all the time.” W

Get Your Own Hubble Photos

ou can’t travel to the Eagle Nebula or the Whirlpool Galaxy, but the new Astronomy Printshop section of Hubblesite offers quality Hubble photos that Y you can print out as you would a digital picture. These gallery-quality images are designed to be printed out by a photo store, photo kiosk, or online photolab, though you can also use a home printer. Take a piece of the universe home with you! To find out more visit http://hubblesite.org/gallery/printshop/.

 The Cycle 14 TAC Results

D. Macchetto, [email protected], R. Williams, [email protected], & B. Blacker, [email protected]

Overview he Cycle 14 science program of the Hubble Space Telescope was defined by the peer review of the Time Allocation Committee (TAC), which took place in Baltimore on 14–19 March 2005. The TAC evaluated all proposals and recommended programs to the Director for awards of observing time and archival research funding. The principal investigators (PIs) of selected programs were notified within three weeks of the TAC meetings. The Tfirst observations for Cycle 14 programs should begin execution in July 2005, only six months after submission of the proposals. Due to the failure of the Space Telescope Imaging Spectrograph, Cycle 14 is the first for which no moderate- or high-resolution spectroscopy will be available on Hubble. As a result, the number of proposals submitted—727—was less than the 949 in Cycle 13. The resulting oversubscription rate in requested orbits was 4.8 to 1, as shown in the accompanying figures. In Cycle 14, proposers found the Astronomer's Proposal Tool package easier for Phase I submissions than in Cycle 13, due partly to their increased familiarity with the software and partly to improvements made since the last cycle. The possibility that much of Cycle 14 might be executed with degraded pointing performance in two-gyro pointing mode required extra preparation for all proposals. PIs were asked to specify the requirements of their programs for both normal three-gyro pointing and degraded two-gyro pointing. Testing after the Cycle 14 deadline found little degradation of the pointing performance in two-gyro mode. Peer Review Process and Results The peer review process for Cycle 14 was essentially the same as in recent cycles (described in the summer 2004 Newsletter). One important change, implemented at the suggestion of previous panelists and the Space Telescope Users Committee (STUC), was broadening the base of the pre-meeting triage to include evaluations by all panelists, rather than only those of the primary and secondary reviewers of a proposal. Although this change required significantly more time and effort, it generated positive feedback from all panelists. The triage removed from consideration the bottom third of the proposals of each panel. The distributions of selected proposals across disciplines and between larger and smaller programs were similar to previous cycles (see accompanying tables and figures). A substantial fraction of Cycle 14 observations continue to be devoted to extragalactic astronomy. The increasing size, breadth, and value of the Hubble archive is attracting more attention, and the oversubscription of funding requests for Hubble archival research increased from previous cycles and now approaches the oversubscription in the General Observer program. Treasury and Other Large Programs The only Treasury program approved by the TAC will exploit the slitless grism capability of the Advanced Camera for Surveys (ACS) to obtain spectra of faint galaxies in the Hubble Ultra Deep Field (HUDF), some of which will undoubtedly exhibit high redshifts and provide information on the reionization of the early universe. The TAC approved other large programs (over 100 orbits) in Cycle 14. Infrared imaging in the HUDF will seek to detect additional candidates for high-redshift galaxies. An earlier study of the sources of gamma-ray bursts, which elucidated the possible connection with massive stars, will continue. An earlier supernova program, which found the first evidence for the accelerating expansion of the universe, will continue studies of distant Type Ia supernovae in dust-free environments. Another large program is devoted to obtaining astrometric positions of nearby stars for which accurate radial velocity measurements have indicated the presence of planets. The Hubble Fine Guidance Sensors will attempt to detect small, milliarcsecond variations in the positions of the candidate stars. Positive detections, together with the radial-velocity measurements, would constrain the orbital inclinations of the planets, thus enabling the determination of reliable planetary masses. Future Cycles We do not foresee major changes in the TAC peer review process in future cycles. The capabilities of the telescope will change over time due to Continued page  ageing equipment and, if another servicing mission is undertaken, from the

 installation of new instruments. Such changes could modify the information requested for Phase I Cycle 14 Review from page 5 proposal submission. We have already discussed some changes to the proposal form with STUC, particularly to clarify the information requested on “previous observations.” Defining the Hubble science program is one of the most important features of the Institute’s mission, and community involvement in the TAC process is crucial to its success. We are indebted to the many panelists who devote their time and energy to evaluating Hubble proposals and writing the panel assessments and comments that are passed on to the PIs. We thank them—and especially the Cycle 14 TAC Chair, Dr. Roger Blandford—for their diligent work. In briefing the Institute on its recommendations to the Director, the TAC members emphasized how impressed they were with the overall quality of the proposals for this cycle. TAC members who have served as panelists in previous cycles affirmed that, in their experience, the quality of the proposed observations for this cycle was as high as it has ever been and they are confident that important discoveries will come from the Hubble observations of Cycle 14. W

Elusive Planet Reshapes a Ring Around Neighboring Star

his view, taken by NASA’s Hubble Space Telescope is the most detailed visible-light image ever taken of a T narrow, dusty ring around the nearby star Fomalhaut (HD 216956). The image offers the strongest evidence yet that an unruly and unseen planet may be gravitationally tugging on the ring. Part of the ring [at left] is outside the telescope’s view. Hubble unequivocally shows that the center of the ring is a whopping 1.4 billion miles (15 astronomical units) away from the star. This is a distance equal to nearly halfway across our solar system. The geometrically striking ring, tilted obliquely toward Earth, would not have such a great offset if it were simply being influenced by Fomalhaut’s gravity alone.

http://hubblesite.org/newscenter/newsdesk/archive/releases/2005/10/ Credit: NASA, ESA, P. Kalas and J. Graham (University of California, Berkeley), and M. Clampin (NASA’s Goddard Space Flight Center)

 Cycle 14: TAC and Panel Members

Member Institution Member Institution

TAC Chair Extragalactic Panel Members Roger Blandford Standford University Roberto Abraham University of Toronto Itziar Aretxaga Instituto Nacional de Astrofísica, Óptica y Electrónica Solar System Panel Members Dave Axon (Chair) Rochester Institute of Technology Matthias Bartelmann Universität Heidelberg Fran Bagenal (Chair) University of Colorado at Boulder Aaron Barth University of California - Irvine Lotfi Benjaffel CNRS, Institut d’Astrophysique de Paris Eric Bell Max-Planck-Institut für Astronomie, Heidelberg Paul Feldman The Johns Hopkins University George Bendo University of Arizona Doug Hamilton University of Maryland Katherine Blundell University of Oxford Joachim Saur The Johns Hopkins University Applied Physics Laboratory Joel Bregman University of Michigan Amy Simon-Miller NASA Goddard Space Flight Center Andrew Bunker University of Exeter Chad Trujillo Gemini Observatory, Northern Operations Allesandro Capetti Osservatorio Astronomico di Torino Mike Wolff Space Science Institute Jane Charlton The Pennsylvania State University Laura Woodney University of Central Florida Danny Dale University of Wyoming Eliot Young Southwest Research Institute Gianfranco De Zotti INAF, Osservatorio Astronomico di Padova Michael Dopita The Australian National University Galactic Panel Members Eric Emsellem Observatoire de Lyon Sandra Faber University of California - Santa Cruz Rachel Akeson California Institute of Technology Laura Ferrarese Rutgers, the State University of New Jersey John Bally University of Colorado at Boulder Jacqueline Fischer Naval Research Laboratory Fabio Bresolin University of Hawaii Karl Gordon University of Arizona Bruce Elmegreen (Chair) IBM T.J. Watson Research Center Fred Hamann University of Florida Cesara Esteban Instituto de Astrofísica de Canarias/Universidad Jason Harris University of Arizona de La Laguna Kelsey Johnson University of Virginia Jose Franco Universidad Nacional Autónoma de México (UNAM) Lisa Kewley University of Hawaii Peter Garnavich University of Notre Dame Gillian Knapp Princeton University John Gizis University of Delaware Jean-Paul Kneib Observatoire de Marseille Jules Halpern Columbia University Ken Lanzetta Stony Brook University Suzanne Hawley University of Washington Jennifer Lotz University of California - Santa Cruz Todd Henry Georgia State University Research Foundation Lori Lubin University of California - Davis Lynne Hillenbrand California Institute of Technology Paul Martini Harvard-Smithsonian Center for Astrophysics John Hillier University of Pittsburgh Francesca Matteucci INAF, Osservatorio Astronomico di Trieste Ivan Hubeny University of Arizona Richard Mushotzky (Chair) NASA Goddard Space Flight Center John Hutchings Herzberg Insitute of Astrophysics Ramesh Narayan Harvard University Rodrigo Ibata Université de Strasbourg 1 Colin Norman (Chair) The Johns Hopkins University Hugh Jones University of Hertfordshire Sally Oey University of Michigan Michael Jura University of California - Los Angeles Ernesto Oliva INAF, Osservatorio Astronomico di Arcetri Gloria Koenigsberger (Chair) Universidad Nacional Autónoma de México (UNAM) Michael Pahre Harvard-Smithsonian Center for Astrophysics David Koerner Northern Arizona University Eric Perlman University of Maryland Baltimore County Chryssa Kouveliotou NASA Marshall Space Flight Center Saul Perlmutter University of California - Berkeley Sandy Leggett Joint Astronomy Centre (JAC) Hans-Walter Rix Max-Planck-Institut für Astronomie, Heidelberg Kevin Luhman Harvard-Smithsonian Center for Astrophysics Piero Rosati European Southern Observatory - Germany Peter Lundqvist Stockholm University David Sanders University of Hawaii Mordecai-Mark Mac Low American Museum of Natural History Henrique Schmitt Naval Research Laboratory Phil Massey Lowell Observatory Alice Shapley University of California - Berkeley Antonella Natta (Chair) Osservatorio Astrofisico di Arcetri Thaisa Storchi-Bergmann Universidade Federal do Rio Grande do Sul Alberto Noriega-Crespo California Institute of Technology Jean Surdej Université de Liège Bob O’Dell (Chair) Vanderbilt University Roger Thompson University of Arizona Ruth Peterson University of California - Santa Cruz Christy Tremonti University of Arizona John Raymond Harvard-Smithsonian Center for Astrophysics Pieter van der Kruit (Chair) Kapteyn Astronomical Institute Harvey Richer University of British Columbia Stefan Wagner Landessternwarte Heidelberg Carmelle Robert Université Laval Martin Ward (Chair) University of Durham Edward Robinson University of Texas at Austin Robert Rubin NASA Ames Research Center Ata Sarajedini University of Florida Richard Shaw National Optical Astronomy Observatories Nick Suntzeff National Optical Astronomy Observatories - CTIO Xander Tielens Kapteyn Astronomical Institute Monica Tosi (Chair) Osservatorio Astronomico di Bologna Stefanie Wachter California Institute of Technology Don Winget University of Texas at Austin Adolf Witt University of Toledo

 Proposals by Country

Country Submitted Approved Australia 6 2 Austria 1 0 Belgium 2 2 Brazil 1 0 Summary of Cycle 14 Results Canada 8 2 Chile 1 1 Denmark 1 0 France 8 2 Proposals Requested Approved % Accepted ESA Accepted ESA % Total Germany 19 6 Greece 1 0 General Observer 487 127 26.1% 38 29.9% Ireland 1 0 Snapshot 63 23 36.5% 1 4.3% Italy 21 4 Archival Research 132 44 33.3% Japan 1 0 AR Legacy 13 4 30.8% Korea 2 0 Theory 32 11 34.4% Russia 1 0 Total 727 209 28.7% 39 26.0% Spain 8 4 Sweden 4 2 Primary Switzerland 4 2 Orbits 14190 2948* 20.8% 536 18.2% The Netherlands 8 4 United Kingdom 26 10 *Does not include 11 calibration orbits USA 602 167 Venezuela 1 0 ESA Countries 112 40

Orbits by Science Category

Solar System 3%

Star Formation 5% AGN 3% Proposals by Science Category

Solar System 6.70% ISM 8% Hot Stars 4% Star Formation 6.70% Cosmology 29% AGN 9.09% Cool Stars 4%

Stellar Pops. 10% Cosmology 13.40% ISM 9.09%

Hot Stars 9.57% Galaxies 30% QAL 4%

Galaxies 26.32%

Cool Stars 5.74% Stellar Pops. 10.05% QAL: Quasar Absorption Lines ISM: Interstellar Medium QAL 3.35% AGN: Active Galactic Nuclei

 US Proposals by State

State Submitted Approved AL 6 0 AZ 57 16 CA 120 36 Instrument Statistics CO 21 6 CT 3 2 DC 15 6 DE 1 0 Instruments Mode Requested Orbits % Approved Orbits % FL 7 1 GA 6 2 ACS/HRC Imaging 1719 9.3% 423 HI 13 4 ACS/HRC Spectroscopy 325 1.8% 151 IL 9 2 ACS/SBC Imaging 221 1.2% 50 IN 4 1 ACS/SBC Spectroscopy 194 1.0% 23 69.2% KY 5 3 ACS/WFC Imaging 8702 47.0% 1823 LA 3 1 ACS/WFC Spectroscopy 204 1.1% 200 MA 46 14 FGS POS 423 2.3% 131 MD 104 29 FGS TRANS 43 0.2% 21 3.9% MI 20 6 NIC1 Imaging 534 2.9% 13 MN 4 1 NIC2 Imaging 1901 10.3% 167 19.1% MO 2 1 NIC3 Imaging 1458 7.9% 555 NH 2 0 NIC3 Spectroscopy 204 1.1% 20 NJ 8 3 WFPC2 Imaging 2603 14.0% 280 7.3% 1 NM 10 0 Total Orbits 18531 3857 NY 32 3 2 OH 8 3 Imaging 85.8% OK 2 1 Spectroscopy2 10.2% 2 OR 3 1 FGS 3.9% PA 35 11 RI 2 0 1 Includes Coordinated Parallels 2 SC 2 0 Excludes Pure Parallel and Snapshot programs TN 2 1 TX 18 6 VA 8 1 WA 12 4 WI 8 1 Proposal Acceptance Ratio WY 1 1

Oversubscription by Cycle 9.00 GO Proposal oversubscription 8.00 AR Funding oversubscription GO Orbit oversubscription 7.00

6.00

5.00

4.00

3.00

Oversubscription Ratio 2.00

1.00

0.00 1 2 3 4 5 6 7 7N 8 9 10 11 12 13 14 Cycle

 Name Institution Type Title

Large Programs

10 Thomas Ayres University of Colorado at Boulder AR StarCAT CYCLE 14: Approved Observing Programs Observing Approved 14: CYCLE

George Benedict University of Texas at Austin GO Astrometric Masses of Extrasolar Planets and Brown Dwarfs Carme Gallart Instituto de Astrofísica de Canarias GO The Onset of Star Formation in the Universe: Constraints from Nearby Isolated Dwarf Galaxies Chris Impey University of Arizona AR Legacy HST Spectroscopy of the Low Redshift Intergalactic Medium Shrinivas Kulkarni California Institute of Technology GO Gamma-Ray Bursts from Start to Finish: A Legacy Approach Douglas Leonard California Institute of Technology AR A Re-evaluation of the Cepheid Distance Scale from a Homogeneous Analysis of 22 Galaxies Observed with WFPC2 Philip Marshall Stanford University AR The HST Archive Galaxy-scale Gravitational Lens Search Keith Noll Space Telescope Science Institute SNAP Kuiper Belt Binaries: Probes of Early Solar System Evolution Saul Perlmutter University of California - Berkeley GO Decelerating and Dustfree: Efficient Dark Energy Studies with Supernovae and Clusters Massimo Stiavelli Space Telescope Science Institute GO Searching for Galaxies at z > 6.5 in the Hubble Ultra Deep Field David Turnshek University of Pittsburgh GO Neutral Gas at Redshift z = 0.5

Treasury Program

Sangeeta Malhotra Space Telescope Science Institute GO Probing Evolution And Reionization Spectroscopically (PEARS)

Extra-Galactic Programs

Eric Agol University of Washington GO A Cosmic String Lens Candidate Alessandra Aloisi Space Telescope Science Institute - ESA GO NGC 4449: a Testbed for Starbursts in the Low- and High-Redshift Universe Alessandra Aloisi Space Telescope Science Institute - ESA GO The Rosetta Stone without a Distance: Hunting for Cepheids in the "Primordial" Galaxy I Zw 18 Edward Baltz Stanford University GO Microlensing in M87 and the Virgo Cluster Robert Becker University of California - Davis AR HST Observations of MilliJansky Radio Sources from the VLA FIRST Survey Edo Berger Carnegie Institution of Washington AR Looks Matter: Tracing Galaxy Evolution Through the Morphologies of GRB Host Galaxies Edo Berger Carnegie Institution of Washington GO Gotcha! Using Swift GRBs to Pinpoint the Highest Redshift Galaxies Mariangela Bernardi University of Pennsylvania SNAP The Most Massive Galaxies in the Universe: Color-Gradients and Texture John Biretta Space Telescope Science Institute GO HST/Chandra Monitoring of a Dramatic Flare in the M87 Jet Adam Bolton Massachusetts Institute of Technology SNAP Measuring the Mass Dependence of Early-Type Galaxy Structure Michael Brotherton University of Wyoming SNAP The Host Galaxies of Post-Starburst Quasars Remi Cabanac Canada-France-Hawaii Telescope Corporation GO The Highest Redshift Einstein Ring: Probing a Dark Matter Halo at z = 1 and Galaxy Morphology at z = 3.8 Daniela Calzetti Space Telescope Science Institute GO Calibrating Star Formation: The Link between Feedback and Galaxy Evolution Michele Cantiello INAF, Osservatorio Astronomico di Teramo AR Measurements of Surface Brightness Fluctuations Gradients in Normal and Peculiar Early-type Galaxies Christopher Churchill New Mexico State University AR Morphologies and MgII/CIV Absorption in 85 Intermediate Redshifts Galaxies Andrew Connolly University of Pittsburgh AR Marked Correlation Functions and Understanding the Evolution of Galaxies Romeel Davé University of Arizona AR High-Redshift Galaxies in GOODS: Simulations vs. Observations Roelof de Jong Space Telescope Science Institute SNAP The Halo Shape and Metallicity of Massive Spiral Galaxies Arjun Dey National Optical Astronomy Observatories GO ACS Observations of the Galaxies in a Giant Ly-alpha Nebula at z ~ 2.7 Mike Disney University of Wales, College of Cardiff (UWCC) GO Validating a Dark Galaxy Megan Donahue Michigan State University SNAP A Snapshot Survey of a Complete Sample of X-ray Luminous Galaxy Clusters from Redshift 0.3 to 0.7 Renato Dupke University of Michigan AR A Search for the Missing Baryons in Nearby Cosmic Filaments II - Sources of Bias Simon Dye University of Wales, College of Cardiff (UWCC) GO Accurate Dark-matter Mass Profiles in Three Elliptical Galaxies As a Test of CDM Harald Ebeling University of Hawaii SNAP A Snapshot Survey of the Most Massive Clusters of Galaxies Erica Ellingson University of Colorado at Boulder AR On the Road to Coma: A "Longitudinal Study" of Galaxy Cluster Evolution Richard Ellis California Institute of Technology GO Characterizing the Sources Responsible for Cosmic Reionization Thomas Erben Universität Bonn, Inst für Astrophysik und Extraterrestris GO A Detailed Study of the Mass Properties for the Galaxy Cluster RX J1347-1145 Aaron Evans State University of New York at Stony Brook SNAP HST Optical Snapshot Survey of Intermediate-Redshift Ultraluminous Infrared Galaxies Name Institution Type Title

Aaron Evans State University of New York at Stony Brook GO An ACS Survey of a Complete Sample of Luminous Infrared Galaxies in the Local Universe Sandra Faber University of California - Santa Cruz AR The Stellar Mass Function of Disks and Bulges at z = 1 Andrew Fabian University of Cambridge GO The Filaments of NGC 1275 Gary Ferland University of Kentucky AR Numerical Simulations of Time-variable AGN Emission and Absorption Line Regions David Finley Eureka Scientific Inc. AR Absolute Spectrophotometric Calibration to 1% from the FUV through the near-IR Derek Fox California Institute of Technology GO Solving the Mystery of the Short-Hard Gamma-Ray Bursts Avishay Gal-Yam California Institute of Technology GO A Survey for Supernovae in Massive High-Redshift Clusters Robert Geller University of California - Santa Barbara AR Flares from Tidal Disruption of Stars by Galactic Supermassive Black Holes Markos Georganopoulos University of Maryland Baltimore County GO Probing the Jet Matter Content of Quasar PKS 0637-752 David Goldberg Drexel University AR Measuring Gravitational Flexion in ACS Clusters Rosa Gonzalez Delgado Instituto de Astrofísica de Andalucía (IAA) SNAP Near-UV Snapshot Survey of Low-Luminosity AGNs Paul Goudfrooij Space Telescope Science Institute GO The Formation of Spiral Spheroids and Their Globular Cluster Systems Sara Heap NASA Goddard Space Flight Center AR Constraining both the Star-Formation History and Metal-Enrichment History of Galaxies Luis Ho Carnegie Institution of Washington AR The Spectral Energy Distributions of Low-Luminosity AGNs Luis Ho Carnegie Institution of Washington GO AGNs with Intermediate-mass Black Holes: A Test of the Black Hole-Bulge Paradigm Programs Observing Approved 14: CYCLE Benne Holwerda Kapteyn Astronomical Institute AR An Dust Extinction Map of M51 from Counts of Distant Galaxies Benne Holwerda Kapteyn Astronomical Institute AR Tracing the Dust Extinction in M101 from Counts of Distant Galaxies Michael Hudson University of Waterloo AR Linking Galaxies and their Dark Matter Haloes with Gravitational Lensing Chris Impey University of Arizona AR The ACS Mosaic of M51 and the Intersection of Research and Education Helmut Jerjen Australian National University SNAP Securing the Faint-End Galaxy Luminosity Function with Surface Brightness Fluctuation Distances Charles Keeton Rutgers, the State University of New Jersey GO A Last Look at the First Gravitational Lens Charles Keeton Rutgers, the State University of New Jersey AR The Theory of Multiscale Gravitational Lensing Jeffrey Kenney Yale University GO Ram-Pressure Stripping and Dense-Cloud Ablation in the Virgo Spiral NGC 4402 Roy Kilgard Harvard-Smithsonian Center for Astrophysics AR A Comparative X-ray and Optical Study of M51 Makoto Kishimoto University of Edinburgh, Institute for Astronomy GO Hosts of Quasars with Opaque Partial Covering Markus Kissler-Patig European Southern Observatory - Germany GO The Nature of LSB Galaxies Revealed by their Globular Clusters Christopher Kochanek The Ohio State University Research Foundation GO The Cluster Lens SDSS 1004+4112: Constraining World Models with Its Multiply-Imaged Quasar and Galaxies Leon Koopmans Kapteyn Astronomical Institute GO Imaging the Mass Structure of Distant Lens Galaxies Hermine Landt Harvard-Smithsonian Center for Astrophysics AR The Geometry of Broad Emission Line Regions in AGN Tod Lauer National Optical Astronomy Observatories GO The Compact Disk of Blue Stars Orbiting the M31 Black Hole Karen Leighly University of Oklahoma Norman Campus AR Accurate Accelerations in AGN Outflows Yeong-Shang Loh University of Colorado at Boulder SNAP A Snapshot Survey of Brightest Cluster Galaxies and Strong Lensing to z = 0.9 Marcella Longhetti Osservatorio Astronomico di Brera, Milano GO Morphology of Massive Early-type Galaxies at z > 1.2: Constraining Galaxy-Formation Models Jennifer Lotz University of California - Santa Cruz AR A Multi-Wavelength Study of Galaxy Mergers out to z ~ 2 Paul Martini Harvard-Smithsonian Center for Astrophysics AR The Influence of Bars on the Centers of Galaxies Brian McNamara Ohio University GO The Nuclear Environment of the Galaxy Hosting the Largest Known Radio Outburst Simona Mei The Johns Hopkins University GO Witnessing Galaxy Transformation in Galaxy Groups at z > 1 Chris Mullis University of Michigan GO The Most Distant X-ray Cluster at z = 1.4: Morphologies, Color-magnitude Relation and Fundamental Plane Kai Noeske University of California - Santa Cruz GO Kinematics and Morphology of the Most Massive Field Disk Galaxies at z > 1 Goran Ostlin Stockholm University GO Lyman-alpha Morphology of Local Starburst Galaxies Anna Pasquali Eidgenössiche Technische Hochschule (ETH) GO The Fine Structure of Elliptical Galaxies in Voids Eric Peng Dominion Astrophysical Observatory GO The Unique Star Cluster System of M85 Bradley Peterson The Ohio State University Research Foundation GO Host Galaxies of Reverberation-Mapped AGNs

11 Joel Primack University of California - Santa Cruz AR Simulated HST Images of Merging Galaxies Including Star Formation and Dust

Jason Prochaska University of California - Santa Cruz AR The Low-Redshift IGM Enrichment History Gabriel Prochter University of California - Santa Cruz SNAP An ACS Imaging Survey of the Galaxies Hosting Strong Mg II Absorption Daniel Proga Princeton University AR AGN Outflows and Their Three-Dimensional Nature Adam Riess Space Telescope Science Institute GO Cepheid Calibrations of the Luminosity of Two Reliable Type Ia Supernovae and a Re-determination of the Hubble Constant Name Institution Type Title

Timothy Roberts University of Leicester GO ULX Counterparts: The Key to Finding Intermediate-mass Black holes Blair Savage University of Wisconsin - Madison AR Tracing Baryons in the Warm-Hot Intergalactic Medium with Broad Ly-alpha Absorption

12 Paul Schechter Massachusetts Institute of Technology GO Dark Matter and the Missing Images of CX2201-3201 CYCLE 14: Approved Observing Programs Observing Approved 14: CYCLE

Gary Schmidt University of Arizona GO Bipolar Scattering Structures in AGN James Schombert University of Oregon AR S0 Evolution from Archival HST Images Marc Seigar University of California - Irvine AR The Co-evolution of Spiral Structure and Mass Distribution in Disk Galaxies Alice Shapley University of California - Berkeley GO Imaging a Proto-cluster at z = 2.3: The Morphology-Density Relation at High Redshift Ray Sharples University of Durham GO Globular Cluster Systems of Elliptical Galaxies in Low Density Environments Gregory Sivakoff The University of Virginia GO Probing the Galaxy-wide Globular Cluster—Low Mass X-ray Binary Connection in Early-type Galaxies Evan Skillman University of Minnesota - Twin Cities GO Quantifying Star Formation and Feedback: The M81 Group Dwarf Galaxies William Sparks Space Telescope Science Institute SNAP Ultraviolet Snapshots of 3CR Radio Galaxies Chris Stubbs Harvard University GO Resolving the LMC Microlensing Puzzle: Where Are the Lensing Objects? Jason Surace California Institute of Technology GO ACS Imaging of a Unique Spitzer Field: Morphology of mid-IR Variable Sources Nial Tanvir University of Hertfordshire GO GRB Afterglows and Host Galaxies at Very High Redshifts David Thilker The Johns Hopkins University GO Probing the Star Formation Law in the Extreme Outer limits of M83, a Prototypical XUV-Disk Galaxy Kim-Vy Tran Eidgenössiche Technische Hochschule (ETH) GO Life Before the Fall: Morphological Evolution of Galaxies in Groups Prior to Cluster Assembly at z = 0.37 David Turnshek University of Pittsburgh AR Are Our Ideas About Quasar Absorption Lines Consistent with Galaxy Images? David Tytler University of California - San Diego AR High-resolution Simulations of the Low-Redshift Intergalactic Medium Claudia Urry Yale University AR Host Galaxy Morphologies and SEDs of High-Luminosity AGN William Vacca Universities Space Research Association GO Sizes, Shapes, and SEDs: Searching for Mass Segregation in the Super Star Clusters of Nearby Starburst Galaxies Marianne Vestergaard University of Arizona AR Accuracy of Quasar Black Hole Mass Estimates Michael West University of Hawaii GO Archaeology of Fossil Galaxy Groups Andreas Zezas Harvard-Smithsonian Center for Astrophysics GO The Link between X-ray Source and Stellar Populations in M81 Bodo Ziegler Universitäts-Sternwarte Göttingen GO Galaxy Transformation As Probed by Morphology and Velocity Fields of Distant Cluster Galaxies

Galactic Programs

Nicholas Abel University of Kentucky AR Physical Processes in Orion’s Veil: A High-Resolution UV-Absorption Study of the Line of Sight towards the Trapezium Eric Agol University of Washington AR Finding Terrestrial Planets with HST Scott Anderson University of Washington GO Timing Studies of the X-ray Binary Populations in Globular Clusters David Ardila The Johns Hopkins University GO A Search for Debris Disks in the Coeval Beta Pictoris Moving Group Luigi Bedin European Southern Observatory - Germany GO Exploring the Bottom End of the White Dwarf Cooling Sequence in the Galactic Open Cluster NGC 2158 George Benedict University of Texas at Austin GO Precise Distances to Nearby Planetary Nebulae—Finishing Up in Cycle 14 David Bennett University of Notre Dame GO Resolved Images of LMC Microlensing Events Observed by a Telescope at 2 AU from Earth Howard Bond Space Telescope Science Institute GO The Light Echoes around V838 Monocerotis: MHD in 3 Dimensions, Circumstellar Mapping, and Dust Physics Howard Bond Space Telescope Science Institute GO Dynamical Masses and Third Bodies in the Sirius System Herve Bouy Instituto de Astrofísica de Canarias GO Astrometric Monitoring of Binary L and T Dwarfs Alexander Brown University of Colorado at Boulder GO Imaging Extended UV H2 Emission Around T Tauri Stefan Cartledge Louisiana State University and A & M College AR Digging for Interstellar Rare Elements in Archival UV Spectra Rupali Chandar Space Telescope Science Institute GO Extending the Heritage: Clusters, Dust, and Star Formation in M51 Andrew Cole Kapteyn Astronomical Institute GO Star-Formation History of an Unmerged Fragment: the Leo A Dwarf Galaxy Sean Colgan NASA Ames Research Center GO Massive Star Formation and the Proper Motions of the OMC-1 Molecular Hydrogen Fingers Joseph Collins University of Colorado at Boulder AR Si III Absorption As a Sensitive Probe of the High-Velocity Cloud Population Gary Da Costa Australian National University GO The Star Formation Histories of Early-Type Dwarf Galaxies in Low-Density Environments: Clues from the Sculptor Group John Debes The Pennsylvania State University GO Confirming Planetary Candidates in the Stellar Graveyard with NICMOS Andrea Dieball University of Southampton GO A Deep UV Imaging Survey of the Globular Cluster M 30 Andrew Dolphin University of Arizona GO ACS Zero-Point Verification Andrew Dolphin University of Arizona GO ACS Photometric Calibration from Faint Standards Name Institution Type Title

Vikram Dwarkadas University of Chicago AR Probing the Circumstellar Environment and Shock Interaction in SN 1987A and Cas A Nancy Evans Harvard-Smithsonian Center for Astrophysics GO The Dynamical Mass of the Bright Cepheid Polaris Jay Farihi Gemini Observatory, Northern Operations GO Resolving Ultracool White-Dwarf Binaries Gary Ferland University of Kentucky AR Dynamical flows in PNe: Interpreting HST Images on a Physical Basis Francesco R. Ferraro Bologna University GO Blue Stragglers: A Key Stellar Population to Probe Internal Cluster Dynamics Edward Fitzpatrick Villanova University SNAP A SNAP Program to Obtain Complete Wavelength Coverage of Interstellar Extinction Silvia Galleti Osservatorio Astronomico di Bologna GO The Outermost Globular Cluster of M31 Andrea Ghez University of California - Los Angeles AR An HST/NICMOS Study of our Galaxy’s Central Supermassive Black Hole and its Environment Douglas Gies Georgia State University Research Foundation SNAP Binary Stars in Cyg OB2: Relics of Massive Star Formation in a Super-Star Cluster Patrick Godon Villanova University AR Combined HST-FUSE Far-Ultraviolet Spectral Study of Cataclysmic Variables Paul Goudfrooij Space Telescope Science Institute GO A Reference Database for Accurate Ages and Metallicities of Globular Clusters in the Magellanic Clouds Dimitrios Gouliermis Max-Planck-Institut für Astronomie, Heidelberg GO Star Formation in the LMC—The Complete IMF of a Stellar Association Suzanne Hawley University of Washington SNAP Characterizing the Near-UV Environment of M Dwarfs: Implications for Extrasolar Planetary Searches and Astrobiology Todd Henry Georgia State University Research Foundation GO Calibrating the Mass-Luminosity Relation at the End of the Main Sequence J. Hester Arizona State University GO Dynamics of the Polarization Structure of the Crab Nebula Programs Observing Approved 14: CYCLE Dean Hines Space Science Institute GO Imaging Scattered Light from Debris Disks Discovered by the Spitzer Space Telescope Around 20 Sun-like Stars Andres Jordan European Southern Observatory - Germany GO Resolving the Connection Between Globular Clusters and Low-Mass X-ray Binaries Paul Kalas University of California - Berkeley GO ACS Imaging of Fomalhaut: A Rosetta Stone for Debris Disks Sculpted by Planets Paul Kalas University of California - Berkeley GO Multi-color Imaging of two 1 Gyr-old Debris Disks within 20 pc of the Sun: Astrophysical Mirrors of Our Kuiper Belt David Kaplan Massachusetts Institute of Technology AR The Proper Motion and the Parallax of the Crab Pulsar Oleg Kargaltsev The Pennsylvania State University GO Ultraviolet Spectrum of the Binary Millisecond Pulsar J0437-4715 Oleg Kargaltsev The Pennsylvania State University GO Studying the Spectum of PSR B0656+14 Robert Kirshner Harvard University GO SAINTS—Supernova 1987A INTensive Survey Arunav Kundu Michigan State University GO A Deep H-band Probe of the Globular Cluster Mass Function Tod Lauer National Optical Astronomy Observatories GO Resolving M32’s Main Sequence: A Critical Test for Stellar Population Studies Claus Leitherer Space Telescope Science Institute AR Calibrating Post-Main-Sequence Evolution in the Upper HRD Knox Long Space Telescope Science Institute AR Winds of Cataclysmic Variables Kevin Luhman Harvard-Smithsonian Center for Astrophysics GO An Edge-on Disk around a Brown Dwarf? Peter Lundqvist Stockholm University GO The High Proper Motion of PSR B0540-69.3 Jesús Maíz-Apellániz Space Telescope Science Institute - ESA GO A Complete Multiplicity Survey of Galactic O2/O3/O3.5 Stars with ACS Mario Mateo University of Michigan SNAP Globular Clusters in the Direction of the Inner Galaxy Margaret Meixner Space Telescope Science Institute SNAP A Snapshot Survey of Post-AGB Objects and Proto-Planetary Nebulae Peter Milne University of Arizona GO The Very Late Phases of a Thermonuclear Supernova Antonella Nota Space Telescope Science Institute - ESA GO Charting the Sparkling Star Formation in NGC 346 C. O’Dell Vanderbilt University GO Determining the Lifetime of Planetary Nebula Knots from Observations of the Core of the Helix Nebula Sally Oey University of Michigan SNAP Are Field OB Stars Alone? Joana Oliveira University of Keele GO The IMF in NGC 6611: The Environmental Influence on the Formation of Low-Mass Stars and Brown Dwarfs Deborah Padgett Jet Propulsion Laboratory GO Multiwavelength Imaging of Edge-on Protoplanetary Disks: Quantifying the Growth of Circumstellar Dust Steven Pravdo Jet Propulsion Laboratory GO Imaging Astrometrically-Discovered Brown Dwarfs Thomas Puzia Space Telescope Science Institute GO Intermediate-Age Globular Clusters in M31 John Raymond Harvard-Smithsonian Center for Astrophysics GO Resolving the Non-radiative Shock in SN1006 Ignasi Ribas Institut d’Estudis Espacials de Catalunya GO Eclipsing Binaries in the Local Group: Calibration of the Zero-point of the Cosmic Distance Scale and Fundamental Properties of Stars in M31 Massimo Robberto Space Telescope Science Institute - ESA GO The Distance of the Orion Nebula Cluster

13 Edward Robinson University of Texas at Austin GO High Temperature Accretion Flows and Reprocessing in X-ray Binaries: The ADC Source 4U 1822-371

Raghvendra Sahai Jet Propulsion Laboratory SNAP What Are Stalled Preplanetary Nebulae? An ACS SNAPshot Survey Raghvendra Sahai Jet Propulsion Laboratory AR Corkscrew Structures and Precessing Jets Raghvendra Sahai Jet Propulsion Laboratory GO Caught in the Act with HST—Active Jet Sculpting in the Young Preplanetary Nebulae IRAS 22036+5306 Ata Sarajedini University of Florida GO The Formation History of the M81 Spheroid Name Institution Type Title

Ivo Saviane European Southern Observatory - Chile GO A Tip of the Red Giant Branch Distance to NGC 4038/39 (“The Antennae”) Glenn Schneider University of Arizona GO Near-IR Spectrophotometry of 2MASSWJ 1207334-393254B—An Extra-Solar Planetary Mass Companion to a Young Brown Dwarf

14 Paul Scowen Arizona State University AR Multiwavelength Analysis of the Star-Formation Process in M51 CYCLE 14: Approved Observing Programs Observing Approved 14: CYCLE

Janet Simpson NASA Ames Research Center GO Testing the Stellar Coalescence and Accretion Disk Theories of Massive Star Formation with NICMOS Stephen Smartt The Queen’s University of Belfast GO Detecting the Progenitors of Core-collapse Supernovae Tammy Smecker-Hane University of California - Irvine GO Resolving the Complex Star-Formation History of the Leo I Dwarf Spheroidal Galaxy Angela Speck University of Missouri - Columbia AR Evolution of Molecular Gas and the Origin of Cometary Knots in Planetary Nebulae Karl Stapelfeldt Jet Propulsion Laboratory GO Coronagraphic Imaging of Bright New Spitzer Debris Disks Ben Sugerman Space Telescope Science Institute GO Probing Circumstellar and Interstellar Dust with Scattered-Light Echoes Schuyler Van Dyk Jet Propulsion Laboratory AR The Local Environments of Supernovae Theodore von Hippel University of Texas at Austin SNAP White Dwarf Cooling Physics: Calibrating the Clock Alycia Weinberger Carnegie Institution of Washington GO Imaging Nearby Dusty Disks Daniel Welty University of Chicago AR An Archival Survey of Interstellar Abundances in the Magellanic Clouds Janos Zsargo University of Pittsburgh AR Treating the UV and X-ray Spectral Regions Self-Consistently: Developing an Enhanced Stellar Atmosphere Code David Zurek American Museum of Natural History AR NGC 6681: The Deepest Ultraviolet Observations of a Globular Cluster

Solar System Programs

Gilda Ballester University of Arizona AR Studies of Europa’s Plasma Interactions and Atmosphere with HST/STIS FUV Images Michael Brown California Institute of Technology GO Icy Planetoids of the Outer Solar System John Clarke Boston University GO ACS Imaging of the Uranus Aurora and Hydrogen Corona Jean-Claude Gérard Université de Liège GO Coordinated Observations of Saturn’s Auroral Dynamic Morphology and Cassini Plasma Measurements Denis Grodent Université de Liège GO High-resolution Imaging of Jupiter’s Diffuse Auroral Emissions Inside and Outside the Main Oval During Solar Minimum. William Grundy Lowell Observatory GO Orbits, Masses, and Densities of Three Transneptunian Binaries Daniel Hestroffer Observatoire de Paris GO Internal Structure and Figures of Binary Asteroids Matthew Holman Harvard-Smithsonian Center for Astrophysics AR Search for Companions to Known Asteroids Using Archived Images from ACS and WFPC2 Philippe Lamy Laboratoire d’Astronomie Spatiale GO A Multiwavelength Investigation of Comet 73P/SW3-C William Merline Southwest Research Institute SNAP Search for Binaries among Faint Jupiter Trojan Asteroids Kathy Rages SETI Institute SNAP Active Atmospheres on Uranus and Neptune Scott Sheppard Carnegie Institution of Washington GO A Search for Satellites around Kuiper Belt Objects Which Exhibit High Angular Momentum Faith Vilas NASA Johnson Space Center GO Probing Asteroid Families for Evidence of Ultraviolet Space-Weathering Effects Dr. Matt Mountain,

New Institute Director

att Mountain will become the Director of the Space Telescope Science Institute on September 1, 2005. M Matt is currently the Director of the Gemini Observatory, which is based in Hilo, Hawaii. The Observatory has a staff of approximately 190 and is responsible for the operation and development of the two 8-meter Gemini Telescopes on Mauna Kea, Hawaii, and Cerro Pachón in Chile. He is also the Telescope Scientist for NASA’s James Webb Space Telescope, a member of the Webb Science Working Group, and a Visiting Professor at the University of Oxford (UK). Matt’s background is in physics and astronomy. He received a Bachelor of Science degree in physics in 1978 and a Ph.D. in astronomy in 1983—both from the Imperial College of Science and Technology, London University— where he also held a Research Fellowship before joining the staff at the Royal Observatory in Edinburgh. During The Institute's new director, Matt Mountain. his seven years in Edinburgh, he worked on observations Image Credit: K. Pu’uohau-Pummill of star formation processes and instrumentation for (Gemini Observatory). infrared astronomy, which culminated in the successful commissioning of a new infrared spectrometer for the United Kingdom Infrared Telescope in Hawaii. In 1992, Matt became Project Scientist for the Gemini 8-meter Telescopes Project—then based in Tucson, Arizona—and went on to become Project Director in 1994. During his tenure as Project Director, he had direct responsibility for the construction and commissioning of the two Gemini telescopes, which were accomplished on schedule, within a fixed budget of $184 M. In 1998 he moved to the “big island” of Hawaii, with responsibility for the creation of the Gemini Observatory— formulating, implementing, and running the operations and development programs of the two telescopes. As part of the development program, he built up a world-renowned adaptive optics group, which has kept the Gemini telescopes at the forefront of observational infrared astronomy. His initiation of a partnership with the National Optical Astronomy Observatory (NOAO) resulted in the formation of the Association of Universities for Research in Astronomy’s (AURA’s) “New Initiatives Office,” which conducted a two-year study of the feasibility of ground-based 30-meter telescopes. The success of this study led to the inclusion of AURA in the Thirty Meter Telescope (TMT) project. Matt’s related responsibilities have included memberships on the review committee of the California Extremely Large Telescope and the TMT Board. Matt’s principle research interests have included star formation in galaxies (including our own), advanced infrared instrumentation, and the capabilities of advanced telescopes. He has published more than 100 research papers, articles, and reports. He is a fellow of the American Astronomical Society, the Royal Astronomical Society, and the American Association for the Advancement of Science; and a member of the International Society for Optical Engineering. In 2003 Matt was awarded the Gabriela Mistral Medal for excellence in education by the Chilean Ministry of Education (the first time this award has been made outside of Chile) for the Gemini StarTeachers education program. W

15 James Webb Space Telescope Status

M. Giavalisco, [email protected], & P. Stockman, [email protected]

he Webb project has been making steady progress in a number of important areas. Many subsystems successfully passed their preliminary or critical design reviews (PDR, CDR), clearing the way to detailed design studies and early construction work. The manufacturing of the primary mirror segments is progressing well and continues to meet its schedule goals. Unfortunately, the Webb Project has identified several areas where the Tdevelopment budget has increased to levels that exceeds the spending guidelines provided by NASA Headquarters (HQ). The Project, the Science Working Group (SWG), and a special HQ-chartered tiger team will re-examine the scientific priorities for the mission with the goal of reducing the remaining development costs and technical risks, while preserving important science goals. Webb Budget Woes In early April, the Webb Project received notice from Northrop Grumman Space Technologies (NGST, the prime contractor) that their expected costs had increased by approximately $300M. While NASA has not yet received NGST’s detailed proposal for the associated contract changes, it is known that these increases deal with changes in the launcher (from a U.S. vehicle to an Ariane 5) and the Integrated Science Instrument Module (ISIM) requirements, and with increased complexity in the testing program. The new NASA administrator, Dr. Mike Griffin, has recently forwarded his approval for the change to the Ariane 5 launcher to the State Department. The Project is also aware of $200M in additional liens due to increased ISIM and science- instrument costs, full-cost accounting at government centers, and mandatory funding reductions to support other NASA missions. As a result, the current NASA funding guidelines are not sufficient to meet the official 2011 launch date, necessitating at least a one-year launch slip and additional costs due to the delay. The total added costs—from the $500M increases, the launch slip, and additional NASA HQ reserves—amount to approximately $1.1B, which is needed between fiscal years FY’05 and FY’13. While some cost increases were to be expected in a program of Webb’s size and complexity and some have been covered in part by allocated reserves, the needed amount exceeds current reserves. The occurrence of this problem before mission PDR is a great concern to NASA, the SWG, and the international partners. In addition to studying these increases in more detail, NASA requested the Project to consider the cost savings involved in reducing the mission objectives to their original “floor”: a 4-m diameter mirror, no mid-infrared instrument, and a de-scoped near-infrared camera and spectrograph. The Project found that within the current architecture, such a mission would not significantly reduce the budget problem (changes cost money, too). The SWG reported to NASA HQ that such a minimum mission would lose more than half of its expected science breadth and NASA-roadmap objectives. As a result, NASA HQ is chartering a scientific “tiger team” to assist the Project and SWG in evaluating and prioritizing the science capabilities of the mission in the context of expected state of science and facilities in the 2012 timeframe. Matt Mountain (future Institute Director) and Peter Stockman will co-chair the tiger team. Alan Dressler (chair of the HST & Beyond Committee) and Chris McKee (NAS Decade Committee Co-Chair) have also agreed to serve. Other members include Roberto Abraham, Kathryn Flanagan, Bob Gehrz, Malcolm Longair, and Sara Seager. In June, the tiger team met by telecon to discuss the status of the Webb science program and receive briefings from the SWG and the Project. Their interim report (due July 8) is expected to strongly endorse the Webb science goals. However, the team noted that the likely construction in the next decade of giant ground-based telescopes with multi-conjugate adaptive optics would reduce the uniqueness of Webb capabilities at wavelengths below 1.6 microns. Thus, the report is expected to recommend relaxing or eliminating the requirements at wavelengths below 2 microns. Based on estimates provided by NASA, the resulting changes in the development and testing program would result in significant savings (> $300M) and reduce the risk of future cost increases. A Cryo-Cooler for the Mid-Infrared Instrument (MIRI) In March the Project approved an important design change for MIRI. The instrument will now have a cryo-cooler to reach and maintain the required operating temperature for the Si:As detectors, in place of the originally planned cryostat (dewar). The measure comes with a substantial reduction in the mass of the instrument, approximately 250 kg, which significantly reduces the overall Webb mass, both directly and through reducing the requirements on the supporting ISIM and telescope

16 backplane structures. However, the cryo-cooler increases the overall power demand by about 400 W, narrowing the power margin. Scientifically, the elimination of the cryostat is good news, because it may be possible to extend the operational life of MIRI from five years to ten. Successful CDRs and PDRs In January, the NASA Project passed the PDR for the ISIM structure. The ISIM team is now proceeding with the detailed design of the module. The University of Arizona and Lockheed Martin passed the CDR in March for the optical design of the Near Infrared Camera (NIRCam). This milestone clears the way to the building phase of the optical assembly of the instrument. The NIRCam team has received approval for purchasing the optics. (NIRCam is essential for the early testing of the Webb telescope optics, during integration and test.) Also in March, the European Consortium successfully passed the PDR of the MIRI optical bench assembly. The detailed design effort is now underway. In May, the Canadian Space Agency team passed the PDR for the Fine Guidance Sensors and the Tunable Filter Imager. Mirror segments delivered The Project passed a major milestone in March, when the last blank of the primary mirror segment was delivered to Axsys, where the blanks are being light-weighted and figured before delivery to Tinsley for polishing. The successful manufacture of the blanks is just the first step in the five-year process of delivering 18 cryo-figured segments to Webb for integration into the telescope assembly in 2009. Orbit study completed Mark Clampin (Goddard Space Flight Center) led an NGST/NASA/Institute team in studying the Webb launch options, with the goal of reducing scattered light from the Earth and Moon during the ten-year mission. The team recommended a plan that provided adequate launch opportunities during the year, while eliminating the possibility that moonlight could be reflected by the secondary mirror directly into the science instruments. W

The Webb Integrated Science Instrument Module Secondary Primary Mirror (SM) Mirror (PM) M. Greenhouse, Matt.Greenhouse@nasa.gov Integrated Science Instrument Module he James Webb Space Telescope is under (ISIM) development by NASA in partnership with the Optical Telescope European and Canadian Space Agencies, with Element (OTE) launch planned for 2011. The Webb observatory Tis designed to enable a five-year science mission, which is focused on four themes: (i) observation of the first luminous objects after the Big Bang, (ii) the assembly of these objects into galaxies, (iii) the birth of stars and planetary systems, and (iv) the formation of planets and Sunshield Spacecraft Bus the origins of life. Cold, Space-facing side Warm, Sun-facing side Enabling the Webb investigations poses unique engineering challenges, requiring high sensitivity and Figure 1: The Webb observatory consists of three separately integrated elements: the Hubble-like angular resolution from near- to mid-infrared. ISIM, the Optical Telescope Element (OTE), and the spacecraft. The cryogenic portion The observatory—with a 25 m2 collecting area and of the ISIM is located at the focus of the OTE and contains the science-instrument operating at ~40 K—includes the largest cryogenic payload of the observatory. telescope ever to be built. Simulating the flight-cryogenic environment to test the telescope before launch will require large and complex facilities. To make the testing more practical, NASA decided on a modular architecture for Webb, which permits an incremental approach to integration and testing. The Integrated Science Instrument Module (ISIM) is Continued one of three major elements of the observatory, each of which is designed page 18

17 for incremental testing and flight qualification, in Webb Science The Webb Mission at a Glance from page 17 parallel, prior to integration as a system. The ISIM, which contains a fine guidance sensor and ~70 million infrared detectors in four science Mission Objective instruments, is the science-instrument payload of Study the origin and evolution of galaxies, stars and planetary the Webb observatory. It also contains a passive systems. thermal-control system for the 40 K temperature Organization range, a cryo-cooler to achieve ~6 K for some • Mission Lead: Goddard Space Flight Center. detectors, computer systems for commanding • International collaboration with ESA & CSA. instruments and handling data, flight software • Prime Contractor: Northrop Grumman Space Technology. for the instruments, and an optical metering • Instruments: structure. The ISIM is responsible for acquiring s Near Infrared Camera (NIRCam) – Univ. of Arizona. science data, fine-guidance data for telescope- s Near Infrared Spectrograph (NIRSpec) – ESA. pointing control, and wavefront-sensing data for s Mid-Infrared Instrument (MIRI) – JPL/ESA. in-flight adjustment of the telescope optics. s Fine Guidance Sensor (FGS) – CSA. The ISIM project developed and demonstrated Description several new technologies to enable the science- • Deployable telescope w/ 6.5m diameter segmented adjustable

013 2014 2015 2016 2017 primary mirror. 2 instrument designs. These include: (i) 4-Mpixel, 0.6–5 micron, near-infrared sensor chip arrays • Cryogenic temperature telescope and instruments for infrared Science Operations and 16-Mpixel focal-plane array assemblies, performance. involving both HgCdTe and InSb detector • Optimized for infrared observations (0.6–28 mm). material (HgCdTe was selected for flight); (ii) • Launch in 2011 to Sun-Earth L2. Launch a cryogenic, application-specific, integrated • 5-year science mission (10-year goal). circuit providing complete front-end detector

st control and data conversion electronics; (iii) Te 1-Mpixel, 5–28 micron, mid-infrared Si:As sensor chip arrays; (iv) a 250-Kpixel Micro

n Electro-Mechanical system (MEMS) cryogenic micro-shutter array system for sparse-target, multi-object and Hadamard-transform integral- field spectroscopy; and (v) a facility-class Hadamard-transform spectrometer for the brication, Assembly and y National Optical Astronomy Observatory’s Confirmation for Fa da 4-m telescope at Kitt Peak, to prove the Mission Implementatio To applicability of this technique to Webb. The Design, instrument-development teams are developing these technologies to flight readiness. Figure 2: A pictorial representation of the JWST orbital The ISIM science instruments provide imagery position around the Lagrangian point L2 of the Sun-Earth with high angular resolution and spectroscopy system. Thanks to this location 1.5M km from the Earth, with medium spectral resolution from 0.6 to 28 the cold telescope is shielded by its sunshield from the microns. Further information on the science Sun, the Earth, and the Moon. capability of these instruments can be found at http://www.stsci.edu/jwst/docs/flyers/. Goddard Space Flight Center (GSFC) is responsible for developing the ISIM, with major systems provided by the University of Arizona, Lockheed Martin Advanced Technology Center, the Jet Propulsion Laboratory, the UK Astronomy Technology Center, EADS Astrium, EMS Technologies,

Concept Development Rockwell Scientific, Raytheon Vision Systems, and Alliant Techsystems.

1999 2000 2001 2002 2003 2004 2005 2006 2007 2008 2009 2010 2011 2012 The ISIM will be integrated at GSFC, and tested in the GSFC Space Environment Simulator Authorized using a cryogenic simulator of the observatory telescope. After flight qualification, the ISIM will

Mission Formulation be delivered to Northrop Grumman Space Technologies for integration with the telescope at the Johnson Space Center in 2009. W

18 Figure 3: The ISIM will be integrated with the OTE at Johnson Space Center (JSC); testing will occur in JSC Chamber A—one of the largest vacuum test chambers in the world (note the person shown on the work platform for scale). Helium- cooled shrouds (not shown) enclose the ISIM/OTE assembly and its surrounding test tower to simulate the thermal environment of the L2 orbit.

Figure 4: The ISIM cryogenic assembly, integrated with its four science-instrument sub-systems.

Figure 6: A flight-production MEMS micro-shutter wafer. The flight array Figure 5: Concept of the detector flight package for the assembly consists of four arrays of 171 × 365 pixels, with a pixel size of NIRCam, shown containing four HgCdTe sensor chip arrays 105 × 204 microns. Each shutter is individually addressed, magnetically (SCAs; produced by Rockwell Scientific), which are used actuated, and electrostatically latched. The micro-shutter system is by each ISIM near-infrared instrument. Each array contains designed for cryogenic operation at ~40 K, and is used to provide aperture 4 Mpixels. Data-conversion electronics are contained in control for the NIRSpec instrument. a cryogenic, application-specific, integrated circuit (not shown) located within a few cm of the SCAs to reduce susceptibility to electromagnetic interference.

Figure 8: The ISIM cryogenic assembly, integrated with the OTE Simulator (OSIM), in the GSFC Space Environment Simul- ator chamber. At this level of integration, the science instru- ment performance is verified with the ISIM structure and electronics systems prior to delivery of the ISIM for integra- tion with the OTE.

Figure 7: The micro-shutter array assembly flight package for the NIRSpec instrument.

19 The 2005 HST Calibration Workshop

P. Goudfrooij, [email protected]

he Institute will host a calibration workshop for the Hubble scientific instruments on October 26–28, 2005. The workshop will feature recent calibrations and advances in understanding data from five instruments: Advanced Camera for Surveys (ACS), Near Infrared Camera and Multi-Object Spectrometer (NICMOS), Space Telescope Imaging Spectrograph (STIS), Wide Field and Planetary Camera 2 (WFPC2), and Fine Guidance Sensor (FGS). Other topics to be covered are the calibration status for the TCosmic Origins Spectrograph (COS) and Wide Field Camera 3 (WFC3), cross-calibration efforts between Hubble, Spitzer, and Webb instruments, analysis of dithered, undersampled data, Hubble archive and Virtual Observatory enhancements, and calibration software developments, such as MultDrizzle, PyRAF, and the Space Telescope Science Data Analysis System (STSDAS). The workshop is intended to foster the sharing of information and techniques between observers, instrument support teams, and instrument developers. There will be oral and poster sessions and time for demonstrations and splinter-group meetings on topics of special interest. The proceedings of the meeting will be published in early 2006. Invited speakers include principal investigators and co-investigators of recent Hubble Treasury Programs and Calibration Outsourcing Programs, as well as instrument scientists at the Institute and the Space Telescope European Coordinating Facility in Germany. More information on the calibration workshop is available at http://www.stsci.edu/institute/ conference/cal05. Anyone interested in contributing oral or poster presentations can submit an abstract through the website; the abstract deadline is August 12, 2005. Online registration and payment processing for the workshop will also be available via a new, secure web interface; the registration deadline is September 16, 2005. W

Poster for the 2005 HST Calibration Workshop which will take place at STScI on October 26–28, 2005.

20 MAST News

R. Somerville, [email protected], for the MAST team

s of May 1, 2005, MAST contained about 24 Tbytes of data. In April 2005, we archived 17 Gbytes/day on average, and users retrieved an average of about 85 Gbytes/day; the median retrieval time from the Data Archive and Distribution System was around 2 hours, with on-the-fly-recalibration (OTFR) requests taking a median time of about 4 hours and non-OTFR requests taking about 0.25 hours. AGALEX News Early this year, MAST added imaging data from the first Galaxy Evolution Explorer (GALEX) data release. Grism data are now available as well. We have also implemented a version of the CASJobs tool created by workers at The Johns Hopkins University, which allows users to submit batch jobs to the GALEX database. GALEX data may be cross-correlated with the Sloan Digital Sky Survey via either a MAST SQL form or CASJob pages. Find out more at http://galex.stsci.edu/. Users can also now easily cross-correlate data from the GALEX mission with other MAST missions. GALEX is now included in the following MAST search forms: quick search (http:// archive.stsci.edu/), cross-correlation search (http://archive.stsci.edu/xcorr.php), and the Vizier search (http://archive.stsci.edu/vizier.php). Results can be output in several formats (e.g., ASCII, HTML, VOtable). The default search radius for GALEX is set to 6 arcmin. MAST Scrapbook News Many users are familiar with the MAST Scrapbook tool (http://archive.stsci.edu/scrapbook. php), which allows you to search multiple MAST missions for “representative” images or spectra by target name or coordinate. The Scrapbook tool is now available as a registered web service (see the MAST web services page at http://archive.stsci.edu/vo/mast_services.html for details). This development allows other data centers to access the MAST Scrapbook data through their own site. For example, users can now access the MAST Scrapbook through the OASIS tool from the NASA/IPAC Infrared Science Archive (IRSA) website (http://irsa.ipac.caltech.edu/data/ Scrapbook/). As a result of an IRSA-MAST interoperability project, users can now obtain 2MASS (Two Micron All Sky Survey) images for any object in the Scrapbook through either interface (MAST or IRSA). The 2MASS images (available in both jpg and FITS format) are 20 × 20 arcmin and are centered on the listed MAST target. GOODS Cutout Tool Available The Great Observatories Origins Deep Survey (GOODS) project imaged two 160-arcmin2 fields with the Advanced Camera for Surveys (ACS) on Hubble (http://www.stsci.edu/science/ goods/). For some time now, the reduced, mosaiced images have been publicly available at MAST in our High Level Science Products (HLSP) database (http://archive.stsci.edu/prepds/goods/). However, sometimes users are interested only in specific objects and do not want to have to download a large volume of data. MAST has now made available a “cutout tool,” which produces FITS and/or PostScript or PNG “postage stamps” in all four of the available bands (B, V, i, z), as well as three-color images. Users can specify coordinates or target names and a cutout size through a web form (http://archive.stsci.edu/eidol.php). The cutout tool is also a registered web service (http://nvo.stsci.edu/VORegistry). The service is based on the Eidol tool created by GOODS team member Dr. Leonidas Moustakas. At the moment, the cutout tool works only on GOODS data, but we plan to expand it in the future to work with other HLSPs. MAST Suggestion Box MAST welcomes comments and suggestions from our users about how we can improve or expand our services. We have created a new “suggestion box” web form, where users can submit suggestions (http://archive.stsci.edu/suggestions.html). We will archive the suggestions and our responses (with the submitter’s permission) on a public website.

Pipeline MultiDrizzle Image Orientation Changed The default orientation for pipeline MultiDrizzle ACS images (* _ drz.fits) has been changed to the unrotated image frame, instead of having north “up.” This leads to smaller images, which are easier to transfer and display, and which can still be readily oriented with a north-up orientation using most image display programs (such as ds9). More importantly, images delivered in the unrotated frame allow instrument-specific effects to be more Continued easily identified and accounted for, including: bad columns, stellar diffraction page 22

21 spikes, charge-transfer-efficiency (CTE) trails, and point-spread function effects. They are also MAST News from page 21 more useful for polarimetric, coronagraphic, and grism data. The ACS CTE correction formulae can also be more readily applied to unrotated images. If north-up images are still required, these can be generated by appropriately setting the “final _ rot” parameter when running MultiDrizzle off-line on the calibrated flt (flat-fielded) files delivered from the pipeline. The default orientation change was implemented March 25, 2005 at 12:50 p.m. EST. M51 High-Level Science Products now available In January 2005, the Hubble Heritage team obtained a large four-color mosaic image of the Whirlpool Galaxy NGC 5194 (M51) and its companion, NGC 5195, using Hubble’s ACS. See Hubble observing program 10452 (PI: Steven V. W. Beckwith) for more details. HLSPs (Drizzle-combined FITS files at a scale of 0.05 arcsec per pixel and with dimensions of 8600 × 12200 pixels) from this program are now available through MAST at URL http://archive.stsci.edu/prepds/m51/. New High-Level Science Products from the Archival Pure Parallel Program The Archival Pure Parallel Program has delivered a new set of HLSPs, which represents an update from v0.5 to 1.0 and also contains some new four-filter data. This is now the final delivery for the Large Magellanic Cloud, Small Magellanic Cloud, and nearby galaxies; nevertheless, we anticipate that we will receive additional pointings at a later stage. Find out more about the program and the data at http://archive.stsci.edu/prepds/appp/. Updated NICMOS Ultra Deep Field Data We have archived version-2 HLSPs from the Hubble Ultra Deep Field Treasury program using the Near Infrared Camera and Multi-Object Spectrometer (NICMOS). The extraction procedures are detailed in Thompson et al. 2005, AJ, in press (astro-ph/0503504). The data may be found at: ftp://archive.stsci.edu/pub/hlsp/udf/nicmos-treasury/version2/ or by ‘ftp’ing to archive. stsci.edu and then typing cd /pub/hlsp/udf/nicmos-treasury/version2. MAST Newsletter Catch up on MAST news for the past year by reading the MAST Newsletter at http://archive. stsci.edu/archive_news/archive_news_apr2005.html. You can subscribe to receive future editions of this electronic newsletter by sending an email to archive _ [email protected] with the single word ‘subscribe’ in the body of the message. W

Outburst from Comet Targeted By Deep Impact

n a dress rehearsal for the rendezvous between NASA’s Deep Impact spacecraft and comet 9P/ I Tempel 1, the Hubble Space Telescope captured dramatic images of a new jet of dust and gas streaming from the icy comet. The images are a reminder that Tempel 1’s icy nucleus, roughly half the size of Manhattan, is dynamic and volatile. Astronomers hope the eruption of dust seen in these observations is a preview of the fireworks that may come July 4, when a probe from the Deep Impact spacecraft slams into the comet, possibly blasting off material and giving rise to a similar plume of dust and gas.

http://hubblesite.org/newscenter/newsdesk/archive/releases/2005/16/ Credit: NASA, ESA, P. Feldman (The Johns Hopkins University) and H. Weaver (The Johns Hopkins University Applied Physics Laboratory)

22 Supernova Remnant N 63A Menagerie

violent and chaotic-looking mass of gas and dust is seen in this Hubble Space Telescope image of a nearby supernova remnant. Denoted N 63A, A the object is the remains of a massive star that exploded, spewing its gaseous layers out into an already turbulent region. The supernova remnant is a member of N 63, a star-forming region in the Large Magellanic Cloud (LMC). Visible from the southern hemisphere, the LMC is an irregular galaxy lying 160,000 light-years from our own Milky Way galaxy. The LMC provides excellent examples of active star formation and supernova remnants to be studied with Hubble.

http://hubblesite.org/newscenter/newsdesk/archive/releases/2005/15/ Credit: NASA, ESA, HEIC, and The Hubble Heritage Team (STScI/AURA)

Contact STScI:

The Institute’s website is: http://www.stsci.edu Assistance is available at [email protected] or 800-544-8125. International callers can use 1-410-338-1082. For current Hubble users, program information is available at: http://presto.stsci.edu/public/propinfo.html. ST-ECF The current members of the Space Telescope Users Committee (STUC) are: Martin Elvis (chair), Harvard-Smithsonian CfA, [email protected] Newsletter he Space Telescope–European Coordinating Facility David Axon, RIT C. Robert O’Dell, U. Vanderbilt publishes a newsletter which, although aimed principally Martin Barstow, U. of Leicester Regina Schulte-Ladbeck, U. Pittsburgh at European Space Telescope users, contains articles of Eric Emsellem, CRAL Monica Tosi, OAB general interest to the HST community. If you wish to be included in the mailing list, please contact the editor Laura Ferrarese, NRC-CNRC Donald G. York, U. Chicago Tand state your affiliation and specific involvement in the Space Pat McCarthy, OCIW Telescope Project.

The Space Telescope Science Institute Newsletter is edited by Robert Brown, Richard Hook (Editor) [email protected], who invites comments and suggestions. Space Telescope–European Coordinating Facility Technical Lead: Christian Lallo, [email protected] Karl Schwarzschild Str. 2 Contents Manager: Sharon Toolan, [email protected] D-85748 Garching bei München Design: Krista Wildt, [email protected] Germany To record a change of address or to request receipt of the Newsletter, E-Mail: [email protected] please send a message to [email protected].

23 Contents: Calendar Cycle 14 Cycle 14 Cycle 14 TAC Results ...... 5 Cycle 14: TAC and Panel Members ...... 7 Webb Quarterly Review in Victoria, B.C...... 19–21 July 2005 Cycle 14: Statistics ...... 8 Cycle 14 EPO proposal deadline ...... 19 August 2005 Cycle 14: Approved Observing Programs ...... 10 Beginning of Matt Mountain’s term as Director ...... 1 September 2005 Start of 2-gryo operations on Hubble ...... 22 August 2005 AURA Board meeting in Hilo, Hawaii ...... 7–9 September 2005 Institute News Webb SWG meeting at the Institute ...... 21–22 September 2005 IDEAS proposal deadline ...... 21 October 2005 Hubble’s 15th Anniversary ...... 1 Director’s Perspective ...... 2 Caroline Herschel Distinguished Lectures at the Institute, 3:30 pm New Institute Director ...... 15 Stellar Populations and the Evolution of Galaxies Webb Status ...... 16 Monica Tosi ...... 10 August 2005 The Webb Integrated Science Instrument Module ...... 17 Chemical Evolution of Galaxies: Constraints on Galaxy Formation Mechanisms 2005 HST Calibration Workshop ...... 20 Francesca Matteucci ...... 31 August 2005 MAST News ...... 21 Clumpy High Redshift Galaxies in the Hubble Ultra Deep Field Debra Meloy Elmegreen ...... 5 October 2005

Contact STScI ...... 23 Calendar ...... 24

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