VOL
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20
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ISSUE
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03
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The Cycle 12 Proposal
Peer Review
Credit: NASA, NOAO, ESA, the Hubble Helix Nebula Team, M. Meixner
(STScI), and T.A. Rector (NRAO). See page 6 for more information.
S p a c e Te l e s c o p e S c i e n c e I n s t i t u t e
2003
W
The oversubscription of Hubble observing time and data-reduction
funds remains high. Evaluating such a large number of proposals has
led to some distinctive procedures followed by the panels in identify
the best proposals. We expect these procedures to apply to future
proposal cycles, as follows.
Two-tiered TAC. In consultation with the Space Telescope Institute
Council, the Director sets aside one third of the available observing
time (~1,000 orbits) for large (over 100 orbits) and Hubble Treasury
proposals, which the TAC evaluates. The remaining two thirds of
observing time is devoted to smaller programs, which are evaluated
exclusively by the individual disciplinary panels. The relevant
disciplinary panels review the large and Treasury proposals, but the
multi-disciplinary TAC performs the final assessment.
Twin panels. Except for the solar system panel, each disciplinary
panel has one or two ‘mirror’ panels that consider those proposals for
which its own members may have some conflict of interest. This
procedure minimizes loss of expertise in the discussion due to panelists
recusing themselves from the evaluations. In Cycle 12, the acceptance rate
for proposals with panelist PIs was the same as that for non-panelist PIs.
Progressive orbit subsidy. In order to encourage
panels to resist a tendency to favor smaller
Continued
page 3
programs because of the greater number of
them that can be approved given the limited
ith the continuing excellent performance of the major
instruments on Hubble, the science program of the
telescope during Cycle 11 has been very productive. At the
same time there is some uncertainty over the timing of the
next servicing mission, which will install the new Cosmic Origins
Spectrograph and Wide Field Camera 3. Cycle 12 observations will begin in
July 2003 on an accelerated timeline in which the Institute has shortened
the period between proposal submission and observations by four months.
The Institute received 1,046 proposals in late January 2003 in response to
the Cycle 12 Call for Proposals. This represents an oversubscription in
requested orbits by more than 6 to 1, down slightly from the 1,075
proposals received in Cycle 11. The full Time Allocation Committee (TAC) and
11 disciplinary panels met in Baltimore in late March to evaluate the
proposals and to recommend programs to the Director for implementation.
As reported in the fall 2002 Newsletter, an external review of the Institute’s
TAC process was conducted last summer, which affirmed the basic integrity
and effectiveness of the Hubble peer review, but which recommended
certain changes in Cycle 12. (See http://www.stsci.edu/resources/
tac_assessment.) Among these changes were a loosening of institutional
conflict-of-interest rules governing panelists’ review of proposals, the
dissemination of reviewer comments to Principal Investigators (PIs) that
reflect the panel discussions, and convening an annual workshop to
facilitate broad collaboration on Hubble Treasury proposals.

Ongoing Features of the Hubble Peer Review
SUMMER
Overview

Duccio Macchetto, macchetto@stsci.edu, Robert Williams, wms@stsci.edu, & Brett Blacker, blacker@stsci.edu
DIRECTOR’S PERSPECTIVE
STARS IN ASTRONOMY
Steven Beckwith, svwb@stsci.edu
he other day a friend of mine remarked casually, “It seems that all stellar
astronomers over the age of 50 have gotten cranky.” We had noticed a certain defensiveness
in one of our colleagues who thought his interests had been marginalized among more fashionable
topics often featured in the popular press. Stellar astronomy dominated the study of the universe for
most of the last 400 years, and astronomers who work on stars are following a rich tradition. But a lot of
us got the feeling that stars are well understood and have moved on to more exotic pursuits, leaving the stellar
astronomers to rethink that rich tradition.
“Stellar” brings to mind “the best and brightest,” and when I talk
about astronomers who work on “stars,” visions of Hollywood and all
its glamour come to mind. Indeed, the importance of stars as a subject
for human inquiry is embedded in the language whenever we want to
describe individual achievement that stands above all the rest. So why
are these “stellar astronomers” cranky?
It cannot be because of any lack of success with the Hubble Space
Telescope. The Cycle 12 TAC rated a stellar proposal, Fritz Benedict’s
(#9879) as its highest priority this year among nearly 1100
competitors. Benedict’s team will measure the distances to Cepheid
variables by direct parallax using the Fine Guidance Sensor (FGS1R) on
Hubble; Howard Bond won time for a similar, albeit smaller program to
recalibrate the Cepheid zero point luminosity-period (L-p) relationship
following precise measurements of the distances to these important stars.
Hubble is now the most precise instrument in history for measuring
the positions of stars, achieving an accuracy of 0.2 milliseconds of
arc (mas), about five times better than Hipparcos, the previous
state-of-the-art. At that precision, several fundamental problems in
astronomy come into reach for the first time. For example, the l
argest uncertainty in the distance scale of the universe, expressed
through H0, is the zero point calibration of the L-p relation, which
Benedict and Bond can improve by a factor of a few to reduce the
error in our knowedge of H0—and thus the age of the universe.

2
Bond is using similar techniques to improve our knowledge of binary
star masses as a check on stellar evolution theory. There has been a
problem with some binary star systems whose components appear to
have much different ages from one another when calculated by our
standard theory, whereas we expect them to be coeval. Initial
observations of Procyon revised the derived masses of the two stars in
this binary system downward and brought the observations into
agreement with theory for the first time. Bond’s team is continuing with
observations of several other binary systems. Stellar evolution theory is
one of the most important advances of 20th century astrophysics, and
its verification remains an essential underpinning for our field.
ER 8 is the coolest known white dwarf in the Galaxy and hence the
oldest. It is nearby and moving rapidly, and by chance it will pass
within 50 mas of a background star in 2006 causing an apparent shift
in the center of light by more than 8 mas owing to gravitational lensing
of the star by the white dwarf. This shift is easily detectable with
FGS1R, allowing Kailash Sahu and his collaborators to measure the
mass of ER 8 to better than 5%. Knowing the mass of this cool white
dwarf will allow them to set the best lower limit to the age of the
Galaxy yet and, by extrapolation, to the universe itself. This measure of
universal age is completely independent of the standard methods of
cosmology and has the potential to either confirm or deny our standard
model for the universe. This is not the sort of impact we expect from a
DIRECTOR’S PERSPECTIVE
device whose main goal is to keep a spacecraft pointed in the right
direction, but then Hubble continues to show its superlative
capabilities in unlikely areas.
Sumner Starrfield and colleagues recently had their image of the
peculiar nova V838 Mon on the cover of Nature, an image so
spectacular that it could displace the Eagle Nebula as Hubble’s most
iconic image in the public’s mind. We already have T-shirts with V838
Mon that are quite popular among the T-shirt wearing crowd. (I am
thinking of getting a tie with that image or maybe another hat.)
The Fine Guidance Sensors don’t get much respect these days, but
they are quietly providing opportunities to rewrite the textbooks.
FGS1R, installed during servicing mission 3a, has improved the
state-of-the-art to such a degree that it opened up a number of new
research areas, just as all of Hubble’s new instruments have. The Cycle
12 TAC recommended programs using the FGS for 5% of the total
orbits at the same time that WFPC2—the venerable camera that is
responsible for 90% of the public and more than 50% of the scientific
impact of Hubble—received only 2% of the time. This change once
again show how servicing Hubble has expanded the range of its
scientific capabilities: FGS1R improved the state-of-the-art for
astrometric precision by as much as the Advanced Camera for Surveys
improved imaging. Servicing Hubble gives us a lot of bang for the buck,
and since it takes a lot of bucks to do it, we are pleased to get a
correspondingly big bang.
Our stellar astronomers have been flying stealthily below our radar
screens to pick off some of the most important problems in astronomy
with Hubble’s unmatched accuracy. The TAC noticed, I noticed, and
pretty soon, someone in the science media will notice that a field
thought by its own practitioners to be less than fashionable is actually
cutting a wide swath through new territory and giving the more
glamorous folks a run for their money.
So, if you are a stellar astronomer who is feeling cranky, you may want
to take heart in the new opportunities offered by Hubble. It is going to
help you rewrite the textbooks as it has with so many other fields.
I, for one, will be cheering you on. Ω
Cycle 12 Review from page 1
observing time, the Institute subsidizes the cost in orbits charged to the panel for moderate
proposals (15-100 orbits). For each orbit approved above 15, an increasing fraction is charged
against a pool of orbits held in reserve for the purpose. This policy has succeeded in increasing
the fraction of moderate programs over the past 5 cycles.
Reviewer comments. Panel feedback with information on the panel’s discussion and
assessment of a proposal is highly desired by most PIs—if not always valued! Each proposal is
assigned a primary reviewer, who is responsible for writing his/her own review and for incorporating
comments from the other secondary reviewers. The primary reviewer leads the panel
discussion and edits the written comments to reflect the panel discussion. Then others—the
secondary reviewers, the panel support scientist (an Institute scientist), and the panel chair—
review the comments before they are sent to the PI.
Also Notable in the Cycle 12 Peer Review
Cycle 12 continued the collaboration between the Institute, the National Optical Astronomy
Observatories, and the Chandra X-ray Center on the peer review of proposals requesting
resources on the Hubble and either Chandra or NOAO telescopes. The Hubble peer review can
approve observing time on the above facilities it deems necessary for the science objectives of
the Hubble proposal. The maximum total time that can be approved in this manner is 400 ksec
on Chandra and 20 nights on NOAO telescopes. For Cycle 12, the TAC and panels recommended
approval of 115 ksec on Chandra and 17.5 nights on NOAO telescopes.
Proposers used the Astronomer’s Proposal Tool (APT) for Phase I and
Continued
Phase II submission for the first time in Cycle 12. APT enables PIs to write
page 4
their proposals in a variety of text editors on different platforms and

3
Cycle 12 Review
from page 3
submit them in a way that results in a uniform format for all proposals. This feature was
essential to our being able to shorten the time between proposal submission and scheduling
observations. While we have experienced some glitches typical of the first-time use of a large
software package, the Institute is committed to correcting the flaws and making APT as user
friendly as possible. Specific comments on APT are welcomed and should be sent to
apt-phase1@stsci.edu.
Advice to Future Proposers
The present Hubble review process is highly regarded and widely copied. We plan to use the
same process in future cycles, which means future proposers should keep in mind the following
advice drawn from experience.
The scientific case should be of broad interest to your fellow astronomers. The most
successful proposals describe the importance of the investigation to all astronomy in a
convincing manner and include sufficient background information to provide a compelling
context. Do not write proposals that are of interest to only a few experts in a narrow subdiscipline.
Instead, present the big picture. This is an explicit evaluation criterion, and proposals are
downgraded for failing to address it.
Ask only for the resources you genuinely need. Justify your request for the number of targets
and orbits and the need for Hubble observations. For example, even if you request observations
in the ultraviolet, it may not be obvious to the reviewers why you cannot achieve the science
aims of your proposal in a different wavelength range. In the infrared, justify your need for
Hubble and NICMOS by comparison with adaptive optics systems on ground-based telescopes.
Because of the limited number of orbits available in a cycle, many truly excellent proposals
must be turned down. Nevertheless, remember that rejected PIs are in very good company and
that many of these proposals succeed in future cycles.
Final Thoughts
There is no ideal process for evaluation of proposals, and the Institute remains open to new
procedures that will improve our evaluation process. We are constantly assessing our
procedures in response to suggestions from the Users Committee and the community. We
augment or modify some aspects of our procedures every succeeding cycle. The Cycle 12 TAC
made many hard decisions, which have produced the Cycle 12 science program for the Hubble.
We express our appreciation to the panelists and TAC members who participated in the recent
TAC process, with special thanks to Dr. Tim de Zeeuw for serving as TAC Chair for this cycle. In
the accompanying tables, we list the panel and TAC members and the programs that have been
approved by the Director to receive observing time and/or data reduction and archival research
funds in Cycle 12. Ω

4
Cycle 12: TAC and Panel Members
Member
Institution
TAC Chair
Tim de Zeeuw
Sterrewacht Leiden
Phil Massey
David Meyer
Georges Meynet
Mark Morris
Antonella Natta (Chair)
Marc Pinsonneault
James Pringle
Tad Pryor
John Raymond
Bo Reipurth
Bradley Schaefer
Regina Schulte-Ladbeck (Chair)
Michal Simon
Ed Sion
Stephen Smartt
Tammy Smecker-Hane
Verne Smith
Alexander Tielens
Todd Tripp
William van Altena
Ted von Hippel
Don Winget
Hans Zinnecker
Ellen Zweibel
Eric Agol
Matthias Bartelmann
Ralf Bender (Chair)
Lowell Observatory
New Mexico State University
Universite de Liege
California Institute of Technology
University of Arizona
University of Hawaii
The Johns Hopkins University Applied Physics
Laboratory
Galactic Panel Members
Charles Bailyn (Chair)
Bruce Balick
Thomas Bania
David Bennett
David Charbonneau
Roger Chevalier
You-Hau Chu (Chair)
Robin Ciardullo
Constantine Deliyannis
Andrew Dolphin
Bruce Elmegreen (Chair)
Rob Fesen
Ed Fitzpatrick
Jules Halpern
Mario Hamuy
Pat Hartigan
Thomas Henning
Pascale Jablonka
Joachim Krautter
Richard Larson
Jeff Linsky
Peter Martin
Institution
Extragalactic Panel Members
Solar System Panel Members
Marc Buie
Nancy Chanover
Jean-Claude Gerard
Amanda Hendrix
Ralph Lorenz
Karen Meech (Chair)
Hal Weaver
Member
Katherine Blundell
Tereasa Brainerd
Elias Brinks
Michael Brotherton
Gerald Cecil
Renyue Cen
Stephane Charlot
Giuseppina Fabbiano (Chair)
Heino Falcke
Yale University
University of Washington
Boston University
University of Notre Dame
California Institute of Technology
University of Virginia
University of Illinois at Urbana - Champaign
The Pennsylvania State University
Indiana University System
National Optical Astronomy Observatories
IBM T.J. Watson Research Center
Dartmouth College
Villanova University
Columbia University
Carnegie Institution of Washington
Rice University
Max-Planck-Institut fur Astronomie, Heidelberg
CNRS, Institute d'Astrophysique de Paris
Landessternwarte Heidelberg
Yale University
University of Colorado at Boulder
University of Toronto / Canadian Institute for
Theoretical Astrophysics
Lowell Observatory
Northwestern University
Geneva Observatory
University of California - Los Angeles
Osservatorio Astrofisico di Arcetri
Ohio State University
Cambridge University
Rutgers the State University of New Jersey
Smithsonian Institution Astrophysical Observatory
University of Hawaii
University of Texas at Austin
University of Pittsburgh
State University of New York at Stony Brook
Villanova University
Cambridge University
University of California - Irvine
University of Texas at El Paso
Kapteyn Astronomical Institute
Princeton University
Yale University
University of Texas
University of Texas at Austin
Astrophysikalisches Institut Potsdam
University of Wisconsin
Xiaohui Fan
Karl Glazebrook
Anthony Gonzalez
Richard Green (Chair)
Henk Hoekstra
Deidre Hunter
William Keel
Jean-Paul Kneib
Ken Lanzetta
Simon Lilly (Chair)
Lynn Matthews
Patrick McCarthy (Chair)
David Merritt
Gerhardt Meurer
Rafaella Morganti
John Mulchaey
Reynier Peletier
Rosalba Perna
Patrick Petitjean
Richard Pogge
Joel Primack
Michael Rauch
Susan Ridgway
Abhijit Saha
David Sanders
Ian Smail
Thaisa Storchi-Bergmann
Michele Thornley
William van Breugel
Liliya Williams
Rogier Windhorst
Donald York
Steve Zepf
California Institute of Technology / University of
Washington
Max-Planck-Institut fur Astrophysik
Universitats-Sternwarte Munchen / Max-PlanckInstitut fur extraterrestrische Physik
University of Oxford
Boston University
Universidad de Guanajuato
University of Wyoming
University of North Carolina at Chapel Hill
Princeton University
Max-Planck-Institut fur Astrophysik / CNRS, Institute
d'Astrophysique de Paris
Smithsonian Institution Astrophysical Observatory
Max-Planck-Institut fur Radioastronomie/University
of Nijmegen
University of Arizona
The Johns Hopkins University
University of Florida
National Optical Astronomy Observatories
University of Toronto / Canadian Institute for
Theoretical Astrophysics
Lowell Observatory
University of Alabama
Observatoire Midi-Pyrynees / California Institute of
Technology
State University of New York at Stony Brook
ETH Zurich
Smithsonian Institution Astrophysical Observatory
Carnegie Institution of Washington
Rutgers the State University of New Jersey
The Johns Hopkins University
Stichting Astronomisch Onderzoek in Nederland
(ASTRON)
Carnegie Institution of Washington
University of Nottingham
Smithsonian Institution Astrophysical Observatory
CNRS, Institute d'Astrophysique de Paris
Ohio State University
University of California - Santa Cruz
Carnegie Institution of Washington
The Johns Hopkins University
National Optical Astronomy Observatories
University of Hawaii
University of Durham
Universidade Federal do Rio Grande do Sul
Bucknell University
Lawrence Livermore National Laboratory
University of Minnesota
Arizona State University
University of Chicago
Michigan State University

5
Proposals By Country
Summary of Cycle 12 Results
Country
Proposals
Submitted
Approved
11
2
4
2
13
3
26
32
2
2
5
22
3
1
1
1
11
4
4
9
1
60
827
190
3
0
0
0
3
0
3
8
0
0
1
4
0
0
0
1
2
0
0
4
0
9
203
32
Australia
Austria
Belgium
Brazil
Canada
Chile
France
Germany
India
Ireland
Israel
Italy
Japan
Mexico
Norway
Russia
Spain
Sweden
Switzerland
The Netherlands
Ukraine
United Kingdom
United States
ESA Countries
General Observer
Snapshot
Archival Research
Theory
Total
Primary Orbits
Requested Approved % Accepted ESA Accepted ESA % Total
819
74
111
42
1046
19674
170
21
41
10
242
3154
20.8%
28.4%
36.9%
23.8%
23.1%
16.0%
28
4
16.5%
19.0%
32
323
16.8%
10.2%
Proposal Acceptance Ratio
The Helix Nebula Detail
T
his cropped version of the Helix Nebula mosaic shows cometary-filaments embedded along a portion of the
inner rim of the nebula's red and blue gas ring. At a distance of 650 light-years, the Helix is one of the
nearest planetary nebulae to Earth. The composite picture is a seamless blend of ultra-sharp NASA Hubble
Space Telescope (HST) Advanced Camera for Surveys images combined with the wide view of the Mosaic
Camera on the National Science Foundation's 0.9-meter telescope at Kitt Peak National Observatory, part of the
National Optical Astronomy Observatory, near Tucson, Arizona Astronomers at the Space Telescope Science Institute
(STScI) assembled the images into a mosaic. The mosaic was blended with a wider photograph taken by the Mosaic
Camera.
Credits: NASA and The Hubble Heritage Team (STScI/AURA)
Acknowledgment: Bo Reipurth (University of Hawaii)

6
US Proposals By State
Instrument Statistics
Instruments Requested Orbits
ACS/HRC
ACS/SBC
ACS/WFC
%
1914
266
11727
7.4%
1.0%
45.3%
FGS
578
2.2%
NIC1
NIC2
NIC3
427
1866
1471
1.6%
7.2%
5.7%
STIS/CCD
STIS/FUV
STIS/NUV
1475
2743
1516
WFPC2
1919
Total
25902
Approved Orbits
State
%
53.7%
251
19
2640
4.7%
0.4%
49.7%
2.2%
268
5.0%
14.5%
183
597
342
3.4%
11.2%
6.4%
5.7%
10.6%
5.9%
27.8%
333
433
126
6.3%
8.1%
2.4%
7.4%
7.4%
123
2.3%
100.0%
5315
100.0%
AL
AZ
CA
CO
CT
DC
DE
FL
GA
HI
IA
IL
IN
KY
LA
MA
MD
MI
MN
MO
NC
NE
NH
NJ
NM
NY
OH
OK
OR
PA
SC
TN
TX
VA
WA
WI
WV
WY
SubTotal
54.8%
5.0%
21.1%
23.2%
2.3%
Orbits include coordinated parallel usage
Excludes Pure Parallel and Snapshot Programs
Proposal and Orbit Results By Science
Submitted
Approved
7
70
135
41
10
11
9
11
10
21
1
18
8
4
3
46
155
21
5
5
1
1
3
13
14
37
11
4
5
53
4
11
30
13
14
18
1
3
0
18
39
13
6
1
3
4
2
5
0
4
2
2
1
11
38
6
0
0
0
1
1
5
3
6
4
1
2
6
1
2
8
3
1
4
0
1
Cosmology 31%
QAL 3%
Cool Stars 5%
Star Formation 6%
Galaxies 19%
Stellar Pops 11%
Hot Stars 6%
Solar Systems 3%
ISM 9%
AGN 7%

7
Institution
Roberto Abraham
Omar Almaini
David Axon
Jack Baldwin
Aaron Barth
Philip Best
John Biretta
Michael Blanton
Torsten Boeker
Gregory Bothun
David Bowen
Michael Brotherton
Scott Burles
Scott Burles
Rupali Chandar
Rupali Chandar
Scott Chapman
Andrew Connolly
Steven Crawford
Roelof de Jong
Renato Dupke
Harald Ebeling
Richard Ellis
Richard Ellis
Eric Emsellem
Gary Ferland
Laura Ferrarese
Duncan Forbes
Marijn Franx
Jeffrey Gardner
Peter Garnavich
C. Gaskell
Karl Gebhardt
Alister Graham
Lincoln Greenhill
Timothy Heckman
University of Toronto
Royal Observatory Edinburgh
Rochester Institute of Technology
Michigan State University
California Institute of Technology
University of Edinburgh, Institute for Astronomy
Space Telescope Science Institute
New York University
Space Telescope Science Institute
University of Oregon
Princeton University
University of Wyoming
Massachusetts Institute of Technology
Massachusetts Institute of Technology
Space Telescope Science Institute
Space Telescope Science Institute
California Institute of Technology
University of Pittsburgh
University of Wisconsin - Madison
Space Telescope Science Institute
University of Michigan
University of Hawaii
California Institute of Technology
California Institute of Technology
Centre de Recherche Astronomique de Lyon
University of Kentucky
Rutgers the State University of New Jersey
Swinburne University of Technology
Universiteit Leiden
University of Pittsburgh
University of Notre Dame
University of Nebraska - Lincoln
University of Texas at Austin
University of Florida
Smithsonian Institution Astrophysical Observatory
The Johns Hopkins University
Extragalactic Programs
Name
GO
GO
GO
GO
GO
GO
GO
AR
GO
GO
GO
AR
AR
GO
GO
GO
GO
AR
AR
SNAP
GO
GO
AR
GO
GO
AR
GO
GO
GO
AR
GO
AR
GO
AR
GO
AR
Type
ACS Imaging of the Gemini Deep Deep Survey Fields: Galaxy Assembly at z = 1.5
A morphological study of EROs and sub-mm sources in a unique deep field
Measuring Black Hole Masses in Double Peaked Broad Lined AGNs
Probing the High Redshift Universe with Quasar Emission Lines
Calibrating the Black Hole Mass Scale for Quasars
Elliptical galaxies in z~1.5 clusters
HST / Chandra Monitoring of a Dramatic Flare in the M87 Jet
Comparing the ACS Ultra Deep Field to Low Redshift Galaxy Observations
The Ages of Nuclear Star Clusters in Early-Type Spiral Galaxies
A New Member of the Local Group?
The rarest of sightlines: probing the metallicity of a DLA with a nearby Low Surface Brightness galaxy
A Decade of AGN SEDs
The low redshift Lyman-alpha forest and the intrinsic QSO continuum
Anomalous Flux Ratios in Quadruple Gravitationally Lensed QSOs
Are We Missing the Dominant Sites of Star Formation in Local UV-Bright Starbursts?
Age-dating Star Clusters in M101
A near-IR imaging survey of sub-mm galaxies with spectroscopic redshifts
The Spectral and Morphological Evolution of Galaxies
The Fate of Luminous Compact Blue Galaxies: An Environmental Approach
The Dusty ISM Substructure in Nearby Spiral Galaxies
A Search for the Missing Baryons in Nearby Cosmic Filaments
Life in the fast lane: The dark-matter distribution in the most massive galaxy clusters in the Universe at z>0.5
The mass assembly history of early-type galaxies at z~1
The role of dark matter and intracluster gas in galaxy formation and cluster evolution
Nailing Down M31's Central Black Hole
Numerical simulations of outflows in quasars: the microphysics of BAL winds
The Upper End of the Supermassive Black Hole Mass Function: Pushing the 10 Billion Solar Mass Limit
The Globular Cluster Systems of Spiral Galaxies along the Hubble Sequence
Deep NICMOS imaging of HDF-South: restframe optical morphologies of high redshift galaxies
Resolving Galaxy Formation and Evolution for Interpretation of HST Observations
ESSENCE: Measuring the Dark Energy Equation of State
A Detailed Photoionization Study of the Broad Line Region of NGC 5548
Search for Black Holes in M31 Globular Clusters
Measurements of core sizes in luminous early-type galaxies
Accurate and Robust Calibration of the Extragalactic Distance Scale with the Maser Galaxy NGC 4258
The Astrophysics of Star Formation & Galaxy Building in the "Middle Ages": z ~ 0 to 2
Title
CYCLE 12: Approved Observing Programs

8
Institution
Carnegie Institution of Washington
Arizona State University
Fermilab
University of Wisconsin - Madison
Gemini Observatory, Northern Operations
Russian Academy of Sciences, Special Astrophysical Obs.
Carnegie Institution of Washington
Yale University
Space Telescope Science Institute
University of California - Santa Cruz
University of California - Santa Cruz
Universiteit Leiden
Universiteit Leiden
State University of New York at Stony Brook
Technion-Israel Institute of Technology
European Southern Observatory - Germany
University of Oklahoma Norman Campus
Carnegie Institution of Washington
Carnegie Institution of Washington
Carnegie Institution of Washington
Smithsonian Institution Astrophysical Observatory
Wesleyan University
Carnegie Institution of Washington
Space Telescope Science Institute
University of Maryland Baltimore County
Ohio State University
Ohio State University
Ohio State University
University of California - Santa Cruz
University of Colorado at Boulder
University of Michigan
The Johns Hopkins University
University of Florida
University of Florida
University of Oregon
Raytheon Technical Services Company
NASA Goddard Space Flight Center
University of California - Davis
Name
Luis Ho
Rolf Jansen
Sebastian Jester
Kelsey Johnson
Inger Jorgensen
Igor Karachentsev
Daniel Kelson
Jeffrey Kenney
Anton Koekemoer
David Koo
David Koo
Konrad Kuijken
Konrad Kuijken
Kenneth Lanzetta
Ari Laor
Soren Larsen
Karen Leighly
Barry Madore
Barry Madore
Patrick McCarthy
Jon Miller
Edward Moran
John Mulchaey
Christopher O'Dea
Eric Perlman
Bradley Peterson
Bradley Peterson
Bradley Peterson
Andrew Phillips
Daniel Proga
Douglas Richstone
Susan Ridgway
Bassem Sabra
Vicki Sarajedini
James Schombert
Edward Shaya
George Sonneborn
S. Stanford
SNAP
SNAP
GO
AR
GO
SNAP
GO
GO
AR
AR
AR
GO
GO
AR
GO
GO
GO
AR
GO
AR
GO
GO
GO
GO
GO
GO
GO
SNAP
AR
AR
GO
GO
GO
AR
AR
AR
GO
AR
Type
A Narrow-band Snapshot Survey of Nearby Galaxies
H-alpha Snapshots of Nearby Galaxies observed in F300W: Quantifying Star Formation in a Dusty Universe
The Nature of the UV Excess in the Jet of 3C273
A Multi-Wavelength Study of Super Star Clusters as They Emerge From Their Birth Material
Galaxy Evolution During Half the Age of the Universe: ACS imaging of rich galaxy clusters
The local Hubble flow and the density field within 6 Mpc
Galaxy Populations at Very Large Cluster Radii: The Outskirts of MS1054-03 at z=0.83
Ram Pressure Stripping in the Virgo Spiral NGC 4522
Morphology and Evolution of the Largest Complete Sample of X-ray Selected AGN
Evolution of the Tully-Fisher Relation of High Redshift z > 1 Disks Using GOODS-N Images and Keck DEIMOS Spectra
The Ages of Distant Field Galaxy Spheroids
Proper motion kinematics in Galactic bulge/bar fields
The mass of the Milky Way: orbits for Leo I and Leo II
Photometry and Photometric Redshifts of Faint Galaxies in the Ultra-Deep Field
Reverberation Mapping of the Least Luminous Seyfert 1 Galaxy NGC 4395
Young Massive Clusters in Spiral Galaxies and the Connection with Open Clusters
UV Spectroscopic Observations of Luminous Narrow-line Seyfert 1 Galaxies
Morphological Evolution of Galaxies from the Present to z = 0.3-0.5
M83: Calibrating the Cepheid PL Relation
Archival Study of Red Galaxies in the Chandra Deep Field South
Observations of Intermediate Mass Black Hole Candidate Ultra-Luminous X-ray Sources
X-ray-Bright, Optically Normal Galaxies: The "Hidden" Truth
The Role of Groups in the Evolution of Galaxies at Intermediate Redshifts
Time Scales for Gas Transport, Star Formation, and AGN Fueling in the Born-again Radio Galaxy 3C236
The Structure and Physics of Extragalactic Jets
AGN Black Hole Masses from Stellar Dynamics
Structure of the Accretion Disk in the NLS1 NGC 4051
Host Galaxies of Reverberation-Mapped AGNs
Nature & Evolution of Compact Galaxies in the GOODS-N Field
AGN Radiation-Driven Outflows: Models vs. Observations
Black Holes in Big Galaxies with Small Bulges
The Evolution of the Host Galaxies of Radio-Quiet Quasars
AALs in Quasars: Diagnostics of the Environment
AGN in the GOODS fields: A Study of Short-Term Variability, Spectroscopy and Morphology
Morphological and Structural Study of the Galaxies in Distant Cluster CL1322.5+3028
Optimization of the Tip of the Red Giant Branch Distance Estimator
Probing the Halo and ISM of Low-Redshift Galaxies with Young Supernovae
The Construction of Elliptical Galaxies at High Redshifts
Title
CYCLE 12: Approved Observing Programs

9

10 
Hector Arce
Taft Armandroff
Philip Armitage
Francesca Bacciotti
John Bahcall
Charles Bailyn
John Bally
Martin Barstow
Luciana Bianchi
Luciana Bianchi
Luciana Bianchi
Ann Boesgaard
Howard Bond
Howard Bond
California Institute of Technology
National Optical Astronomy Observatories, AURA
JILA
Osservatorio Astrofisico di Arcetri
Institute For Advanced Study
Yale University
University of Colorado at Boulder
University of Leicester
The Johns Hopkins University
The Johns Hopkins University
The Johns Hopkins University
University of Hawaii
Space Telescope Science Institute
Space Telescope Science Institute
Space Telescope Science Institute
California Institute of Technology
Princeton University
California Institute of Technology
University of Chicago
Lawrence Livermore National Laboratory
University of Maryland
University of Wisconsin - Madison
National Radio Astronomy Observatory
University of Melbourne
Space Telescope Science Institute
Space Telescope Science Institute
The Johns Hopkins University
Arizona State University
Bell Labs
Arizona State University
University of Arizona
Michigan State University
The Johns Hopkins University
The Johns Hopkins University
Universitats-Sternwarte Gottingen
Massimo Stiavelli
Lisa Storrie-Lombardi
Michael Strauss
Tommaso Treu
Jason Tumlinson
Wil van Breugel
Sylvain Veilleux
Bart Wakker
Fabian Walter
Rachel Webster
Richard White
Bradley Whitmore
Gerard Williger
Rogier Windhorst
David Wittman
Haojing Yan
Yujin Yang
Stephen Zepf
Wei Zheng
Wei Zheng
Bodo Ziegler
Galactic Programs
Institution
Name
AR
GO
AR
GO
GO
AR
GO
GO
GO
GO
GO
GO
GO
GO
GO
GO
GO
AR
SNAP
GO
GO
GO
GO
GO
GO
GO
GO
SNAP
AR
GO
GO
GO
GO
SNAP
GO
Type
The Impact of Infall and Outflow Motions on the Circumstellar Envelope of Young Stars
Dwarf Elliptical Galaxies in Nearby Groups: Stellar Populations and Abundances
Turbulent Variability of Disk Accretion in Cataclysmic Variables
Rotation in Jets from Young Stars: investigating NUV lines with very high Spectral Resolution
Observing the Next Nearby Supernova
Archival Studies of Main Sequence Binaries in 47 Tucanae (NGC104)
An ACS/WFC H-alpha Survey of the Orion Nebula
Verifying the White Dwarf Mass-Radius Relation with Sirius B
The Planetary Nebula K648 in the Globular Cluster M15
UV extinction by dust in unexplored LMC environments
Young Massive Clusters in M33
Boron in F Stars in the Hyades - Insights into the Li-Be Dip
HST Observations of Astrophysically Important Visual Binaries
Trigonometric Calibration of the Period-Luminosity Relations for Fundamental and First-Overtone Galactic Cepheids
The environment of QSOs at the reionization epoch
Morphologies of EROs and Field Galaxies in SIRTF's First Look Survey: A Rich Early Release Dataset
The Host Galaxies of Type II Quasars
The Lenses Structure and Dynamics (LSD) Survey: mass distribution and stellar populations of high redshift E/S0 galaxies
Probing IGM Phases, Metals, and the Cosmic Web with New SDSS QSOs
Giant Lya Halos Around High Redshift Radio Galaxies
The Fundamental Plane of Massive Gas-Rich Mergers
Intergalactic O VI absorption at redshift <0.004
Investigating the Powering Sources of Expanding Supergiant Shells in the Nearby Dwarf Galaxy IC 2574
Microarcsecond Imaging of a Gravitationally Lensed QSO: 2237+0305
Leaky IGM at z=6 or Lyman Alpha Galaxy at z=5?
ACS, NICMOS, and STIS Observations of Three Ongoing Mergers
A test of the foreground proximity effect at z=1.2
NIC3 SNAPs of nearby galaxies imaged in the mid-UV: the remarkable cool stellar population in late-type galaxies.
Probing the Mass Distribution at High Redshift in the UDF
NIC3 Imaging of z~6 Candidates in a Deep ACS Parallel Field: Finding the reionizing population and their LF
Galaxy Evolution in Action: The Detailed Morphology of Post-Starburst Galaxy
The Age and Mass Function of the Intermediate Age Globular Cluster System of NGC 4365
Properties of the Intergalactic Medium near the Epoch of HeII Reionization
Confirmation of New Candidates for the Study of Intergalactic Helium
Evolution of Scaling Relations of Field Spiral Galaxies at Intermediate Redshift
Title
CYCLE 12: Approved Observing Programs
Institution
Institut d'Astrophysique Spatiale
European Southern Observatory
Anglo-Australian Observatory
University Corporation For Atmospheric Research
University of California - Los Angeles
Smithsonian Institution Astrophysical Observatory
Louisiana State University & Agricultural & Medical College
The University of Virginia
American Museum of Natural History
Pennsylvania State University
National Optical Astronomy Observatories, AURA
National Optical Astronomy Observatories, AURA
United States Naval Observatory
Yale University
Rice University
University of Colorado at Boulder
University of Toledo
Kapteyn Astronomical Institute
University of Kentucky
Dartmouth College
University of Southampton
University of Notre Dame
University of Arizona
Georgia State University Research Foundation
Georgia State University Research Foundation
University of Cambridge
University of Delaware
University of Delaware
University of Delaware
New Mexico State University
University of Arizona
University of Colorado at Boulder
McMaster University
Rice University
Open University
Wesleyan University
University of Colorado at Boulder
Arizona State University
Name
Francois Boulanger
Herve Bouy
Terry Bridges
Timothy Brown
Adam Burgasser
Nuria Calvet
Stefan Cartledge
Roger Chevalier
Orsola De Marco
John Debes
Andrew Dolphin
Andrew Dolphin
Bryan Dorland
Gordon Drukier
Reginald Dufour
Douglas Duncan
Steven Federman
Annette Ferguson
Gary Ferland
Robert Fesen
Boris Gaensicke
Peter Garnavich
Donald Garnett
Douglas Gies
Douglas Gies
Gerard Gilmore
John Gizis
John Gizis
John Gizis
Bertrand Goldman
Karl Gordon
Graham Harper
William Harris
Patrick Hartigan
Carole Haswell
William Herbst
Gregory Herczeg
Jeff Hester
GO
SNAP
GO
GO
GO
GO
GO
AR
GO
GO
AR
GO
GO
GO
SNAP
GO
AR
GO
AR
GO
SNAP
AR
GO
GO
GO
SNAP
GO
GO
SNAP
GO
GO
AR
GO
GO
GO
GO
AR
GO
Type
SMC Extinction Curve Towards a Quiescent Molecular Cloud
Multiplicity among brown dwarfs in the Pleiades cluster
Search For Metallicity Spreads in M31 Globular Clusters
A Search for Water Vapor in the Atmosphere of an Extrasolar Planet
T Dwarf Companions: Searching for the Coldest Brown Dwarfs
Search for Core-disrupting Wide-Angle Winds
Exploring Interstellar Krypton Abundance Variations at Kiloparsec Scales
Stellar wind interactions around binary stars: models for planetary nebulae
A tailored survey of proplyds with the ACS
Finding Planets in the Stellar Graveyard: A Faint Companion Search of White Dwarfs with NICMOS
CTE Corrections for WFPC2 and ACS
ACS Photometric Zero Point Verification
The Kinematics and Dynamics of the Material Surrouding Eta Carinae
Shooting Stars: Looking for Direct Evidence of Massive Central Black Holes in Globular Clusters
CIII] Imagery of Planetary Nebulae and HII Regions -- A Snap Program
Experimental Proof of the Neutrino Process in SN from Boron Isotope Measurements
Surveying Interstellar Carbon Monoxide Via Ultraviolet Absorption
Stellar Populations in the Outskirts of M33: A Unique Probe of Disk Galaxy Formation
Calculation of Fe II atomic data required for the modeling of HST observations
Probing the Dynamics and Shock Physics of the Cas A Supernova Remnant
Towards a global understanding of accretion physics - Clues from an UV spectroscopic survey of cataclysmic variables
Transients in the Ultra-Deep Field
Recombination Lines and Temperature Structure in Planetary Nebulae
The Masses of the O-type Binary 15 Monocerotis
Wind Accretion and State Transitions in the Black Hole Binary Cyg X-1
A snapshot survey of rich stellar clusters in the Large and Small Magellanic Clouds
Ultraviolet Observations of a Very Young Brown Dwarf
NICMOS Observations of Cool Brown Dwarf Doubles
A Snapshot Search for Halo Very-Low-Mass Binaries
Brown dwarf atmospheric variability observations
The Exciting Wavelength of Extended Red Emission
New Insights into Betelgeuse's Inhomogeneous Wind
Establishing the Metallicity Distribution in Normal Giant Ellipticals
Ultraviolet Emission from Protostellar Accretion Disks
Microquasars: Outbursts and Outflows in Black Hole Accretion Flows
Natural Coronagraphic Imaging of KH 15D
Models of Gas in Disks of Classical T Tauri Stars
ACS Monitoring of the Polarization of the Crab Nebula
Title
CYCLE 12: Approved Observing Programs

11 
Institution
Space Science Institute
University of Arizona
University of California - San Diego
University of Michigan
Rice University
Rice University
Rice University
Universitat Tubingen, Institut fur Astronomie & Astrophysik
University of California - Berkeley
University of California - Berkeley
Space Telescope Science Institute
University of Washington
University of Southampton
University of Southampton
Space Telescope Science Institute
Northwestern University
University of Wisconsin - Madison
Massachusetts Institute of Technology
University of Hawaii
Osservatorio Astrofisico di Arcetri
Lowell Observatory
Lowell Observatory
California Institute of Technology
New Mexico State University
Smithsonian Institution Astrophysical Observatory
University of Arizona
European Southern Observatory - Germany
Universita di Padova
University of Colorado at Boulder
Universidad de Valencia
Space Telescope Science Institute
Yale University
Vanderbilt University
Vanderbilt University
The Pennsylvania State University
The Pennsylvania State University
College of Charleston
University of Southern California
Name
Dean Hines
Jay Holberg
J. Howk
Jimmy Irwin
Christopher Johns-Krull
Christopher Johns-Krull
Christopher Johns-Krull
Stefan Jordan
Paul Kalas
Paul Kalas
Charles Keyes
Ivan King
Christian Knigge
Christian Knigge
John Krist
James Lauroesch
Alex Lazarian
Walter Lewin
Michael Liu
Roberto Maiolino
Philip Massey
Philip Massey
Bruce McCollum
Bernard McNamara
S. Megeath
Michael Meyer
Roberto Mignani
Yazan Momany
Jon Morse
Jose Munoz
Edmund Nelan
M. Sean O'Brien
Robert O'Dell
Robert O'Dell
George Pavlov
George Pavlov
Laura Penny
Geraldine Peters
GO
GO
AR
AR
AR
GO
GO
GO
GO
GO
GO
GO
GO
GO
GO
GO
AR
AR
GO
SNAP
GO
GO
SNAP
AR
GO
GO
GO
GO
GO
GO
GO
GO
AR
GO
GO
GO
AR
SNAP
Type
Enabling Coronagraphic Polarimetry with NICMOS
STIS Observations of Orbital and Rotational Variations in the Unique Post-Common Envelope System HS1136+6646
Interstellar Cooling in the SMC: a Template for Understanding High-Redshift Star Formation
The Globular Cluster-Low Mass X-ray Binary Connection in Nearby Early-type Galaxies: An Archival Study
Accretion Shocks in Classical T-Tauri Stars
The Distance to the Pleiades
Separating Activity and Accretion in T Tauri Stars
The field structure of the most strongly magnetized white dwarf PG1031+234
ACS Imaging of beta Pic: Searching for the origin of rings and asymmetry in planetesimal disks
ACS detection of sub-stellar companions around Vega, Fomalhaut and beta Pic via parallax & proper motion
Multi-wavelength Observations of Symbiotic Stars in Outburst
The Bottom of the Main Sequence in the Old, Metal-Rich Cluster, NGC 6791
Curing the SW Sex Syndrome
Uncovering the CV population in M15: a deep, time-resolved, far-UV survey of the cluster core
Evolution of Young Stellar Outflows: XZ Tauri and HH 30
The Physical Character of the Smallest-Scale Interstellar Structures
Flows, Turbulence, and Mixing
Archival HST Studies of Six Globular Clusters
NICMOS Confirmation of a Young Planetary-Mass Companion
A NICMOS search for obscured supernovae in starburst galaxies
The Physical Parameters and Stellar Winds of Hot, Massive Stars at High Metallicity: O-stars in the Andromeda Galaxy
A He-rich O2-3 star in the LMC: Freakish Relic or Paradigm Shifter?
First Spectroscopic Study of a Unique Set of Young Stars in the Orion Nebula
Searching for Very Low Mass Objects in M35 Using the HST/FGS Archive
How do Brown Dwarfs Form?
The Origins of Sub-stellar Masses: Searching for the 'End' of the IMF
Timing of the proposed optical counterpart of the 16 ms LMC X-ray pulsar PSR J0537-6910
SagDIG: a benchmark for understanding star formation in extreme low-metallicity galaxies
Tracking the Homunculus and Outer Ejecta of Eta Carinae
A Survey of Extinction Curves to Redshift z=1
Dynamical Masses and Radii of Four White Dwarf Stars
The Distance and Mass of the Neutrino-Luminous White Dwarf PG 0122+200
Analysis of Helix Nebula Observations During the Leonids Encounter of 2002
Calibration of the ACS Emission Line Filters
Far-UV Spectrum and Pulsations of PSR 0656+14: Thermal vs. Nonthermal
What's The Point? Deep NICMOS Imaging of the Central X-ray Point Source in Cas A
Projected Rotational Velocities of O-type Stars at Low Metallicity
A SNAPSHOT Survey of Sharp-Lined Early B-Type Stars
Title
CYCLE 12: Approved Observing Programs

12 
Institution
Università di Padova
Jet Propulsion Laboratory
European Southern Observatory - Germany
National Optical Astronomy Observatories, AURA
University of Hawaii
University of California - Los Angeles
European Southern Observatory - Germany
University of Barcelona
Smithsonian Institution Astrophysical Observatory
Jet Propulsion Laboratory
Jet Propulsion Laboratory
Space Telescope Science Institute
University of California - Berkeley
The Johns Hopkins University
The Pennsylvania State University
University of Florida
Harvard University
Observatoire de Strasbourg
Space Telescope Science Institute
NASA Ames Research Center
University of Cambridge
University of Colorado at Boulder
Space Telescope Science Institute
California Institute of Technology
University of Victoria
State University of New York at Stony Brook
University of California - Berkeley
University of Chicago
Universitat Tubingen, Institut fur Astronomie & Astrophysik
California Institute of Technology
Space Telescope Science Institute
University of Colorado at Boulder
The Johns Hopkins University
Astrophysikalisches Institut Potsdam
Name
Giampaolo Piotto
Steven Pravdo
Francesca Primas
Barton Pritzl
Bo Reipurth
Michael Rich
Martino Romaniello
Pilar Ruiz-Lapuente
Steven Saar
Raghvendra Sahai
Raghvendra Sahai
Kailash Sahu
Karin Sandstrom
Ravi Sankrit
Divas Sanwal
Ata Sarajedini
Dimitar Sasselov
Matthias Schreiber
Kenneth Sembach
Janet Simpson
Stephen Smartt
John Stocke
Roeland van der Marel
Schuyler Van Dyk
Don Vandenberg
Frederick Walter
Barry Welsh
Daniel Welty
Klaus Werner
Russel White
Robert Williams
Brian Wood
Rosemary Wyse
Hans Zinnecker
GO
GO
GO
SNAP
GO
SNAP
GO
GO
GO
GO
SNAP
GO
GO
GO
GO
GO
GO
GO
GO
GO
GO
GO
AR
AR
GO
GO
GO
GO
GO
GO
GO
AR
AR
GO
Type
Geometric Distances of the Galactic Globular Clusters NGC2808 and NGC6752
NICMOS Observations of the Gl 164 Companion
Boron in stars of same O and Li, but different Be: testing cosmic-ray vs. neutrino spallation
The Second Parameter Effect in Metal-Rich Globular Clusters: A Snapshot Study of NGC 6388
HH110: Collision between a Jet and a Cloud
A Snapshot Survey of Galactic Bulge Globular Clusters
Low Mass Star Formation at Low Metallicity: Accretion Rates of Pre-Main Sequence Stars in the Large Magellanic Cloud
Probing the nature of Type Ia SNe through HST astrometry
Whirling Dervish Dynamos: Magnetic Activity in CV Secondaries
Tracking the Evolution of a Knotty, High-Speed Jet in the Carbon Star, V Hydrae
Are OH/IR Stars the Youngest post-AGB stars? A NICMOS Imaging Survey
Accurate Mass Determination of the Ancient White Dwarf ER 8 Through Astrometric Microlensing
UV Spectroscopy of the Hot, Helium-Core White Dwarf Companion in HR 1608
Kepler's Supernova Remnant: an Imaging Study of the Blast Wave - Circumstellar Medium Interaction
Optical Counterpart of the Neutron Star 1E 1207.4-5209 in PKS 1209-51/52 Supernova Remnant
Main Sequence Turnoff Ages For Second Parameter Clusters in M33
OGLE-TR-56b: The Most Interesting Transiting Planet
Detecting the hottest white dwarf in a dwarf nova: V446 Her as a laboratory for irradiated accretion discs
The Properties of Highly Ionized High Velocity Gas in the Distant Galactic Corona and Local Group
A Search for the Exciting Sources in OMC-1 through NICMOS Polarization Measurements
Direct imaging of the progenitors of massive, core-collapse supernovae
Probing Outflowing Winds from the Galactic Center
Stellar Dynamical Models for HST Proper Motion Datasets
The Local Environments of Supernovae in Archival HST Images
Parallaxes of Extreme Halo Subgiants: Calibrating Globular Cluster Distances and the Ages of the Oldest Stars
The Parallax of Geminga
Where is the Local Hot Gas?
Abundances, Dust, and Physical Conditions in the LMC ISM
Iron deficiency in hot hydrogen-deficient post-AGB stars
A Search for Young Binary Brown Dwarfs: Constraining Formation Scenarios and Masses Through Multiplicity
Integrated Absorption- and Emission-Line Analysis of Nebulae
Searching for Astrospheric Lyman-alpha Absorption Detections in the HST Archive
An astrometric standard field in omega Cen
A NICMOS direct imaging search for giant planets around the seven single white dwarfs in the Hyades
Title
CYCLE 12: Approved Observing Programs

13 
Institution

14 
University of Texas at Austin
University of California - Davis
Smithsonian Institution Astrophysical Observatory
Space Telescope Science Institute
University of California - Los Angeles
Lawrence Berkeley National Laboratory
Space Telescope Science Institute
Space Telescope Science Institute
Cornell University
Wellesley College
University of Arizona
Texas A & M Research Foundation
University of Michigan
California Institute of Technology
Southwest Research Institute
Southwest Research Institute
NASA Ames Research Center
Space Telescope Science Institute
The University of Virginia
The Johns Hopkins University
Arizona State University
Nicholas Scoville
Rodger Thompson
California Institute of Technology
University of Arizona
Hubble Treasury Programs
Fritz Benedict
Michael Gregg
Christopher Kochanek
Sangeeta Malhotra
Matthew Malkan
Saul Perlmutter
Adam Riess
Kailash Sahu
Large Programs
James Bell
Richard French
Erich Karkoschka
Mark Lemmon
Tariq Majeed
Jean-Luc Margot
William Merline
Joel Parker
Mark Showalter
William Sparks
Anne Verbiscer
Harold Weaver
Rogier Windhorst
Solar System Programs
Name
GO
GO
GO
SNAP
GO
GO
GO
GO
GO
GO
GO
GO
GO
GO
AR
GO
SNAP
GO
GO
GO
AR
GO
AR
Type
The COSMOS 2-Degree ACS Survey
Deep Near IR Images in the Chandra Deep Field South Ultra Deep Field
An Astrometric Calibration of the Cepheid Period-Luminosity Relation
The Next Generation Spectral Library
HST Imaging of Gravitational Lenses
The Grism-ACS Program for Extragalactic Science (GRAPES)
The NICMOS Parallel Observing Program
Exploration of the SN Ia Hubble Diagram at z > 1.2
Tracing the History of Cosmic Expansion to z~2 with Type Ia Supernovae
The Galactic Bulge Deep Field: A Planetary Transit Survey and Very Deep Stellar Mass Function
Spectroscopy and Polarimetry of Mars at Closest Approach
Saturn's rings and small moons on the eve of Cassini
The Long-term Observational Record of Uranus' Atmosphere, its Rings, and its Satellites: the WFPC2-ACS Link
From molecules to aerosols: observing the haze creation process during Titan's polar summer
Using STIS Observations of Auroral Lyman Alpha Line Profiles to Map High-Altitude Winds on Jupiter
Binary systems in the Kuiper Belt
An Imaging Survey of the Statistical Frequency of Binaries Among Exceptionally-Young Dynamical Families in the Main Asteroid Belt
Ceres: High-Resolution Mapping and Determination of Physical Properties
Rings of Uranus: Dynamics, Particle Properties and Shepherding Moons
Lightning on the Jovian Dayside
UVBRI Photometry of Janus and Epimetheus
Volatile Abundances and the D/H Ratio in Long-Period Comets
All-Sky Archival Zodiacal Background Measurements: Constraints to Kuiper Belt Objects at R=28-60 mag.
Title
CYCLE 12: Approved Observing Programs
Hubble Fellowship Program
Michael Fall, fall@stsci.edu
H
ubble Fellowships are awarded annually to outstanding young scientists engaged in
research related to the Hubble mission. The research may be observational—either
space-based or ground-based—or theoretical. The Fellowships provide three years of
salary and other support at U.S. host institutions of a Fellow’s choice (subject to a
maximum of one new Hubble Fellow per institution per year).
A selection committee met at the Institute in January 2003 to review about 100 applications
for Hubble Fellowships to start in September 2003. The new Fellows are listed in the table below.
Hubble Fellows present the results of their research each year at a Hubble Fellows
Symposium held at the Institute. The most recent Symposium was held on March 6 and 7, 2003.
We plan to select approximately 12 new Hubble Fellows in winter 2003/4 for positions to
start in fall 2004. The Announcement of Opportunity, available at http://www.stsci.edu/
stsci/hubblefellow/ao.html, provides instructions for the application process. Ω
2003 New Hubble Fellows
Name
Ph.D. Institution
Host Institution
Avishay Gal-Yam
Marla Geha
Jason Harris
Wynn Ho
Marc Kuchner
Darren Madgwick
Michael Muno
Jeffrey Newman
Nathan Smith
Tommaso Treu
Risa Wechsler
Qingjuan Yu
Tel Aviv, 2003
Santa Cruz, 2003
Santa Cruz, 2000
Cornell, 2003
Caltech, 2000
Cambridge, 2002
MIT, 2002
Berkeley, 2000
Minnesota, 2002
Pisa/STScI, 2001
Santa Cruz, 2001
Princeton, 2002
Caltech
Carnegie
Arizona
Stanford
Princeton
LBNL
UCLA
LBNL
Colorado
UCLA
Chicago
Berkeley
The Dumbbell
Nebula - M27
A
n aging star’s last hurrah is creating a flurry of glowing
knots of gas that appear to be streaking through space in
this close-up image of the Dumbbell Nebula, taken with
NASA's Hubble Space Telescope. The Dumbbell, a nearby
planetary nebula residing more than 1,200 light-years away, is
the result of an old star that has shed its outer layers in a
unique display of color.
Image Credit: NASA and the Hubble Heritage Team (STScI/AURA)
Acknowledgment: C.R. O’Dell (Vanderbilt University)

15 
The Local Group: The Universe
In A Nutshell
Mario Livio, mlivio@stsci.edu
T
his year’s May Symposium was on the topic of “The Local Group as an Astrophysical
Laboratory.” The Symposium took place May 5-8, 2003, and it attracted about 130
participants. The choice of topic reflected the fact that observations of the Local Group
have reached the point where they can provide a closer look at processes characterizing
the universe at large.
From observations of the cosmic microwave background by the Wilkinson Microwave
Anisotropy Probe (WMAP), we know that the energy density of the universe is dominated by
‘dark energy’ (about 73%) and non-baryonic dark matter (about 22%). Originally it was thought
that the mass in the halos of galaxies might be dominated by Massive Compact Halo Objects
(MACHOs), such as brown dwarfs. Microlensing observations towards the Magellanic Clouds
revealed that even in the most optimistic case, MACHOs could not constitute more than 5% of
the dark matter in the universe, in agreement with the WMAP results. Furthermore, 4 out of the
17 observed microlensing events, for which additional information about location exists, seem
to be due to self lensing by Magellanic Clouds stars rather than by MACHOs. Thus, the fraction
of mass in MACHOs could be even much smaller.
Structure formation is a second topic to which Local Group observations have contributed and
will continue to contribute significantly. Current models indicate that the growth of structure in
the universe occurred by hierarchical accretion and merger of dark-matter halos. Since galaxy
halos should simply be scaled versions of galaxy clusters, a few hundred satellites should
accompany galaxies like the Milky Way. The number observed is only a few tens. This increases
the importance of studies of high velocity clouds in the Local Group (as potential satellites) and
of processes within galaxies, such as feedback from star formation. At the same time,
observations of the halo of M31 reported at the Symposium support the idea of past mergers.
These observations reveal the presence of a significant population of stars with ages of 6-8
billion years, in contrast to the halo of the Milky Way, where all the ages are between 11 and
13 billion years. This result suggests that M31 may have undergone a major merger some 6 to
8 billion years ago, which threw younger stars from the disk into the halo.
Central black holes are a third topic for which observations within our cosmic backyard are
important. Black holes have already been discovered at the centers of many galaxies, and
collapse into a black hole may be inevitable at the center of very dense stellar systems. The
center of the Milky Way afforded a very special treat at the Symposium, with the report that full
orbits have now been determined for a few stars around the Galactic black hole, Sgr A∗.
Furthermore, evidence suggests the existence of intermediate-mass (a few thousands to a few
tens of thousands solar masses) black holes at the centers of the Galactic globular cluster M15
and the M31 cluster G1.
Finally, the Local Group allows a glimpse at star formation in different environments, with
different metallicities. Theory suggests that in a hot, metal-free universe, the Initial Mass
Function was strongly biased towards massive stars. Starburst regions in the Local Group offer
the opportunity to test some of these ideas.
Observational and theoretical tools can both now be used on the Local Group to place
meaningful constraints on our understanding of the universe. Ω

16 
Advances with ACS
Roeland P. van der Marel, marel@stsci.edu
F
igure 1 provides a spectacular illustration of the powerful capabilities of the Advanced
Camera for Surveys (ACS). In a large Cycle 11 program, Tom Brown and collaborators used
the Wide Field Channel (WFC) to take deep images of a field in the halo of the Andromeda
galaxy (Messier 31). The panels in the figure show cut-outs that each cover about 1% of
the total WFC field of view. Each panel shows a stunning combination of Andromeda halo
stars and background galaxies. The results of this program provide the deepest image obtained
with Hubble to date. Objects are detected to a limiting magnitude of 31 and there are 300,000
stars in a single ACS/WFC field. The color-magnitude diagram of the stars indicates that
approximately one-third of the Andromeda halo stars formed only 6 to 8 billion years ago, which
is much younger than the 11-to-13 billion-year age of the stars in the Milky Way’s halo. This
finding provides important new clues to the formation of galaxy halos (http://hubble.stsci.edu/
newscenter/archive/2003/15/).
On Astronomy Day, May 10, the Institute released a beautiful mosaic of the Helix nebula (NGC
7293; see http://hubble.stsci.edu/newscenter/archive/2003/11/) in conjunction with a
variety of other outreach activities. ACS obtained the data for this image during the Leonids
Figure 1: Advanced Camera for Surveys images of fields in the halo of the Andromeda galaxy (Messier 31). Each
panel covers about 1% of the total field of view of the Wide Field Channel and shows a stunning combination of
Andromeda halo stars and background galaxies. Tom Brown and his collaborators are using these data to study the
formation of galaxy halos.
meteor shower in November 2002. At that time we pointed Hubble in the anti-radiant
direction of the meteor shower to minimize the risk for potential damage to the telescope. The
Helix nebula happens to lie close to this anti-radiant direction. This provided an opportunity for
a group of Institute staff and astronomical community members to observe the nebula in a
non-proprietary campaign.
The Hubble Heritage Team used data from a program aimed at calibration
Continued
of the ACS polarizer filters to create a spectacular image of the Egg
page 18
nebula (http://hubble.stsci.edu/newscenter/archive/2003/09).

17 
Advances with
ACS from page 17

18 
ACS will continue to be a focus of attention in Cycle 12. The Institute Director announced the
approved programs in April 2003. They are listed on page 8 in this newsletter. ACS
observations again make up more than half the accepted programs. The Treasury program of
Scoville and collaborators is of particular interest. These investigators will perform a 2 square
degree imaging survey (the Cosmic Evolution Survey—COSMOS) with ACS. The survey will
study an equatorial field that is accessible to all ground-based telescopes. The data will be
non-proprietary and will be available for use by the entire astronomical community.
The Cycle 12 TAC also approved four ACS calibration proposals from the astronomical
community. We are looking forward to the results from these programs and the improved
understanding that they will provide of the instrument.
At the Institute, we are continuing to analyze Cycle 11 ACS calibration data. Sixteen
supported modes of the ACS High Resolution Channel (HRC) lie in the wavelength regime below
4000 Å. We have now created improved flat field reference files for these modes. For those
filters that do not have significant red leaks, we used observations of the bright Earth
(http://www.stsci.edu/hst/acs/documents/isrs/isr0302.pdf). While the bright Earth is a poor flat
field source at optical wavelengths because of structure in the cloud cover, it is a uniform source
of diffuse light at shorter wavelengths due to the high optical depth above the cloud layer.
Observations of Wolf-Rayet stars are useful for the wavelength calibration of the
ACS/WFC G800L grism. Dispersion solutions were derived from such data (http://www.stsci.edu/
hst/acs/documents/isrs/isr0301.pdf). The results were incorporated into the extraction
software ‘aXe’ (http://www.stecf.org/software/aXe/), which is maintained by the Space Telescope
European Coordinating Facility.
We completed a variety of checks and tests of ACS. We photometrically verified the stability
of the shutters for short exposure times and found that they operate within the pre-launch
specifications. We also monitored for a potential decrease of ultraviolet sensitivity due to
contamination but found none.
Photometry of star fields revealed that the point-spread function (PSF) on WFC shows mild
variations over the field of view. We found that this is the result of small spatial variations in the
thickness of the detector, which affect the charge diffusion properties of the CCD. John Krist
developed a model for this effect and included it in the new release of his PSF modeling
software Tiny Tim (http://www.stsci.edu/software/tinytim/).
We are now analyzing the first external calibration data taken on ACS to measure the effects
of Charge Transfer Efficiency (CTE) degradation on stellar photometry. Preliminary results match
expectations. For typical observing backgrounds and stellar fluxes, CTE losses on WFC are
typically 1 to 2% far from the readout amplifier and readily correctable. However, in worst-case
scenarios—faint sources observed with narrow-band filters—CTE losses can be significantly
larger. No measurable CTE effects are seen for the HRC at this time. As for other CCD detectors
in space, the CTE of ACS is expected to degrade with time. The advent of the Aft Shroud Cooling
System (ASCS) during the next servicing mission should mitigate this degradation. The thermal
vacuum testing of the ASCS was just completed successfully at Goddard Space Flight Center.
Investigators preparing WFC observations for Cycle 12 should pay particular attention to the
anticipated growth of hot pixels (see: http://www.stsci.edu/hst/acs/documents/isrs/isr0209.pdf).
Proper dithering strategies are required to correct for hot pixels during data reduction, as
described in the most recent ACS newsletter (http://www.stsci.edu/hst/acs/
documents/newsletters/stan0302.html). This newsletter also provides other important
information for those preparing Phase II programs. For example, we are now providing full bias
calibrations for the non-default gain settings 2 on WFC and 4 on the HRC, in addition to the
default settings (1 and 2, respectively). Also, selection of general subarrays will be available in
Cycle 12 and, in some cases, supported. In this context, supported means that bias frame
calibrations will be supplied by the Institute for a predefined set of subarrays.
Many papers on the calibration of ACS, both from Institute staff and members of the
astronomical community, can be found in the proceedings of the 2002 HST calibration workshop,
which are now available on-line (http://www.stsci.edu/hst/HST_overview/documents/
calworkshop/workshop2002). As always, the latest news about ACS can be found at
http://www.stsci.edu/hst/acs/. Ω
JWST Mission Replan
Nino Panagia, panagia@stsci.edu
S
purred by a better understanding of the mission costs and available funding, NASA
management began an end-to-end examination of the program in November 2002. The
‘replan’ teams involved members from all the development partners and the recently
selected Science Working Group (SWG).
On January 15, the replan teams reported their conclusions to the JWST project manager Phil
Sabelhaus and NASA Headquarters (HQ). If the plan is implemented, the greatest savings will
be achieved by ESA providing an Ariane V for the launch vehicle. Northrop Grumman Space
Technology (NGST) will develop the integration and test system and the flight software and
hardware for the observatory instead of NASA. Integration and test of the science instrument
module remains a NASA responsibility. NASA will supply the detectors and support electronics
for the ESA near infrared spectrograph. All other instrument projects will procure their own
detectors and associated electronics. The observatory-level integration and test plan was
simplified to provide additional time for the development and delivery of the science instruments.
To further reduce risk, the project decided to reduce the effective area of the primary mirror
to 25 square meters (down from 29.4 in the original TRW/Ball proposal). The smaller size meets
the baseline science requirements and can be achieved with larger but fewer segments (18
instead of 36). For additional savings, the Canadian Space Agency (CSA) contribution of tunable
filters cameras was removed from the Near Infrared Camera (NIRCam) and combined with the
Fine Guidance System. While this step did not significantly reduce U.S. costs, it simplifies the
working arrangements between CSA and other JWST partners and reduces technical risk in the
NIRCam. The Mid-Infrared Instrument (MIRI) team proposed reductions in U.S. contributions to
the MIRI development by reducing detector and cryocooler development costs and by increasing
software contributions from the European team.
The replan is on its way to becoming reality. ESA has proposed to provide the Ariane V
launcher for JWST. NASA HQ has reviewed the replan and the cumulative savings and has given
approval to move forward. Anne Kinney, the director of the Astronomy and Physics Division at
NASA HQ, has repeated her endorsement of the basic JWST instrument capabilities (NIRCam,
Near Infrared Spectrometer, and MIRI). With these steps, the Project will complete the
replanning exercise and prepare for the key reviews that are required before the JWST team can
begin detailed design and development planning (Phase B). Ω
News from the Multimission
Archive at STScI (MAST)
Paolo Padovani on behalf of the MAST team, padovani@stsci.edu
I
n early June 2003, Hubble data archive contains 13.8 terabytes of data in about 312,000
science data sets. The archive ingestion rate set another record in February 2003 at almost
19 gigabytes per day. The retrieval rate also set a record the same month, reaching almost
60 gigabytes per day.
New MAST Search Interface Features
We have added three new features to the MAST search interfaces:
• Multiple input targets. This feature allows users to search MAST on a list of sky positions
or astronomical names, providing a quick and easy way to look for sources having MAST
data in an arbitrary catalog.
• New preview page for Hubble data. This feature now conforms to the preview pages of
other missions by including not only the data preview but also
Continued
essential information on the observation and the original proposal and
page 20
links to published papers.

19 
Mast from
page 19
• High Level Science Products (HLSP) column. The MAST search output page now has an
extra column for HLSP, which is for the fully processed images and spectra. A number in
this column shows if and how many HLSP related to a given dataset are available and provides
links to an HLSP page where one can download the data and access information about them.
As usual, send any comments/questions/suggestions/praises you might have to archive@stsci.edu.
Cycle 12 Treasury, Large, & Legacy Archival (TALL) Programs
At the MAST, we are making plans to archive sets of contributed data coming from TALL
programs recently awarded time in Cycle 12. As we are doing for the Cycle 11 TALL programs,
we will be ingesting into MAST HLSP for these projects as soon as they are made available.
The full lists of Cycle 11 and Cycle 12 TALL programs, along with links to the available HLSP and
individual program World Wide Web sites, are available at http://archive.stsci.edu/hst/tall.html.
NICMOS Added to the Hubble ‘Pointings’ Interface
By now readers should be familiar with the MAST ‘pointings’ interface
(http://archive.stsci.edu/cgi-bin/point), a tool that allows users to make advanced searches
by position and by ranges of the sky in Galactic latitude, ecliptic latitude, right ascension, and
declination to which Hubble has been ‘pointed’. We are pleased to announce that this tool now
includes Near Infrared and Multi-Object Spectrometer (NICMOS) data. An example of the
queries that are now possible: “How many regions of the sky have been observed at least twice
in the J and H band for longer than 1,000 s?” (Answer: 98). Future versions of this tool will
include Advanced Camera for Surveys (ACS) data.
StarView News
We recently released StarView 7.2. Current users of StarView are upgraded automatically
through the self-update feature. This version of StarView’s most prominent new feature is the
Vizier catalog interface. Vizier is the astronomical catalog system supported by SIMBAD at the
Centre de Donnees astronomiques de Strasbourg (CDS). Users can now make queries of any
catalog available through Vizier and then search for corresponding Hubble observations. We
have also simplified user preferences and enabled a ‘right-click’ option to retrieve specific files.
For example, when looking at the reference or On-The-Fly-Reprocessing screen results for a
dataset and wanting to retrieve a single reference file, one can now simply ‘right click’ on the
name to request that file. Users can also request specific files by their file name directly from
the Retrieval window. StarView is also ready to work with the new Hubble data distribution
system, which will be opened to the public in late summer or early fall. We have also included
a new and improved version of SpecView for spectral data preview exploration.
Ingest and Distribution Systems Redesign
For the last couple of years, the Institute has been developing a Unix-based replacement for
the Data Archive and Distribution System (DADS). As storage and CPU requirements intensified,
the Institute also invested in a massive ‘spinning disk’ storage system, an EMC Symmetrix 8830,
and a multi-CPU, multi-domain Sunfire 15K server. Once the software solution for DADS
retrievals is operational, users will be able to retrieve subsets of the data (e.g., just the raw data
or just the calibrated data). They will also have guest privileges for public data, which means
that registration will no longer be necessary for non-proprietary data. DADS should work more
reliably and faster because it will retrieve most of the basic data from spinning disk rather than
jukeboxes of platters. Internally, we will be able to manage queues more sensibly than
‘first-come, first-served’, which is the only mode currently available.
MAST to Archive Galaxy Evolution Explorer Data
On April 28 the Galaxy Evolution Explorer (GALEX) satellite was successfully launched on a
Pegagus XL rocket. Its mission is to survey the whole sky for ultraviolet-bright stars and
galaxies to constrain the history of star formation and galaxy evolution back to a redshift of 2. It
will also conduct a number of deeper probes over smaller areas. GALEX will provide images and
intermediate-resolution spectra of ultraviolet-bright objects in both near- and far-ultraviolet
bandpasses. The GALEX Project at JPL (http://www.galex.caltech.edu) will release its data
in three stages: an initial (‘samplers’) Data Release 0 (DR-0) in September 2003, a DR-1 perhaps
in late summer of 2004, and a DR-2 at the end of the mission, some 29 months after launch.
MAST will be the sole host of GALEX data and serve them at the http://archive.stsci.edu/galex.
At this writing, the site is populated with a limited amount of simulated data to allow users to

20 
become familiar with it. Initially the site will allow the retrieval and browsing of specific data
sets, but we expect its primary use to be to permit complex queries (either by point-and-click
or Structured Query Language) as well as cross-correlations with Sloan Digital Sky Survey data.
By the time of DR-0, we expect to provide the on-line overplotting capability of “ION” (IDL On
Line). We look forward to your exercising this system and becoming skillful in manipulating
GALEX data in the coming months. Ω
Supernova Shock Wave Paints
Cosmic Portrait
R
emnants from a star that exploded thousands of years ago created a celestial abstract portrait, as
captured in this NASA Hubble Space Telescope image of the Pencil Nebula. Officially known as NGC
2736, the Pencil Nebula is part of the huge Vela supernova remnant, located in the southern
constellation Vela. Discovered by Sir John Herschel in the 1840s, the nebula's linear appearance
triggered its popular name. The nebula's shape suggests that it is part of the supernova shock wave that
recently encountered a region of dense gas. It is this interaction that causes the nebula to glow,
appearing like a rippled sheet.
Image Credit: NASA and The Hubble Heritage Team (STScI/AURA)
Acknowledgment: W. Blair (JHU) and D. Malin (David Malin Images)

21 
Starburst99 & Mappings
—A Perfect Match
Claus Leitherer, leitherer@stsci.edu
T
he Starburst99 evolutionary synthesis code (Leitherer et al. 1999) and its associated
website at http://www.stsci.edu/science/starburst99/ are premier tools for
modeling star-forming regions containing hot massive stars. Evolutionary and population
synthesis codes aim to simulate as many observed properties of resolved and
unresolved stellar populations for a predefined set of input parameters, such as the chemical
composition, the star-formation history, and the stellar initial mass function. Starburst99 is one
of several synthesis codes developed over the past decade, such as GISSEL (Bruzual & Charlot
1993), SED@ (Cerviño & Mas-Hesse 1994), Dial-A-Model (Worthey 1994), PÉGASE (Fioc &
Rocca-Volmerange 1997), Alexandre Vazdekis’ models (Vazdekis 1999), Alberto Buzzoni’s
database (Buzzoni 2002), or GALEV (Anders & Fritze-v. Alvensleben 2003), to name a few. Links
to these and other models are compiled on the website of IAU Commission 35, Stellar
Constitution, at http://iau-c35.stsci.edu. The concept of evolutionary synthesis dates back to
an influential paper by Tinsley (1968), who pioneered the field of utilizing and testing the
predictive power of stellar evolution and atmosphere models.
Figure 1: Starburst99 portal. The link to the new Mappings interface is highlighted in red.
Starburst99 is an ongoing effort at the Institute and owes its capabilities to the contributions
of numerous undergraduate and graduate students, postdocs, and collaborators. Its main focus
is on hot, massive stars and their main observables. While Starburst99 is a stellar and not a
nebular code, there is strong interest in predicting nebular star-formation tracers as well.
Star-formation indicators such as the Hα luminosity of HII regions are widely used as a proxy for
the emitted stellar light at far-ultraviolet (far UV) wavelengths (Kennicutt 1998). Predictions for nebular
recombination lines are, of course, trivial and are included in the standard Starburst99 application.
Modeling non-recombination lines, such as collisionally excited [OIII] 5007 Å is outside the
scope of Starburst99 and can only be accomplished in combination with photoionization codes.
Stasińska & Leitherer (1996) made a first attempt in linking Starburst99 to the photoionization
code PHOTO. Comparison between predicted and observed emission-line strengths in a sample
of HII galaxies suggested ionizing stellar populations with a mass spectrum with close to a
Salpeter (1955) slope. Kewley et al. (2001) fed Starburst99 into the Mappings code and pointed
out shortcomings of current stellar models when the ionizing radiation field is tested in HII
regions. Such tests are particularly revealing when the stellar content is known independently,
e.g., from UV spectroscopy. Leitherer et al. (2001) and Robert et al. (2002) discussed how the

22 
strength and in particular the blueshift of the UV stellar-wind lines can be used to infer the age
and mass spectrum of the ionizing stellar population. The underlying physical mechanism is the
tight relation between stellar-wind properties (i.e., the line shape and velocity) and luminosity,
which is an immediate consequence of a radiatively driven wind. This method has become the
standard tool to study stellar populations in the UV (Leitherer 1998). Applying this technique
and using the CLOUDY code to model the nebular lines, González Delgado et al. (2002)
discussed the potential of simultaneous nebular and stellar modeling and identified areas
requiring improvement.
We felt the time was finally ripe for developing a simple, robust, and astrophysically sound
interface between Starburst99 and a major photoionization code. We opted for Mappings
(Sutherland & Dopita 1993), both for physical and practical reasons. Mappings accounts for
thermal and non-thermal (shock) energy input, eventually allowing us to link the stellar wind and
supernova energy release predicted by Starburst99 with the Mappings shock modeling. On the practical
side, a lot of preparatory work had already been done in Lisa Kewley’s thesis, thereby minimizing our
effort spent on designing the interface code. Alternatively, Gary Ferland’s widely used CLOUDY
photoionization code (Ferland et al. 1998) would be an excellent match for Starburst99.
Starburst99 and Mappings are mature, independent codes. Therefore we decided to leave
the codes on their existing servers at the Institute and CfA and design an interface that would
provide an automatic file transfer between the two domains at http://www.stsci.edu and
http://www.-cfa.harvard.edu. A new button was added to the familiar Starburst99 portal at
the Institute, giving access to the new interface (see Figure 1). The link leads to the new Mappings
portal, where the user can specify the model parameters from the input page (Figure 2). This
initiates the calculation of a stellar spectral energy distribution with the Starburst99 code at the
Institute. Upon completion, the Starburst99 output is automatically transferred to the Mappings
Figure 2: Mappings input page. The user can interactively specify a wide range of stellar, nebular, and dust parameters.
server at CfA and a photoionization model is initialized. Once finished, the
photoionization output is returned to the Institute by ftp, and an email
notification is sent to the user. The destination directory at the Institute
Continued
page 24

23 
Starburst99
from page 23
contains both the nebular output from Mappings and the stellar spectra from Starburst99. While
this may sound quite complicated, users do not have to worry about the file transfer between the
Institute and CfA. This process occurs entirely behind the scenes. All that needs to be done is
to specify the input parameters and
wait for an email notification.
The Starburst99-Mappings interface
became fully operational in December
2002 and has since been widely used by
us and by the community at large. An
application is shown in Figure 3, where
Dopita et al. (2000) computed a grid of
diagnostic line ratios to constrain
abundances and ionization parameters
in HII regions. Those particular calculations
made use of older, unblanketed Wolf-Rayet
model atmospheres by Schmutz et al.
(1992), which produced an overly hard
ionizing radiation field for metal-rich
Figure 3: Diagnostic plot of [OIII]/Hb vs. [NII]/Ha.
stellar populations. In the meantime, a
Instantaneous zero-age starburst models computed with
new set of fully blanketed models has
Starburst99-Mappings. The theoretical grids of ionization
become available and was implemented
parameter and chemical abundance are shown as well
into Starburst99 (Smith et al. 2002).
(Dopita et al. 2000).
With this upgrade, Starburst99 uses
the most advanced stellar model
atmospheres currently available for
massive, hot stars. We are particularly excited about the prospects of using Starburst99Mappings for the interpretation of infrared spectra of dust-embedded starbursts that will be
provided by the upcoming SIRTF mission. Ω
Acknowledgements
Julia Chen’s expertise in developing the Starburst99™-Mappings interface is deeply appreciated. My
collaborator Lisa Kewley supported the back-end work at CfA and provided expert advice on issues
related to photoionization modeling. We are grateful to the Institute computer support, whose friendly
staff helped us overcome numerous roadblocks. This work was made possible by funding from the
Director’s Discretionary Research Fund.
References
Anders, P., & Fritze-v. Alvensleben, U. 2003, A&A, 401, 1063
Bruzual A, G., & Charlot, S. 1993, ApJ, 405, 538
Buzzoni, A. 2002, AJ, 123, 1188
Cerviño, M., & Mas-Hesse, J. M. 1994, A&A, 284, 749
Dopita, M. A., Groves, B. A., Sutherland, R. S., & Kewley,
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Dopita, M. A., Kewley, L. J., Heisler, C. A., & Sutherland,
R. S. 2000, ApJ, 542, 224
Ferland, G. J., Korista, K. T., Verner, D. A., Ferguson, J.
W., Kingdon, J. B., & Verner, E. M. 1998, PASP, 110, 761
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González Delgado, R. M., Leitherer, C., Stasińska, G., &
Heckman, T. M. 2002, ApJ, 580, 824
Kennicutt, R. C. 1998, ARA&A, 36, 189
Kewley, L. J., Dopita, M. A., Sutherland, R. S., Heisler,
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Leitherer, C. 1998, in Stellar Astrophysics for the Local
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A Surprise from the
Andromeda Halo
Thomas Brown, tbrown@stsci.edu
O
ur textbook concept of giant spiral galaxies is largely driven by our own Milky Way,
which has an old 1, metal-poor 2 halo of stars, and a younger 3, chemically-enriched 4
stellar disk. However, within the Local Group of galaxies, the Andromeda galaxy offers
an important contrast to this picture. Although it is of similar size and Hubble type to
the Milky Way, its halo population has a relatively high metallicity 5, as indicated by the colors of
its bright red giant stars. These stars offer a good indication of the halo's metallicity, but they
tell us little about its age distribution. Thus, without better
evidence, the Andromeda halo was assumed to be an old
population that underwent more rapid chemical enrichment
than the halo of the Milky Way. Accurate ages for stellar
populations come from photometry reaching the subgiant
branch and main sequence, but these fainter stars have always
been beyond the reach of both space-based and ground-based
telescopes. However, with the installation of the Advanced
Camera for Surveys (ACS) in 2002, we can now resolve these
stars in an observing program of reasonable duration.
Early in the proposal process, we realized that a detailed
observing strategy would be critical to the success of this
project. We first considered the required exposure depth.
Some team members wanted to resolve stars two
magnitudes below an old main sequence turnoff, because
that is the level used historically to determine accurate ages
in Galactic globular clusters. The halo population of a giant
galaxy would be more complicated than that of a globular
cluster (where all the stars are the same age and chemical
composition), so it made sense that one would want photometry
at least as deep as that used to study star clusters. However,
the hundreds of Hubble orbits needed to reach that depth
seemed unreasonable, even for a scientific goal we felt to be
very important. Instead, we chose a goal of 1.5 mag below
the turnoff and decided that a large sample of stars could
compensate for depth. While accurate photometry requires
that images have no more than one star per tens of resolution
elements, with the large ACS format we could still comfortably
include hundreds of thousands of stars in our halo images.
Figure 1: A 25.5 by 36.4 arcsecond subsection of an ACS image
We produced artificial ACS images realistically simulating a
showing distant background galaxies through the Andromeda halo.
broad range of conditions: the effects of the Hubble
point-spread function, sky background, detector noise, and
various stellar population mixes. From these simulations, we
found the level of crowding where we could blindly recover our input population from the
photometry. This level of crowding defined a limiting elliptical annulus around Andromeda. We
then picked a field along the southeast minor axis within this annulus that also included the
globular cluster GC312, thus enabling a secondary goal of studying the age of Andromeda's halo
relative to that of one of its clusters.
A review of previous Hubble imaging of the chosen field 6 ensured accurate predictions of the
crowding. Because we were concerned about the systematic errors that might be introduced by
1
2
3
4
5
6
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Continued
page 26
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using a new Hubble camera, we included images of five Galactic globular clusters with the same
ACS filters in order to produce empirical isochrones of old stellar populations, and to calibrate
the theoretical isochrones, which could be used to model younger populations.
The observations of our Galactic clusters were scattered over the second half of 2002, while
the main program in Andromeda executed from 2 Dec 2002 to 11 Jan 2003, obtaining 250
exposures with a total integration time of 3.5 days. The final drizzled images are beautiful
(Figure 1), showing thousands of
background galaxies through a
veil of ~300,000 stars in the halo
of Andromeda.
The big surprise came from
comparisons of our Andromeda
color-magnitude diagram to those
of the clusters. These show that
the Andromeda halo population
spans a wide range in both
metallicity and age (Figure 2). The
metal-poor stars Andromeda are
about as old as the stars in M92 (13
Gyr), but those at higher metallicity
in Andromeda are younger than
those in the clusters. The age
spread is indicated by the subgiant
branch and main sequence turnoff,
which are increasingly brighter in
Andromeda than those in the clusters
as one moves to higher metallicity.
To quantify this further, we
used the cluster data to calibrate
a library of isochrones7 in the
Hubble bandpasses and then fit
the Andromeda data using the
Figure 2. Left panel: The color-magnitude diagram of the Andromeda halo as observed with the
ACS. Completeness limits are marked (the data are 50% complete at Johnson V = 30.7 mag).
StarFish code8. This code takes
Right panel: Comparison to the ridge lines of five Galactic globular clusters shows that the metal-rich
the isochrones, scatters them to
populations in Andromeda are significantly younger than those in the clusters.
match the photometric errors in
the data, and then tries to
reproduce the data using a linear
combination of the isochrones. We find that no combination of old isochrones (11.5 to 13.5 Gyr)
can reproduce the Andromeda data. Instead, a wide range in age (6 to 13.5 Gyr) is required. The
best-fit model puts approximately 30% of the Andromeda halo at young ages (6 to 8 Gyr) and high
metallicity ([Fe/H] > -0.5).
Because the gas in a young giant galaxy rapidly falls into the disk, it seems very unlikely that
this newly revealed intermediate-age population can be explained by star formation continuing
unassisted in the halo for more than 6 Gyr. A more plausible explanation is a merger with a large
satellite galaxy when the universe was approximately half of its present age—or a series of
mergers with smaller satellites. The resulting halo would be a mix of stars originally formed in
the halo, disrupted disk stars, disrupted satellite stars, and stars formed during the merger(s).
It remains to be seen whether halos typically form in a relatively quiescent process, like that in
our own Galaxy, or a violent one, like that in Andromeda. Ω
Andromedea Halo
from page 25
7
8

26 
VandenBerg, D.A., & Clem, J.L. 2003, AJ, in press.
Harris, J., & Zaritsky, D. 2001, ApJS, 136, 25
The Omega Nebula
R
esembling the fury of a raging sea, this image actually shows a
bubbly ocean of glowing hydrogen gas and small amounts of
other elements such as oxygen and sulfur.
The photograph, taken by NASA's Hubble Space Telescope,
captures a small region within M17, a hotbed of star formation. M17,
also known as the Omega or Swan Nebula, is located about 5,500
light-years away in the constellation Sagittarius.
Credit: NASA, ESA and J. Hester (ASU)
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ST-ECF
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The current members of the Space Telescope Users Committee (STUC) are:
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Debbie Elmegreen, (CHAIR)
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Martin Elvis, Harvard-Smithsonian
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Astronomy
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Laboratory
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T
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
27 
Contents:
Calendar
Cycle 12
Cycle 12 Results . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .1
Cycle 12: TAC and Panel Members . . . . . . . . . . . . . . . . . .5
Cycle 12: Statistics . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .6
Cycle 12: Approved Observing Programs . . . . . . . . . . . . . .8
JWST Science Working Group at the Institute . . . . . . . . . . . . . . .October 1-2, 2003
STUC at Institute . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .November 6-7, 2003
Institute News
Director’s Perspective . . . . . . . . . . . . . . . . . . . . . . . . . . . .2
Hubble Fellowship Program . . . . . . . . . . . . . . . . . . . . . . .15
The Local Group: The Universe in a Nutshell . . . . . . . . . . .16
Advances with ACS . . . . . . . . . . . . . . . . . . . . . . . . . . . .17
JWST Mission Replan . . . . . . . . . . . . . . . . . . . . . . . . . . .19
MAST News at STScI . . . . . . . . . . . . . . . . . . . . . . . . . . .19
Institute Science
Starburst99 & Mappings—A Perfect Match . . . . . . . . . . .22
A Surprise from the Andromeda Halo . . . . . . . . . . . . . . . .25
Contact STScI . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .27
Calendar . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .28
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