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A N N U A L
R E P O R T
|
2000
the union of separate strengths
syn•er•gism — to achieve a greater reality
Space Telescope
Science Institute
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2000
Views | 3
News | 7
R e v i e w s | 15
Director’s Office | 16
Strategic Planning | 17
Program Management | 17
Development, Technology, and Innovation Projects | 17
Strategic Communications | 18
Missions Directorate | 19
Hubble Division | 20
Archive, Catalogs, and Data Services Division | 25
Next Generation Space Telescope Division | 26
Engineering and Software Services Division | 28
Administration Division | 33
Computing and Information Services Division | 35
Science Directorate | 38
Science Division | 39
Science Policies Division | 40
Office of Public Outreach | 41
S c i e n c e p u b l i c a t i o n s L i s t | 44
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f r o m
t h e
d i r e c t o r
1
T
he Hubble Space Telescope was the first of NASA’s ‘Great
Observatories.’ The Great Observatories, including Hubble,
the Compton Gamma Ray Observatory, the Chandra X-Ray
Observatory, and the Space Infrared Telescope Facility, were
meant to operate together, viewing the sky through complementary spectral windows and studying different aspects of
complex phenomena. Ten years after Hubble’s launch, the power
of this idea appears in many multispectral and multimission
observations that involved contributions from Hubble. In the
coming decade, Hubble will join forces with the Next Generation
Space Telescope (NGST) to increase its power even further.
It is now common in science for
By continually emphasizing the need to combine
diverse approaches to supply complementary pieces of a puzzle, fitting
together for scientific progress. Last
year, Hubble and the Chandra X-Ray
Observatory won kudos for their com-
collabor ation
Director ’s Foreword
our diverse talents in every aspect of our work, we will achieve the
collaboration needed to make all of our missions successful.
bined discovery that supermassive
black holes may exist in centers of most
if not all galaxies. Similarly, sources of
Synergism—the union of separate strengths to achieve a reality more than the
bursts of gamma rays have been known
parts—was an Institute theme in the year 2000 and will be our major challenge for
since the 1960’s, when they were
the next several years. It was at work in our science collaborations, our reorganiza-
discovered accidentally by satellites
tion to operate multiple missions, our efforts to optimize Hubble and NGST, and our
monitoring nuclear tests on Earth, but
archive of astronomical data from many sources. This union is simple in concept,
their origin remained unknown until
yet it is difficult to harness the diversity in a large organization such as ours to benefit
three years ago. Then, a combination
our mission and support the astronomical community. By continually emphasizing
of an Italian satellite called Beppo-Sax
the need to combine our diverse talents in every aspect of our work, we will achieve
with the William Herschel Telescope,
the collaboration needed to make all of our missions successful.
the Keck Observatory, and Hubble
solved the mystery, showing that they
came from objects in very distant galaxies
when the universe was less than half
its present age. The discovery that the
universe is accelerating relied on combining observations at ground-based
observatories, which found distant
supernovae and got their spectra, with
Hubble images, which measured
accurately the supernovae brightnesses
as they waxed and waned. These
examples of Hubble’s collaborative
The Institute’s Annual Report for 2000 shows you how our organization and staff
have worked together on behalf of our stakeholders on many fronts, with the Hubble
instrument teams, with Hubble researchers, with NASA and ESA, and with educators
and the news media to produce discoveries with Hubble and bring them to classrooms
and homes. It also provides a snapshot of astronomy at the turn of the millennium.
The Views section offers a perspective on the changing character of astronomy as a
professional activity. The News items showcase personalities, events, and science.
The Reviews section presents a report from the organizational units at the Institute,
including a mission statement, a basic description of the work, and important achieve-
ments of the last year. We hope you find our Annual Report interesting and informative. Most particularly, we hope you find that the Institute is harnessing the benefits
of diversity with good effect for the advancement of knowledge.
strength portend synergy with SIRTF
Steven Beckwith
in 2002 and NGST in 2009.
Baltimore, Maryland | 6 March 2001
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3
Astronomy
in the 21st Century
N
ow is a good time to be an astronomer. Investment in
astronomy is large and growing, from both private and public
sources. The generosity of private donors, such as the Keck Foundation
and the Research Corporation, and public support for projects like
Gemini and the VLT have created a revolution in ground-based astronomy. Strong backing at NASA, ESA, and the Japanese space agency
has produced a similar revolution in space astronomy. Never have
astronomers had access to more state-of-the-art observing
facilities. These developments have been helped by the remarkable
success of the Hubble Space Telescope. The impacts of Hubble on
science—and on public awareness of science—have helped convince
the sponsors of astronomy that their support will be repaid many
times over in pushing back the limits of our knowledge
about the universe.
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It is through scientifically motivated Institutes such as ours that scientists can guide the nature of big
projects so that the spark of individual creativity can flourish after the project is built.
it’s
here is a trend toward larger
projects. Science projects, like
young galaxies, have undergone
hierarchical clustering. Many of the
small exploratory projects have been
done, and the natural tendency is to
increase the size or capability of our
instruments. We are on the threshold
of building facilities to answer very
old questions. These questions include,
how did the universe look when the
first stars and galaxies were created?
And, have other planetary systems
given rise to life? To address these
questions, we need new telescopes of
unprecedented scale, and we must
learn how to build them, even if they
are technically daunting.
Such great investments in telescopes
call for corresponding investments in
scientists to define the facilities and
use them wisely. Indeed, the opportunities for young scientists today are
good and getting better. Most young
astronomers are finding secure research
or teaching positions; the best have
several choices. The problem, if there
is one, lies in the changing relationship
between the individual scientist and
the ever-larger scale of research facilities.
The challenge of this trend is to
preserve the individual creativity stimulated by small-scale science, while
taking advantage of the techniques of
large-scale organization to build and
operate major facilities. Culturally,
astronomy is in a better position to
meet this challenge than, for example,
high-energy physics has been. Our
large facilities enable hundreds of
individual projects each year. The
T
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Big Time
Hubble program provides money along
with the telescope time, allowing investigators to get all the support they need
with one proposal—support that now
includes time at NOAO and on Chandra,
based on time-sharing agreements we
have with those facilities. The majority
of science done with our observing
facilities is of the small sort, involving a
few researchers working creatively to solve
the problems of most interest to them.
Perhaps the most difficult challenge
will be to educate the next generation
of instrument scientists, since use of
shared facilities does not teach the skills
needed to build them.
There are passionate debates on
the merits of this culture shift, and
there are clearly some advantages and
disadvantages to its long-term impact
on science. Yet, it seems inevitable that
we must understand how to do largescale science and learn to manage the
consequences. The frontier has moved
farther away. The next frontier needs
large-scale organization to be conquered.
Two hundred years ago, there were still
unexplored regions on Earth that could
be breached by a few people in canoes
or on foot. Those days are gone forever.
The Space Telescope Science
Institute enables small science by taking
responsibility for the many routine
tasks needed to make the observations.
We do not do your science; we enable
you to do your science. It is no longer
necessary for many observers to learn
technical details of their trade in the
same manner as past generations,
who often needed engineering and fabrication skills, not to mention physical
stamina, just to get the data. Hubble
users can spend their time planning
their observations and interpreting the
results. The consequence is for scientists
to become more specialized and to rely
increasingly on other people to enable
the research enterprise.
The purpose of the Institute is to
let scientists set the major directions
for large efforts while continuing to
support the small groups that stimulate
individual creativity. We take this role
seriously, especially the need to make it
easy for individual scientists to get the
support they need to carry out research.
Our grants program is one of the
largest in astronomy. We made available
$22 M for support of Hubble observations, fellowships, and related research
last year. This amount will grow in
the coming years to accommodate the
increasing data rates from new instruments to be installed on Hubble.
For the last seven years, we have
continually lowered the cost of Hubble
operations while increasing the grants
budget at a rate above inflation to meet
growing user needs as the data rates
become higher. Even while we reduced
the number of people needed to schedule Hubble observations, we nearly
doubled the observing efficiency of the
telescope. Our response time to targets
of opportunity is now as short as 48
hours, compared to a few weeks earlier
in the program.
Many of our projects are aimed
at making it easier for scientists to use
Institute services while reducing the
long-term costs to the government. For
example, our Astronomer’s Proposal
Tools project will make proposal preparation and observation planning easier
through the use of visually intuitive
interfaces. Grant management is now
done electronically through our new
Grants Management System interface,
making it easier for both users and
administrators to request and track
research funding. By themselves, such
innovations may not produce new
science directly, yet they have the positive effect of unburdening individual
scientists of details that have little to
do with research.
More importantly, we represent
the community in the enterprise of
constructing large astronomical facilities in space. The Next Generation
Space Telescope requires many daily
decisions about the way it is constructed
and how it will be operated. These
decisions shape the future of the facility
in the same way that individual scientists once determined the destiny of
their own experiments by hand. It is
truly big science to undertake a large
project and ensure that it is optimized
for its intended purpose. It is through
scientifically motivated Institutes such
as ours that scientists can guide the
nature of big projects so that the spark
of individual creativity can flourish
after the project is built.
5
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New Manager
Professional Profile
proud to
serve
Community Service
In keeping with AURA expectations, Institute staff serve the national and
international communities in many ways beyond the operation of our
observatories. They serve on advisory committees, science working groups,
review panels, and as officers of professional societies. In roles large and
small, formal and informal, Institute staff strive to be good citizens of the
science community.
In 2000, our staff members served the National Academy of Sciences’s
National Research Council as members of the Space Studies Board, the
Committee on Planetary Exploration, and the Astronomy and Astrophysics
Survey Committee (the Decadal Survey), including chairing the Panel on
Ultraviolet, Optical, Infrared, and Radio Astronomy from Space.
They served on numerous NASA committees and panels. Last year,
these included the Origins Subcommittee of the Space Science Advisory
Committee, the Mars Climate Orbiter Mishap Investigation Board, the
Planetary Atmospheres Program Review Panel, the review panel for the Long
Term Space Astrophysics and Astrophysics Data Programs, the Astrophysics
Senior Review Committee, and the SIRTF Science Center Oversight
Committee. They chaired a Terrestrial Planet Finder Architecture Study
science team, the 2 Micron All Sky Survey (2MASS) External Review Board,
the Astrophysics Data Centers Coordinating Council, and the Second NASA
Panel for the Non-Advocate Review of Ground-Based IR Interferometry for
Detecting Exozodiacal Dust.
They participated on users committees and time allocation committees
of many other observatories, including NOAO, NRAO, Chandra, and
NASA/Keck.
They served as officers or committee members in professional organizations, including the American Astronomical Society, the International
Astronomical Union, the American Association for the Advancement of
Science, and the Optical Society of America. Many staff members provided
other professional services as members or leaders of organizing committees
for major professional meetings, as reviewers of proposals to NASA and
NSF, and as reviewers of research papers for the leading journals.
Institute staff are proud of their many
opportunities to serve astronomy and the astronomical
community on a personal basis.
7
Henry Ferguson
Henry (Harry) Ferguson is the new Head
of the Science Instrument Support
Department. Harry's formative years were
spent in New York and New England,
although for three years he lived in India,
where he developed life-long interests
in music and in other cultures. His interest in astronomy began at an early age,
and as a teenager he spent many nights
observing Messier objects, variable stars,
and meteor showers. He obtained his
undergraduate degree in Astronomy and
Astrophysics from Harvard University,
where he worked as a research assistant
on the Einstein Observatory and also
led the percussion section of the “marching” band.
After a year teaching high-school
physics, Harry enrolled as a graduate
student in Physics and Astronomy at
The Johns Hopkins University. There he
became heavily involved in the Hopkins
Ultraviolet Telescope (HUT) project,
writing much of the ground-support software and assisting in the calibration of
the detector and gratings. He was gearing up do his thesis on observations of
elliptical galaxies with HUT when the
Challenger shuttle explosion put the
mission on hold. Harry retooled himself
as a ground-based astronomer and
undertook a study of dwarf galaxies in
nearby clusters with visiting professor
Allan Sandage.
From Hopkins, Harry moved to
Cambridge, England, for postdoctoral
fellowship at the Institute of Astronomy,
where his interest in dwarf galaxies led
him to explore possible solutions to the
“faint blue galaxy” problem. He also spent
much of his time commuting back to
the United States for repeated attempts
to launch HUT and for collaborations on
reducing and interpreting HUT results
from the successful 1990 flight on the
Space Shuttle.
Harry returned to the US in 1993,
spent two years as a Hubble Fellow at
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Professional Profile
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Antonella Nota
Antonella Nota, the Deputy Head of the
Science Division, was born and raised
in Venice, Italy. Her love of astronomy
started very early. As a teenager, she
was one of the first women to join the
American Association of Variable Star
Observers in Europe and monitored
variable stars for years from the Lido in
Venice. She completed her university
studies at the Institute of Astronomy of
the University of Padua, home of Galileo.
She worked at the Italian Aerospace
Company LABEN where she participated
in the initial design of the Beppo-Sax
mission. Later she moved to Darmstadt,
Germany, where she spent almost two
years providing scientific support for
the Exosat x-ray astronomy mission.
Antonella joined the Institute in
1986, as a member of the science
team for the Faint Object Camera. She
became a member of the ESA staff in
1990. She spent ten years supporting
Hubble instrument science operations,
taking on increasingly challenging
management positions, as Lead of the
Faint Object Camera Group, Lead of
the Observatory Support Group, and
Lead of the NICMOS Group. Recently,
she has taken on a new challenge as
Deputy Head of the newly formed
Science Division.
Antonella’s scientific interests are
mainly in the field of post main sequence
evolution of very massive stars, especially Luminous Blue Variables and
Ofpe/WN9 stars. She has studied the
nebulae ejected by these stars and used
the nebular properties to constrain the
ejection mechanism and to refine the
understanding of the last evolutionary
phases of these very luminous and
massive objects. More recently, she has
developed an interest in the stellar function of young star clusters, especially at
very low masses.
Outside astronomy, Antonella has
many interests, including modern art
and classical music. She loves extreme
sports and spends her vacations scuba
diving in remote areas of the world,
parachuting, or skiing. She is married to
Mark Clampin, an astronomer colleague
whom she met at the Institute. They
have a six-month-old daughter, Simona.
bravo
Hubble Heritage Wins Award
The Institute’s Hubble Heritage Project has received the Infinity 2000
Award for Applied Photography from the International Center of
Photography (ICP) in New York City. The award cited Hubble Heritage’s
purpose, “to mine the scientific observations to create breathtaking
images intended to both inform and inspire,” and noted that Hubble
imagery has “stimulated the global public’s contemplation of the cosmic
in emotional and philosophical ways.”
The mission of the ICP is “to present photography’s vital and central
place in contemporary culture, and to lead in interpreting issues central
to its development.” The ICP’s Infinity Awards “celebrate the infinite
potential of the photographic medium.” The selection of Hubble
Heritage was announced at the 16th annual awards ceremony, which
took place in New York City on May 11.
The Applied Photography category of the Infinity Awards encompasses architectural, fashion, and
scientific photography. Past winners of this award include some of the biggest names in photography, like
Annie Leibovitz, whose work has appeared in Rolling Stone, Vogue and Vanity Fair.
The Hubble Heritage team consists of astronomers and technical experts whose goal is to produce
beautiful and compelling images. Hubble Heritage Program Scientist Keith Noll says, “We plan all our
observations keeping in mind the immense scientific value of Hubble images. We want the end products
to be both beautiful images and research papers, and this has already happened.”
The Hubble Heritage website is http://heritage.stsci.edu, and the ICP’s is http://www.icp.org.
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Kudos on
Hubble’s Ten
Years in Space
On April 24, 1990, a spectacular morning
launch of the Space Shuttle Discovery ushered in
a new era of astronomy. The payload in Discovery’s
cargo bay, NASA’s Hubble Space Telescope, was released by the
crew into Earth orbit the next day. Initially impaired by a flaw
in its main mirror, Hubble’s position above the distortion of
Earth’s atmosphere enabled it to begin making discoveries
even before astronauts repaired it in 1993. When corrective
optics were installed during that dramatic first servicing
mission, the universe snapped into sharp focus, and there
followed a flood of spectacular images and discoveries,
which have forever changed how we view the cosmos.
In its first ten years, Hubble studied 13,670 objects,
made 271,000 individual observations, and returned
7 terabytes of data. Its scientific achievements resulted in
over 2,651 scientific papers.
Many voices strove for fresh superlatives in praising
Hubble on its 10th birthday, including the following
from various quarters.
“The breadth of Hubble’s achievements is just
staggering,” said Wendy Freedman of the Carnegie
Observatories in Pasadena, California. “Hubble increased
the volume of space we could see by a factor of 1,000.”
“No one imagined that HST would get us this far in
understanding galaxy morphology,” said Dr. Alan Dressler,
also of the Carnegie Observatories.
“This month marks the anniversary of one of the
greatest observatories ever flown. We have watched in awe
as the Hubble Space Telescope has produced some of the
most amazing images about the universe that surrounds
us,” said Sen. Barbara A. Mikulski (D-MD). “I am so proud
of the NASA team that has worked to keep it running
and I’m pleased my support has kept your efforts funded
and in business.”
“Hubble’s rate of discovery is simply unprecedented
for any single observatory,” said Dr. Ed Weiler, Associate
Administrator for Space Science, NASA Headquarters,
Washington, DC, who has been associated with the
Hubble program since 1978.
“But what may be even more important
in the long term is what Hubble has given
to just about everyone on Earth.
Hubble’s spectacular images and discoveries of black holes,
colliding galaxies and bizarre objects at the edge of the
universe have been brought into millions of homes by
newspapers, television, and the Internet.”
Henry Ferguson | continued from page 7
10
the Institute, and joined the staff in
1995. He began in the WFPC2 Group,
but soon joined the STIS Group and led
the orbital verification program, which
was carried out jointly by the Institute
and the instrument development team.
Harry was in charge of STIS calibration
for two years before becoming Deputy
Project Scientist in the NGST group
in 1999. There he undertook a number
of studies to firm up the scientific
requirements for NGST, and to develop
concepts for operating it. He also served
as a liaison to the Ad-hoc Science
Working Group.
Harry's research interests in faint
galaxies led to an involvement in the
Hubble Deep Field (HDF) projects. In
1995 and again in 1998, Hubble took
very deep exposures of representative
patches of sky, one in the northern and
one in the southern hemisphere. Harry
coordinated the overall Institute effort
for both campaigns, from planning
through the release of the data. He has
since focused much of his research
on interpretation of the HDF data. He
has used the data variously to rule out
certain evolutionary models for dwarf
galaxies motivated by the Cold Dark
Matter theory, to set limits on the number of low surface brightness galaxies
present in the low redshift universe,
and to search for intergalactic stars
using HDF as a control field. Harry’s
discovery of intergalactic stars in the
Virgo Cluster earned him the AURA
science award in 1997. Harry continues
his broad attack on problems of galaxy
evolution with active Hubble observing
programs on dwarf elliptical galaxies,
spiral galaxy halos, and hot horizontal
branch stars in elliptical galaxies. He
is a co-investigator on the Great Observatories Origins Deep Survey SIRTF
Legacy project, which aims to measure
the mass assembly history of galaxies
over the last 10 billion years. Harry also
contributes to a survey project at the
National Optical Astronomy Observatories
to improve our understanding of the
relation between star formation and the
neutral gas content in nearby galaxies.
While in graduate school, Harry set
down his drumsticks and took up the
hammered dulcimer. He and his wife
Meg (guitar) and Institute colleague Ray
Lucas (fiddle) can be found from time
to time around Baltimore performing
traditional Celtic music.
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David Hunter
David Hunter, the Institute’s Project
Manager for the Next Generation Space
Telescope (NGST), spent his childhood
in Scotland before moving to Canada in
1967. Fascinated by space from an early
age, he obtained a degree in Aerospace
Engineering from the University of
Toronto. Uncertain in which field to specialize he passed up a scholarship for
graduate school and spent the following
summer teaching computer programming and mathematics at St. Lawrence
College in Brockville. Thereafter, he
joined the Communications Research
Center in Ottawa in the position of
Satellite Dynamics Engineer.
The six and a half years that David
spent at the Communications Research
Center proved to be formative for his
life and career. While about half of his
time was consumed developing a
remotely controlled system to measure
mass properties for the Olympus spacecraft of the European Space Agency, the
mandate of the Center enabled him to
explore other fields of interest. He developed orbit analysis software, performed
studies in structural dynamics, developed
a control system for the Space Shuttle
for the Waves in Space Plasmas experiment, and conducted research in neural
networks and robotics. Outside of work,
life was becoming equally interesting. In
1983, he met Maureen Hunt whom he
would later marry. Together, they bought
a turn-of-the-century row house and
proceeded to gut and remodel it.
In 1988, David became the departmental liaison to the Space Station
Program at the National Research
Council of Canada and in 1989 joined
the program full time. At the National
Research Council, he was responsible
for the robotic aspects of the Mobile
Servicing System, a successor to the
shuttle Remote Manipulator, which is
the Canadian contribution to the Space
Station. In this capacity, he led the
development of the Special Purpose
Dexterous Manipulator—a two-arm
robot designed to repair the Space
Station. While the Hubble mission had
pioneered the design of spacecraft to
be serviceable by astronauts, designing
the Space Station to be serviceable by
robots was breaking new ground. David
worked closely with industry and with
the United States and Japanese space
agencies to develop a robotic-maintenance architecture for the Space Station
and a manipulator system that could
perform the required repair operations.
In 1990, the Canadian Space
Agency (CSA) was formed, and it was
announced that the Space Station
Program would be relocated to the new
space agency headquarters in Montreal.
Life in Montreal proved to be both
culturally rich and politically tumultuous.
The Parti Québécois came to power
in 1994 and brought the province to
the brink of separation from Canada.
The Space Station Program was no less
turbulent, and it endured a period of
fluctuating budgets and rescopes. At
CSA, David soon became Manager of
Systems Engineering and responsible
for control systems, simulations, flight
software, the control station, the Space
Vision System, the robotic task verification facility—and of course systems
engineering. The Space Vision System
became standard equipment for Shuttle
docking and assembly operations.
(The black dots on the space station are
targets used by the Vision System to
enable the astronauts to align precisely
the modules and structures they install.)
In 1993, David was selected as the
Canadian representative to the International Advanced Robotics Programme,
a position he held until he moved to
Baltimore to join the Institute in 1999.
David went on to serve as Deputy
Project Manager and Acting Project
Manager for the Mobile Servicing
System and Acting Director of Systems
Engineering for CSA. In the latter position he was responsible for the overall
engineering of the major CSA missions.
He now eagerly anticipates the launch of
the first element of the Mobile Servicing
System, scheduled for April 2001.
Reflecting on his current position,
David comments, “Space Station was
rewarding because there was always
a new challenge and a new project to
tackle. Usually we were trying to do
something that had never been done
before while trying to meet budgetary
constraints. NGST looks to me like it is
going to be similar.”
fig 1
The central region of the starburst galaxy NGC5253 is
shown in the light of Hα (~6563Å) [red] and ultraviolet
(~2600Å) [blue]. The images are from the Hubble
WFPC2, with north up and east left. The two-color
picture highlights the complex morphology of the starburst,
where the Hα emission traces not only the most recent star
formation, but also galactic-scale ejecta from the evolving
massive stars. The ultraviolet emission traces star formation over timescales of a few hundred million years and
is not exactly co-spatial with the Hα emission. Images like
this one show clearly that the evolution of a starburst
cannot be simply described as the aging of a single stellar
population; a starburst comprises a wide range of components of different ages, actively interacting with the
surrounding medium.
fig 2
The central region of the starburst galaxy M83,
the massive companion of NGC5253, is shown
in the ultraviolet (~3000Å), V-band (~5500Å),
and I-band (~8000Å) light. The images are
from the Hubble WFPC2, with north up and
east left. The site of the recent star formation
forms a blue half-ring of small knots and diffuse
light centered on the red nucleus. A prominent
dust lane cuts the western side of the ring
from north to south.
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11
Unveiling Star Formation
espite the many advances in astrophysics and cosmology
over the past decade, there is one fundamental aspect
of the physics of galaxies for which we still lack a basic quantitative understanding: star formation. Not yet unveiled are
the mechanisms that regulate star formation and the duration
of a star forming event, the duty cycle of star formation, its
spatial and temporal evolution, and, finally, the interplay and
feedback between star formation and the surrounding interstellar medium.
Addressing these issues is of critical importance for
understanding the star formation and heavy element enrichment
histories of the universe, the nature of galaxies at all redshifts,
and their evolution on cosmological timescales. For instance,
whether the actively star forming galaxies at high redshift are
building the bulk of their stellar populations or a relatively
insignificant number of stars depends on whether starbursts
have long or short durations.
Starburst galaxies (galaxies undergoing a major star
formation event in their centers) are ideal laboratories for
tackling the questions above, as they provide optimal conditions for investigating the production of stars on galactic
scales. To disentangle the spatial and temporal evolution of
starbursts, we turn to the nearest galaxies, where high spatial
resolution can be achieved with the Hubble Space Telescope.
In addition, the ultraviolet capabilities of Hubble enable the
study of the hot, ionizing stars, the most prominent product
of a starburst, in the wavelength range where they emit the
bulk of their energy.
The two galaxies M83 and NGC5253 form a nearby
massive dwarf pair in the Centaurus Group. Details as small
as the typical size
of stellar clusters
can be resolved
by Hubble’s Wide
Field Planetary
Camera 2
(WFPC2). M83 is
a grand-design
spiral, with a mass
similar to our
Milky Way, hosting
a starburst near its
center. Its companion is an amorphous dwarf about 100
times less massive; it hosts a comparably intense starburst
near its center. A past interaction has been suggested as the
trigger of the central starbursts.
D
science essays
Daniela Calzetti & Jason Harris
The complex morphology of the starburst in NGC5253
is illustrated in Fig. 1, where the WFPC2 Hα and ultraviolet
images have been combined in a two-color picture. The Hα
emission of hydrogen traces the current star formation, while
the ultraviolet emission at ~2600Å traces the star formation
integrated over the last few hundred million years. By combining these tracers with longer wavelength colors and with
ultraviolet spectra, the various components of the stellar
population can be dated in nearby galaxies. It has been known
for a few years that the ultraviolet light of starbursts appears
to comprise two components: only about 20% of the emission
comes from identifiable stellar clusters and the remaining
80% originates from a diffuse stellar population. The picture
that emerges for the starburst in NGC5253 is that star formation has been on-going at a roughly constant pace for the
past ~200–500 million years. The starburst forms stellar
clusters, and the least massive clusters evaporate over timescales of ~20 million years or less. The surviving stars from
the evaporated clusters constitute the diffuse population.
Remarkably, we find that the starburst in NGC5253 has lasted
ten times longer than the duration predicted by semi-analytical
models, thus challenging current star formation theories.
While the distribution of cluster ages across the center
of NGC5253 does not follow any particular order, there is a
suggestion of propagating star formation among the clusters
in the starburst region of M83. The visible star formation in
the center of this galaxy is distributed in a circumnuclear
half-ring (Fig. 2). A dust lane crosses the north-western part
of the starburst region, likely hiding a fraction of the most
recent star formation. The clusters in M83 appear to span a
larger range of ages than those in NGC5253, up to 40 million
years old; they are also more massive. A different picture from
that of NGC5253 seems to be suggested for the evolution
of the starburst in M83. In this galaxy, the starburst began in
the south-eastern region approximately 40 million years ago
or earlier, and moved across the ring towards the north-western
regions. While pockets of star formation remain active throughout the half-ring, the most active star forming regions are
currently located toward the western end of the circumnuclear
ring. Still unclear are the fundamental mechanisms that have
determined the different evolution of the starbursts in the
two galaxies.
Hubble, with its multiwavelength capability and its
superior angular resolution, will play a fundamental role over
the next few years in our quest to understand star formation.
Our investigation has just begun with NGC5253 and M83;
by comparing the star formation histories of starbursts in a
variety of environments, we hope to shed light on the mystery
of star formation.
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The Demography of
Supermassive Black Holes
HST/WFPC2 May 1995
HST/WFPC2 Nov 2000
3
4
Roeland van der Marel
2
9
5
upermassive black holes in the centers of galaxies are
some of the most enigmatic objects in the universe. In
active galaxies and quasars, their appetite for matter provides
us with a stunning display of fireworks, including X-ray
emission, radio jets, and rapidly moving gas clouds. In normal
galaxies, starved of fuel, they lurk quiescently.
The Hubble Space Telescope has revolutionized our
knowledge of these supermassive black holes. By measuring
the motions of stars and gas in the centers of galaxies, Hubble
has not only proven their existence but also determined their
masses. The Space Telescope Imaging Spectrograph (STIS)
is particularly well suited for such studies. STIS is now allowing us to address the demography of the supermassive black
hole population.
A special session entitled “Supermassive Black Hole
Research and Advances with STIS” at the American Astronomical Society meeting in Rochester drew together
astronomers to discuss newly emerging results. Earlier reports
were confirmed that supermassive black holes may well exist
8
7
1
S
Supermassive black holes exist in the centers of many—perhaps all—galaxies.
Recent results suggest that the mass of the black hole increases with the mass of the
spheroidal bulge component of the galaxy. If the black hole is accreting material,
the galaxy is identified as an active galaxy or a quasar.
in all galaxies, and that the black hole mass correlates loosely
with the mass of the galaxy bulge. In addition, two groups
independently reported a strong correlation between the
mass of the black hole in a galaxy and the magnitude of the
random motions of its stars.
These results provide new insight into the origin of
supermassive black holes. One plausible scenario is that
galaxies and their black holes form simultaneously in an
phase that manifests itself through strong quasar activity.
This is quantitatively consistent with the statistics of quasars
in the distant universe and with the statistics of black holes
in the nearby universe.
In the coming years, further studies of supermassive
black holes using STIS will undoubtedly bring a clearer
understanding of the origin and demographics of these
remarkable objects.
11?
6
Star
Star
10?
New Collision Spots 1 - 11
True color images of SN 1987A and its inner circumstellar ring obtained with
Hubble’s Wide Field Planetary Camera 2 in May 1995 (left) and November
2000 (right). These images show that the quiescent ring has developed a number
of new hot spots in the last five years. In a few more years the entire ring will be
glowing much more brightly. [Courtesy of Peter Challis (Center for Astrophysics),
on behalf of the SINS project. (Supernova INtensive Study, PI: R.P Kirshner)]
Fireworks around Supernova 1987A
Nino Panagia
upernova 1987A exploded on 1987 February 23 in the
Large Magellanic Cloud. Although Hubble was not yet
in orbit when this rare chance to observe a nearby supernova
appeared, it took advantage of the opportunity as soon as it
became operational. The European Space Agency’s Faint Object
Camera took the first images of SN 1987A on 1990 August
23-24, which revealed the supernova crowned by a glorious
circumstellar ring. Later, two more rings were discovered.
Hubble has kept an attentive eye on SN 1987A. Hubble
observations have produced many fundamental results, including a direct measure of the supernova expansion, the detailed
properties of its surrounding rings, the distance to the supernova, and the origin of the stars associated with the supernova.
Recently, Hubble has observed the high velocity material
from the supernova explosion starting to overtake and crash
into the slower moving inner ring. The accompanying images
show the dramatic evidence of these collisions. The circumstellar ring, which until 1995 was relatively quiescent (left
panel), started to develop bright spots in 1997. In November
2000 (right panel), one can identify almost a dozen bright
spots due to interactions between the material ejected by the
supernova and the ring material. Within the decade ahead,
the full force of the supernova’s fast material will hit the
whole inner ring, heating and exciting its gas to produce a
new series of cosmic fireworks. Hubble will take pictures of
this spectacular scene until its end of life in 2010.
S
research
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Searching for Planet Transits
Ronald L. Gilliland
ix years ago, the discovery by Michel Mayor and Didier
Queloz of the very short period planet orbiting the
solar-neighborhood star 51 Peg opened a new age of extrasolar planet detections. These ground-based radial velocity
programs have now yielded over 50 planets, most of which
are Jovian scale, with orbits of a few days to now as long as
three years. Continuing these programs for a decade or more
promises to return a rich census of yet longer period planets
having Jovian masses.
The discovery of a class of ‘hot Jupiters’ was particularly
exciting. These Jovian-mass planets, which orbit very close to
the host stars, have major theoretical and practical implications. For example, it seems likely that such planets did not
form where they were found close to their host star, but that
significant orbital evolution has occurred, moving the planets
from cold formation sites far out in to their present toasty
positions. The prevalence of such large planetary migrations
—nearly 1% of stars searched by the radial velocity programs
have such gas-giant planets with orbital periods of only 3 to 5
days—was entirely unexpected.
Hot Jupiters create new observing opportunities. Because
these planets are so close to their host stars, observable transits become possible. Transits are observed when the planet
passes between the observer and the stellar disk, which is
expected 10% of the time for random orientations of 3 to 5
day orbits around solar-type stars. Such a transit will produce
a 1-2% dip in the stellar intensity, proportional to the relative
areas of the planet and star. Indeed, a photometric search
found the transiting planet of HD 209458 ‘on schedule’ in
1999, just as the count of hot Jupiters neared the point of
50% expectation for at least one system oriented for observable transits.
Monitoring stars for radial velocity variations due to
planetary companions is a painstaking endeavor. That approach
involves observing one star at a time with a state-of-the-art
spectrograph. By contrast, a search for planets via transits can
monitor a large number of stars simultaneously with widely
available imaging instruments. The most massive transit
S
relative flux
1.000
0.995
0.990
fig 2
0.985
–0.15
search to date—which also produced the most enigmatic
results—was performed in 1999 using the Wide Field Planetary
Camera 2 imager on the Hubble Space Telescope.
Principal Investigator Ronald Gilliland and his investigator
team chose to observe a tightly packed star field in the globular
cluster 47 Tucanae. The 30,000 stars they monitored are normal
stars but demographically quite
different from stars near the Sun,
due to their greater age, lower metal
content, and greater physical crowding. In the most data intensive
observation yet by Hubble, the team
obtained over 1,300 exposures of
47 Tucanae in 8.3 days to look for
hot Jupiter transits. Such a transit
would appear as a dip of a few
percent in the intensity of a star’s
image, lasting about three hours and
recurring every 3 to 5 days. The
team expected to find about 20
transiting planets if hot Jupiters
occur around globular cluster stars
at the same rate as around the stars
Mosaic of the 47 Tuc core imaged with
in our neighborhood.
Wide Field and Planetary Camera 2
formed by combining 26 U-, 636 V-, and
The team found none. The
653 I-band exposures used in the search for
many variable stars they found
planetary transits around some 30,000
(valuable in their own right)
main sequence stars.
demonstrate the superb quality of
the observations and the excellent sensitivity to transiting
planets—if they were there! It seems that the stars in the globular
cluster 47 Tucanae have at least a ten times lower chance of
having a hot Jupiter than do stars closer to the Sun.
At this time, multiple explanations are under consideration
to help explain the lack of close-in planets in 47 Tucanae. The
lower heavy element abundance may work against the initial
nucleation process of planet coalescence out of protoplanetary
nebulae. During the cluster formation, when the crowded stellar
ensemble included many massive stars with prodigious radiation
and wind output, the protoplanetary nebulae may have been
disrupted. The greater gravitational interactions between the
crowded stars may disrupt planetary orbits, even cast the planets
free of their host stars. While these possible biases against globular
cluster planets were recognized before proposing the observations, none seemed sufficiently convincing to argue that planets
wouldn’t exist. Now that planets are known to be much less
common in a globular cluster, we need to understand why.
–0.10
–0.05
0.00
0.05
0.10
time from center of transit (days)
0.15
fig 1
The transit of HD 209458b, a ‘hot Jupiter’ with a 3.5 day period orbiting a
Sun-like star as observed with Hubble. Note the extreme accuracy obtained
with these observations obtained from above the Earth’s atmosphere.
[Courtesy of T. Brown, High Altitude Observatory, National Center for
Atmospheric Research.]
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re
di
15
ctor ’s offic
e
Strategic
Communications
Deputy
Director
Strategic
Planning
Director
Chief
Information
Officer
D
DT
DTI
Program
Management
Associate
Director
for Science
Head of
Administration
Computing &
Information
Services Division
s c i enc
e
di
r
ct
or
ir
e
sio
ns
d
o
ct
rate
ate
Administration
Division
Science
Division
Science
Policies
Division
Office of
Public
Outreach
Hubble
Division
mi s
Science and Instrument
strumen Support Dept.
New Instruments
nts and S
Servicing Dept.
Hubble Operation
Operations Dept.
NGST
Division
Engineering
& Software
Services Divsion
Archives, Catalogs,
& Data Services
Division
Mission and Flight
light Eng
Engineering Dept.
Ground Systems
System Dept.
Planning and Scheduling
heduling Systems Dept.
Science Usser Systtems Dept.
institute
organization
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we lead
the institute
Director ’s Office
Our responsibility is to lead the Institute. By defining the organization, strategy, policy, and management team, we support the work
of the staff and guarantee the Institute’s commitments to NASA,
the scientific community, and the public. We strive to make it easy
for everyone in the Institute to contribute their best capabilities
to our mission. We obtain the resources needed by our staff to do
their work, and we allocate them to optimize the productivity of
the Institute. We represent the Institute by conducting its external
relations, reporting to oversight committees, and receiving guidance
from advisory groups.
t the beginning of 2000, we adapted the organization to meet our
responsibility for more than one mission. The Institute continues to
operate the Hubble Space Telescope, which is NASA’s most successful
space science mission ever. We are now developing the science and mission
operations plans for the Next Generation Space Telescope (NGST), which
will open an infrared window on the early universe. The data archives for
Hubble and other missions have become research engines in their own right,
and they constitute a separate division in the new organization on par with
Hubble and NGST.
To provide this variety of services with flexibility and economy of
scale, we devised an organizational structure that sharpens project responsibilities and cultivates the strengths needed to meet them.
Each of the projects in the Missions Directorate now reports to the
Deputy Director. Into the Science Directorate, we group all of our scientists
and science-based services. Most scientists report for technical work to divisions in the Missions Directorate. In this manner, science advice permeates
everything we do: operating Hubble, building NGST, and delivering the
most useful data to astronomers’ desktops.
The reorganization gave us an opportunity to examine all of our
management processes. We spent much of the year 2000 looking at our
processes for communication, delegation of authority, and budget planning
under the new structure. This work is continual, since the organization
remains fluid as the staff changes and as unforeseen issues develop with the
missions. We recruited two new top managers: Dr. Ian Griffin as the Head of
the Office of Public Outreach, and Professor Bruce Margon as the Associate
Director for Science (both starting early in 2001). We worked closely with
our counterparts in NASA to maintain good working relationships at all
levels within our projects.
A
Meeting of the Director’s Office Group
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The Hubble project suffered severe budget pressure in 2000
owing to the delay of the third servicing mission and its impact
on the schedule for subsequent missions. This budget pressure
resulted in a 10% reduction in the Hubble staff at the Institute.
The Director’s Office managed that reduction with minimal
damage to the Hubble operations, and we worked to minimize
the negative impact on staff morale. In addition to the budget
reductions, our projects have been affected by new government
rules, such as those arising from the International Traffic in Arms
Regulations, which require considerable attention to ensure that
the mission operations can function smoothly while remaining
within guidelines. We worked with the NGST Division
and the project office at Goddard Space Flight Center to make
sure that impacts on operations are included in any decisions
about the construction of NGST.
The Hubble mission is NASA and ESA’s flagship of science.
We worked to make its highly efficient operations even better
and to increase its capacity for science. By talking with observers
worldwide, we sought to understand their needs and to ensure
that their use of Hubble can maintain its preeminent position in
astronomy, which is so well evidenced today by research papers,
scientific collaborations, meeting topics, and headlines. We
stressed the importance of bringing Hubble’s discoveries to the
public, to inform and inspire all people with these scientific
advances of our culture.
The Astronomy and Astrophysics Survey Committee of the
National Research Council designated NGST as the highest
priority major initiative in the United States astronomy program
for the decade starting in 2000. The Institute undertook a major
challenge when we agreed to help NASA develop NGST. That
task will be an increasing focus of our attention in the years to
come. Our goal is to operate NGST for a fraction of the cost
of Hubble. That goal will be realized in a mission design and a
ground system concept that emphasize technical innovation,
streamlining, and simplicity. These are qualities with which we
have experience. We were able to nearly double the efficiency of
Hubble operations through software improvements and careful
organization of the scheduling team. We intend to build these
economies into the NGST efficiency by using our experience
of improving Hubble’s efficiency.
In 2000, we embarked on several new opportunities to
enable science on behalf of the community. We are working with
the Sloan Digital Sky Survey team to enable standard archiving
and public distribution of the data. We joined a community-based
group to propose the preparatory work for a National Virtual
Observatory, which is the highest priority small initiative
recommended by the Astronomy and Astrophysics Survey
Committee.
Strategic Planning
Starting in the summer of 2000, we developed a new strategic
plan for the Institute taking account of our opportunities,
proven strengths, and philosophy of partnership with the community, NASA, and ESA. The plan presents a vision for the
Institute: “To enable astronomers to explore new realms of space
and discover humankind’s place in the universe.” Our strategic
plan portrays an appropriate leadership role for the Institute,
performing the tasks it must and enabling the community to do
the many tasks it can and should. Through our synergistic
partnerships with the community and sponsoring agencies, the
Institute will help bring about a new era of scientific discovery
in space astronomy.
Program Management
Program management comprises two groups dealing with financial and resource management and one group for developing
innovative programs throughout the Institute. The Resource
Management Group leads financial and business planning activities Institute-wide. It prepares, negotiates, and administers
contract proposals, prepares and administers budgets and staffing
plans, and generates government reports such as budget variance
analyses. Our Operations Management Group provides a
managerial and programmatic liaison between divisions and the
Director’s Office. It is a focal point for managing staffing and
work plans as well as schedules and requirements. This group’s
program managers participate in process improvement activities
and lead special projects, where they promote effective integration, coordination, communication, and conflict resolution.
In early 2000, we completed the myriad details to implement the reorganization. We worked with the new division
managers to prepare individual staff assignments, budget reallocations, and internal management structures. The Institute
implemented the reorganization on schedule, which permitted
a smooth staffing readjustment in April 2000 in response to
budget pressures.
We conducted a bottom-up review of the work performed
by all Institute divisions to find areas where we might increase
efficiency and reduce cost. As a further efficiency improvement,
we installed a new suite of planning and budgeting software for
use at both the division and Institute level.
Development, Technology, and
Innovation Projects
Our goals are to engage the Institute’s expertise in new challenges
within our AURA charter.
In 2000, we defined a new Institute process for identifying
novel ideas and supporting them with appropriate resources. We
examined process improvements in several areas, including the
administrative procedures for procurement and travel and the
Hubble operations tasks of observation planning and instrument
calibration. We also investigated the benefits of incorporating
new communication technologies into conferences and meetings
that the Institute supports.
17
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O f f i c e
The Strategic Communications staff
Strategic Communications
We help provide a coherent Institute voice to the outside world.
We produce the Annual Report. We conduct studies of scientific
and technical issues to increase the value of space astronomy.
Within the Institute, we facilitate improvements of management
processes, promote more effective communications, and provide
organization support to the Director’s Office.
The Annual Report of the Space Telescope Science Institute
was delivered to AURA in April 2000 and widely distributed
within the community, including via the Internet.
(http://sco.stsci.edu/annual_reports/)
We distributed the final recommendations of the Hubble
Second Decade Committee. An earlier recommendation led to
the near-infrared channel currently under development for the
Wide Field Camera 3, which will be installed on the final
Hubble servicing mission. The final recommendations were
directed at the Hubble data archive, which is becoming a major
focus of research in its own right, and at the process for allocating Hubble observing time, which the Committee thought
should be supplemented with a ‘Hubble Treasury Program’ to
facilitate large, strategic, research projects.
(http://sso.stsci.edu/second_decade/recommendations/)
The Institute has taken the first steps in implementing the
Hubble Treasury Program by increasing the fractions of medium
and large programs approved in Cycles 9 and 10.
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we conduct
science & mission
operations
Missions Directorate
We plan, develop, and implement science and mission operations
for all missions for which the Institute is responsible. We are
currently responsible for the Hubble Space Telescope, the Next
Generation Space Telescope, the Multimission Archive at STScI,
and Engineering and Software Services
he Missions Directorate includes four divisions designed
to provide clear responsibility for managing our major
missions. We draw supporting staff, services, and products
from the expertise within the Missions Directorate and the
Science Directorate.
The Hubble Division is responsible for all science operations of the Hubble Space Telescope. The Next Generation Space
Telescope (NGST) Division is responsible for designing and
implementing the science and mission operations for NGST. The
Archive, Catalogs, and Data Services Division provides pipeline
processing and distribution of Hubble data, manages the Hubble
data archive and archives of other ground-based and space telescopes, and develops and maintains the Guide Star Catalog and
Digitized Sky Survey. The Engineering and Software Services
Division provides engineering and software development services
to all programs at the Institute.
In the past year, we carried out orbital verification of the
Hubble observatory following the third servicing mission, resuming
normal science operations with the Wide Field Planetary Camera 2,
Space Telescope Imaging Spectrograph, and Fine Guidance Sensor
within three weeks. We made substantial progress preparing to
operate three new Hubble instruments, the Advanced Camera for
Surveys, Cosmic Origins Spectrograph, and Wide Field Camera 3,
and to operate the Near Infrared Camera and Multi-Object
Spectrometer when its cryo-cooler is installed on the next servicing
mission. We released the first elements of a new generation of
Astronomer’s Proposal Tools, which promise to aid astronomers in
planning their observations with Hubble or other observatories. A
significant transition in archive operations was reached as we began
to migrate data from optical to magneto-optical storage. We were
selected to supply the data archive and public distribution for the
Sloan Digital Sky Survey. We prepared a new facility to house the
Hubble Flight Operations Team and began conducting Hubble
mission operations from the Institute. We participated in many
T
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D i r e c t o r a t e
definition and design studies for NGST and worked with the
scientific community to define its detailed science goals. Such
efforts have led to the European Space Agency selection of
NGST as one of their future missions and to establishment
of NGST as the top priority U.S. astronomy program for the
next decade.
Hubble Division
We carry out the science program of the Hubble
Space Telescope.
We support the astronomical community with scientific and
technical advice on observing programs, as well as on the use of
archival data. We process and schedule the selected observing
programs. We ensure the proper calibration of Hubble data. We
prepare the community and the Institute for the most effective
use of future Hubble instruments.
We combine in one functional unit all the scientific and
operational resources needed to implement the Hubble mission.
We have three departments. Our Hubble Operations
Department has the operational responsibility for scheduling
the current Hubble observing program and includes the Flight
Operations Team, which transferred to the Institute in 2000.
Our Science and Instrument Support Department includes
teams for active instruments and supports observers to ensure an
optimal science program. Our New Instruments and Servicing
Department facilitates the transition of new instruments from
development to operations and ensures their optimal usage and
calibration for science observations.
The year 2000 began with the quick reactivation of the
observatory after Servicing Mission 3A and the preceding sixweek period in zero-gyro safemode. All equipment installed in
the servicing mission worked well, and the two current science
instruments, the Space Telescope Imaging Spectrograph (STIS)
and Wide Field Planetary Camera 2 (WFPC2), were quickly
back in normal operations.
Successful proposers submitted their Cycle 9 observing
programs in the spring, and the programs began executing in
June with high efficiency.
We have made process improvements, including reduction
of the lead time for generating detailed observing schedules.
This reduction has improved our responsiveness for many targetof-opportunity programs, and we are continuing to reduce the
response time below 48 hours on a routine basis.
The Flight Operations Team (FOT) began full-time Hubble
operations from facilities in the Institute in October 2000.
Previously, this team had been located at Goddard Space Flight
Center (GSFC). The FOT relocation required major modifications to facilities on the first floor of the Muller Building and an
extensive test and familiarization period for the team.
The current workhorse instrument of Hubble, the WFPC2,
provided some excitement this year when the shutter did not
operate as planned on a few occasions. Analysis by staff at the
Institute, GSFC, and the Jet Propulsion Laboratory (JPL) led to
an understanding of the problem and then to a software fix,
which was installed in the instrument microprocessor. The repair
was made in time to save a high-redshift supernovae observing
program, which had invested a large amount of ground-based
observing time just prior to the shutter faults.
We actively supported preparations for installing the Advance
Camera for Surveys (ACS) and the Near Infrared Camera and
Multi-Object Spectrometer (NICMOS) cooling system in
Hubble during the next servicing mission. This work included
support of ground tests and continued development of operational and data processing systems.
Our staff participated in the development of the Wide Field
Camera 3 (WFC3) and the Cosmic Origins Spectragraph (COS)
in 2000. We completed plans to adapt our ground systems to
support these instruments and started the work. We obtained
input from the community and selected filters for the WFC3.
We participated with colleagues at GSFC in the testing of prototype optical and infrared detectors for the WFC3. We developed
a detailed Design Reference Mission for the WFC3 and published, with the WFC3 Science Oversight Committee, a white
paper elaborating the scientific goals of the instrument. In July
2000, we conducted a successful Critical Science Review of the
detailed engineering design to demonstrate compliance with
the Design Reference Mission and science white paper.
(http://www.stsci.edu/instruments/wfc3/wfc3-csr.html)
Hubble Operations Department | We implement
Hubble observations to provide observers with data of
the highest possible quality.
We currently provide four functions: observing program development, long-range planning, short-term planning and scheduling,
and—since October 2000—flight operations.
In 2000, we completed all observations remaining in Cycle
6. Cycle 7 is now over 99% complete, with only 21 observations
remaining. Cycle 8 is 97% complete. We are midway through
Cycle 9.
The ingest of Cycle 9 General Observer (GO) programs ran
smoothly. We finished the initial processing and released the
long-range plan on schedule in May 2000. Cycle 9 includes two
target-of-opportunity programs that require execution within
24 hours of activation.
The case of Comet Linear last summer illustrated the scientific benefits of improving our response time. On the morning
of 1 August, the Director approved a target-of-opportunity
proposal to observe Comet Linear, which had swung past the
Sun on 26 July but had not been recovered by ground-based
observers. We prepared the new observations, created a new
calendar timeline, and generated new flight products, which
intercepted the timeline at the earliest moment that was safe for
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the telescope. Hubble obtained the first observations of Comet
Linear on 4 August. A press release on 7 August announced the
Hubble discovery that the comet had broken into pieces.
(http://oposite.stsci.edu/pubinfo/PR/2000/27/pr.html)
A second set of Comet Linear observations planned for 9 August
were placed in jeopardy when Hubble entered a hardware,
sun-pointing safemode on 5 August. However, we helped return
Hubble to normal operations in time for the second set of
observations.
Observing Program Development | We work with
Hubble users to ensure the optimal translation of their
scientific requirements into the technical terms of the
operating observatory.
Our focus is on Phase 2, which follows an observing program’s
approval by the Director. During Phase 2, we interact with the
user to clarify the operational details of his or her observations.
We assign to each Hubble user a Program Coordinator from our
Observation Planning Team, who serves as the user’s primary
contact with the Institute. The Program Coordinator guides user
inputs to ensure the smooth flow of this initial segment of the
operational pipeline.
The most recent servicing mission left Hubble with only
two guiding Fine Guidance Sensors (FGSs) from December
1999 until April 2000 when the replacement FGS2r was brought
online. We reprocessed over 1000 orbits of previously planned
observations to reflect the shift in launch dates and the commissioning time for the FGS, and we also reworked more than 300
orbits of observations that were originally planned for November
and December of 1999 but were deferred because of entry in to
zero-gyro safemode.
We improved the process of generating and scheduling
pure-parallel GO observations to address two such programs that
had had no scheduling success in Cycle 8. As a result, these
programs began execution. The new process, which is almost
entirely automatic, should increase Hubble’s scientific throughput due to parallel observations, particularly when the ACS’s
survey capability becomes available.
Long-Range Planning | We prepare the multiyear,
master observing schedule, which reconciles observing
requirements and operational constraints at a high level.
Both community astronomers and Institute staff use the longrange plan to assess their observing-related workloads. To be
successful, the plan must meet the goals of individual science
and calibration programs as well as satisfy physical, scientific,
and programmatic requirements. Our ability to reconcile 12 to
18 months of planned Hubble observations minimizes the
impact of observatory changes and increases our accommodation
of special observing campaigns, targets of opportunity, and
servicing missions.
During 2000, we began to migrate our long-range planning
procedures from the VMS to the Unix computing environment.
This migration has afforded an opportunity to streamline and
simplify as well.
Short-Term Planning and Scheduling | We fit
candidate observations into an optimal observing
sequence and create the detailed command loads to
execute each week of the Hubble science program.
Short-term scheduling has been likened to assembling a jigsaw
puzzle with extra pieces thrown in. The ‘pieces’ are the approximately 200 orbits of observations identified in the long-range
observing plan as possible for a specific week. Of these, only
80 to 90 orbits can actually be scheduled. The short-term scheduling process takes the individual candidate observations, ranks
them according to time criticality and attempts to put them
together in various sequences. We select the sequence that optimizes the use of the observatory in terms of on-target efficiency
and number of programs accomplished.
In 2000, we continued the work started under the Vision
2000 effort to streamline, simplify, and shorten the calendarbuilding process.
We expect data volumes to triple from the present 35
gigabits of science data per week to about 100 gigabits per week
when ACS and the NICMOS Cooling System are installed.
We will manage these higher data volumes by using the second
solid-state recorder installed on the last servicing mission.
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Flight Operations | We are responsible for spacecraft and instrument housekeeping, monitoring and
maintenance, and for the health and safety of the Hubble
mission.
The Institute’s responsibility for direct flight operation of
Hubble started in October 2000 with the transfer of the Flight
Operations Team from GSFC. An area on the first floor of the
Institute was reconfigured to become the Science Institute
Mission Operations Room (SIMOR). The SIMOR is now
staffed 24 hours per day, every day. The Mission Operations
Room at GSFC remains a back-up for the SIMOR and will be
used during future Hubble servicing missions.
Science and Instrument Support
Department | We enable Hubble observers to use
the science instruments with maximum effectiveness
by providing scientific and technical advice in developing
observing programs and interpreting data, and by
calibrating and characterizing the science instruments.
We support Hubble users during all phases of their observing
programs. For difficult programs, or when requested by the
observer, we assign a contact scientist to the program. These
contact scientists are responsible for aiding the principal investigator teams in strategies for carrying out their programs, and
for answering questions about the execution of the program or
how best to analyze the data.
For programs without contact scientists and for general
questions from the astronomical community, our Help Desk is
available, quickly answering all manner of questions about past,
present, and future instruments, or about proposal preparation,
documentation, or data-analysis software and techniques. Using
Help Desk support software, we track incoming questions. We
answer all queries within two working days—and most within
a few hours. Our data analysts provide additional support supplying hands-on data reduction and analysis support to local,
visiting, and remote observers.
Most of our staff are in groups that correspond to the
Hubble science instruments. We have one group each for the
WFPC2 optical camera, the NICMOS near-infrared camera,
and the ACS UV-optical camera. (Our ACS group is shared with
the New Instruments and Servicing Department in the period
before ACS is installed and commissioned in late 2001.) We
have one group for the STIS spectrograph, the retired Goddard
High Resolution Spectrograph, and the retired Faint Object
Spectrograph. And we have one group for general observatory
support, including the FGSs and the retired Faint Object Camera.
Our Data Analyst Group supports all instrument groups in
their calibration and user support activities. Data analysts often
become the resident experts in some aspect of instrument behavior
or calibration. They also help Institute astronomers in their
personal research and support Institute-wide projects such as the
Hubble Heritage Project. Our twenty-six data analysts are a
diverse group. Some come from undergraduate physics or astronomy backgrounds and may move on to graduate school. Others
have advanced degrees.
The year 2000 began with the recommissioning of the
instruments following the 1999 servicing mission. We restored
the WFPC2 and STIS to science operations after verifying that
their optics had not been contaminated and their detector noise
levels were unchanged. We took advantage of the temporary
low temperatures in the Aft Shroud during the servicing mission
to measure the dark current in the STIS ultraviolet detector
better to predict the background after the Aft Shroud Cooling
System is installed two servicing missions in the future. We
commissioned the newly installed FGS2r as a guider and recommissioned the other two FGSs for guiding as well as astrometric
observations.
Our WFPC2 group improved calibrations of the chargetransfer efficiency degradation, which is now a limiting factor for
precise measurements of globular cluster ages and measurements
of cosmological parameters using Cepheid variables or highredshift supernovae. Building on earlier work by the instrument
development team at GSFC, our STIS group created a correction for the scattered light problem that has vexed echelle observations by filling in absorption lines and introducing systematic
errors. In 2001, this scattered light correction will become part
of the standard pipeline for STIS data reduction.
Flight operations control room
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ACS Group | We are responsible for the scientific
utilization of the Advanced Camera for Surveys and
preparations for its installation in Hubble during the
upcoming Servicing Mission 3B.
During 2000, we continued pre-launch preparations for science
operations with the ACS. We worked closely with engineers at
the Institute, GSFC, and Ball Aerospace to implement onboard
instructions for commanding the CCD cameras in concert with
the Aft Shroud Cooling System. The commanding facilitates
the initial turn-on of the cameras as well as normal operations,
including the annealing procedure that mitigates the impact of
hot pixels caused by Hubble’s nuclear radiation environment.
We added a capability to post-flash CCD exposures, to counter
expected CCD degradation during the instrument’s mission.
We conducted several end-to-end tests of the ACS data analysis
pipeline to verify performance and shake out problems.
We developed tools for analyzing ACS data, including one
to combine and geometrically correct associated data sets. We
prototyped a tool based on the ‘drizzle’ software used for
WFPC2 and STIS, which will be incorporated into the ACS
pipeline. We also developed a prototype display package for
ACS Wide Field Camera images.
We delivered a final version of the ACS instrument handbook, together with an exposure time calculator supporting the
main ACS instrument modes, including ramp filters. Early in
the year we played the lead role in setting up a workshop on
radiation effects on detectors used for Hubble and other missions.
We worked with the ACS instrument team to develop and gain
approval for the ACS orbital verification plan. We also worked
with them to develop a homogenous flat field strategy for initial
ACS science operations, which resulted in a prioritized plan for
flat field requirements during ground calibration, orbital verification, and Cycle 11 operations.
NICMOS Group | We are responsible for the
utilization of the Near Infrared Camera and Multi-Object
Spectrometer.
In 2000, we closed out calibration and characterization of the
passively-cooled NICMOS and prepared to support NICMOS
actively cooled by the NICMOS Cooling System (NCS). The
NCS will be installed on Hubble during the servicing mission
in November 2001. We expect it to restore the NICMOS, with
an operating temperature of about 80 K, as compared to the
original 62 K.
Our close-out activities for the passively-cooled NICMOS
produced some data analysis benefits for both past and future
NICMOS observations. In characterizing the NICMOS
temperature dependence, we laid the groundwork for temperature-dependent calibration reference files for On-the-Fly
Calibration/Reprocessing. We developed an improved linearity
correction, based on on-orbit data, which will replace the previous
linearity correction derived from pre-flight ground testing. In the
process, we discovered a new characteristic of the NICMOS
detectors, a sort of bias instability to intense illumination, which
we are still investigating. We concluded a detailed rework of the
NICMOS photometric calibration, which brought the groundbased and on-orbit scale of standard stars into agreement.
We collaborated with our GSFC and University of Arizona
colleagues on electromagnetic tests of the NCS to verify the
absence of interference. We are now confident that NCS will
bring NICMOS back to life without causing an unanticipated
side effect on detector noise.
We helped develop a plan for the on-orbit verification of
NICMOS following the servicing mission. The plan includes
both science and engineering, particularly to determine the best
NCS operating temperature, which will be a compromise
between power consumption and detector performance in dark
current, quantum efficiency, and well depth.
Observatory Support Group | We maintain the
Hubble focal plane model, monitor the telescope focus,
and support the use of the FGSs as astrometry science
instruments.
In 2000, we recommissioned FGS1r and FGS3 for operations,
recertifying FGS1r as a science instrument. We also supported
the commissioning of newly installed FGS2r as an operational
guider. We identified the astronomical sources required for these
tests, prepared and scripted the Phase 2 proposals for the observations, and analyzed the data.
Based upon our experience with FGS1r during its first year
on-orbit, we expected desorption to change FGS2r’s alignment,
distortion, and interferograms. To track this evolution, we analyzed the data from a series of special engineering tests to gain
insight into the instrument’s characteristics. We also monitored
its guide star acquisition statistics to verify FGS2r’s reliability.
We supported the use of FGS1r as the astrometric science
instrument, including calibration activities, handbook revisions,
and direct support to observers.
The Hubble focus showed a departure from its long-term
trend. To ensure that the telescope remains in focus within tolerances, we supported special monitoring tests before and after the
servicing mission. We provided the Phase 2 proposal for these
tests and played a key role in the analysis of the data.
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Spectrographs Group | We are responsible for the
New Instruments and Servicing Department | We
use of STIS and for supporting archival analysis of data
facilitate the use of new science instruments by partici-
from the retired spectrographs.
pating in their development, by capturing and transferring
information about instrument operation and calibration to
Early in the year 2000, we completed the orbital verification
activities following the third servicing mission. An anomalous
rise noted in the CCD read noise has remained stable with no
adverse impact on scientific observations.
We implemented a tool for users (based on an algorithm
developed by the STIS instrument team) that corrects for scattered
light in echelle spectra. This scattered light leads to systematic
errors of up to 5% in our standard calibration pipeline. When
we release On-the-Fly Reprocessing for STIS data, this new tool
will become a part of the standard pipeline process.
We have increased the scientific efficiency of Hubble through
a careful planning of the STIS calibration program. We reduced
by nearly 50% the number of orbits required, making good use
of our increasing knowledge of the instrument sensitivity, its
stability, and our ability to track its evolution.
WFPC2 group | We are responsible for the use
of WFPC2.
Our most significant activity in 2000 was the correction of an
anomaly in the WFPC2 shutter operation. In August, WFPC2
began experiencing anomalous exposures in which the shutter
failed to open properly, resulting in blank science images. In late
October, the error rate increased sharply and a new problem
appeared: the shutter blades occasionally collided, which caused
them to bounce and remain open. WFPC2 observations were
suspended. The problem was traced to a sensor that measures the
position of a shutter blade. A repair was devised to correct the
problem by modifying (patching) the WFPC2 microprocessor
code to allow the shutter position sensor more time to detect
the shutter’s position. The patch was installed in early November
2000, and WFPC2 has shown no further anomalies.
We continued to study the degradation of charge transfer
efficiency, which grows in severity as radiation damage to the
CCD detectors increases. We conducted studies of its impact on
the of photometry extended targets. We explored techniques to
reduce its effect on data, such as pre-flashing. We released a
handbook on ‘dithering’, a commonly used method to improve
sampling and remove artifacts in astronomical images. The handbook describes strategies for analyzing data taken with position
dithers.(http://www.stsci.edu/instruments/wfpc2/Wfpc2
_driz/dither_handbook.html) We created automated procedures
for generating ‘dark’ calibration reference files, which will reduce
routine work and allow users to use darks customized to the epoch
of their data.
the Institute, and by coordinating the recommissioning of
all the instruments following a servicing mission.
We supported the verification of the Hubble observatory following the successful third servicing mission, and we helped prepare
the instruments for the remaining two missions. On the fourth
servicing mission in late 2001, the astronauts will replace the
Faint Object Camera with ACS and install a new cryo-cooler to
extend the life of NICMOS. In the final servicing mission, they
will install two fourth-generation science instruments, COS and
WFC3, as well as a new Aft Shroud Cooling System to enhance
the performance of STIS and ACS by maintaining the low
temperatures their detectors require.
We continued preparations to operate ACS after it is
installed. We completed the scheduling system and post-observation processing systems, which we will test with the instrument
prior to launch. Working with the ACS team, we helped characterize the flight detectors, calibrate the instrument, and improve
it generally.
We began work on the scheduling system, data pipeline,
and archive for COS, which is being developed by the University
of Colorado. COS is a moderate-resolution, point-source spectrograph, which is designed for the highest possible throughput
and maximum wavelength coverage. In conjunction with the
COS team, local Far Ultraviolet Spectroscopic Explorer (FUSE)
scientists, and GSFC, we have begun to explore calibration
techniques for COS.
We continued to play a strong role in the development of
WFC3, partnering with GSFC, JPL, and Ball Aerospace. WFC3
is a high-resolution, panchromatic camera covering the near
ultraviolet through near-infrared wavelength ranges (0.2 to 1.7
microns). WFC3 will ensure that Hubble retains a superb imaging capability through end of life. In 2000, we began developing
the scientific requirements for the front- and back-ends of our
ground system to handle WFC3 and its data. We supported
the testing of prototype CCD and infrared detectors with our
colleagues at the Detector Characterization Laboratory at GSFC.
We developed an exposure calculator tool to facilitate work on
the WFC3 Design Reference Mission. Working jointly with
members of the Science Oversight Committee, we published a
Science White Paper elaborating the scientific goals for the
instrument. We participated in numerous scientific trade-off
studies for WFC3. We carried out a Critical Science Review as
a precursor to the successful Critical Design Review of WFC3,
which was held in December 2000.
(http://www.stsci.edu/instruments/wfc3/wfc3-csr.html)
In conjunction with NASA’s Office of Space Science, we
hosted a meeting entitled New Detectors for Space Astrophysics
in June 2000 with over 180 registered participants. The meeting
brought together scientists and engineers working in wavelength
domains from gamma rays to radio. The purpose was to evaluate
the state of the art in current and emerging detector technologies. We will publish the proceedings of this meeting in 2001.
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Archive Branch | We operate the Institute’s archive
systems, provide data delivery to users, enhance data
retrieval, and ensure the scientific integrity of the data
archive.
ACDSD staff participate in daily operations status briefing
Archive, Catalogs, and Data
Services Division
We process Hubble data in the pipeline, distribute
Hubble data products to the community, and operate
the Multimission Archive at STScI. We maintain and
upgrade the Guide Star Catalog and Digitized Sky
Survey.
Observation Processing and User Support | We
are responsible for pipeline processing of all Hubble data,
including procedural evaluation of observation quality.
We also provide offset-slew and real-time target acquisition support for Hubble observers.
In 2000, we processed 57,486 observations, up 21% from 1999.
We typically delivered a new science observation into the archive
for access by users within 30 hours of when it was taken. This is
about 15% longer than in 1999, primarily due to system down
time for infrastructure improvements to the production pipeline
and to the archive.
We made major changes to the science pipeline in 2000, the
most dramatic of which was moving almost entirely off VMS
onto Unix computers. Only data conversion for Wide Field
Planetary Camera 2 and Faint Object Camera remains on VMS.
Also, we moved our pipelines and databases out of the secure
environment of the scheduling and spacecraft commanding
systems, which enables sharing computer resources with the
archive. This sharing simplifies the management of calibration
data because the initial processing and the On-the-Fly Calibration
(OTFC) now utilize the same computers and caches of reference
data. We coordinated the science pipeline changes with the
Data Processing Team of the Engineering and Software Services
Division and the Computer Systems Operations Department
of the Computer and Information Services Division.
The Hubble data archive is the most heavily used collection
of pointed observations in astronomy today.
(http://archive.stsci.edu/) Its increasing data volume and usage
enable new approaches to astronomical research and ensure the
archive’s key role in the second decade of Hubble operations.
Indeed, the Hubble archive has demonstrated the fundamental
utility of astronomical archives to the broader community and
has inspired new initiatives now being taken in many groundbased facilities to provide on-line access to their data sets.
The technological barriers to processing large quantities
of data are rapidly vanishing. We are taking advantage of this
opportunity to demonstrate the utility of open access to high
quality science data. Today, the Hubble archive fosters two
exciting kinds of exploration. First, the archive is used for
scientific research and discovery. Second, the archive is in the
vanguard of worldwide efforts to improve the science of archival
research itself.
In 2000, the Hubble archive received 1.1 terabytes of new
data, and the total data volume was over 8 terabytes. (Because
our OTFC system freed up more than a terabyte of storage, the
total volume of the archive actually went down in 2000 with no
reduction in scientific utility.) We distributed 5.3 terabytes of
data to researchers, which brought the total volume of Hubble
data distributed since launch to 23.5terabytes.
We reached a key milestone in our Hubble Archive
Re-Engineering Project (HARP) with the installation of new
magneto-optical (MO) storage units. The MO technology is
eight times less costly than the large format optical platters we
used for the past six years. The MO storage units raise our total
data capacity to 10 terabytes. Coupled with our OTFC and
data compression processes, we will easily be able to store the
anticipated ACS data output online for several years to come.
The Multimission Archive at STScI (MAST) continued to
offer new user services. We began public distribution of data
from the Far Ultraviolet Spectroscopic Explorer (FUSE). We
established a collaboration with the Astrophysics Data Service
(ADS) at Smithsonian Astrophysical Observatory, which will
provide links between MAST data sets (including Hubble) and
the on-line publications that result from those data sets. With
this utility, researchers can quickly identify the specific data used
in published research. This capability will aid the planning of
new observations and facilitate the evaluation of the productivity
of instruments on different missions. Other improvements to
the archive in 2000 included transfer of our VLA FIRST data
to our CD-ROM jukebox, which makes retrievals more rapid,
and expansion of our cross-correlation search tool, which now
works on all supported MAST missions.
(http://archive.stsci.edu/ mast.html)
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MAST received funding from the NASA Senior Review
process, ensuring four years of growth to support optical and
UV missions, such as the Galaxy Evolution Explorer.
We were active in the definition and prototyping of technology and algorithms that will be vital to the National Virtual
Observatory (NVO). We collaborated with counterparts at
GSFC to submit an NVO prototype proposal to NASA.
We have taken a lead role in the Astrophysics Data Center
Coordination Council, which will help define standards and
procedures for improved interoperability between all the major
NASA data centers.
Catalogs and Surveys Branch | We produce
all-sky digital images and deep object catalogs to support
Another plate is prepared for scanning
observatory operations worldwide and to provide a
research resource to the community.
We obtain our images and catalogs by digitizing, processing, and
analyzing the photographic sky survey plates from the Palomar
and Anglo-Australian Schmidt telescopes. These data products
provide accurate target coordinates, guide stars, and finding
charts used in telescope operations. They are used for many
other scientific purposes, such as the optical identification of
sources detected at other wavelengths.
For the Digitized Sky Survey, we are completing the scanning of the second-epoch surveys, which will cover the sky in
three passbands. These products are available to the community
via a number of web servers around the world.
Guide Star Catalog II (GSC-II) will have all-sky coverage
and contain colors and proper motions for about two billion
objects down to at least 18th magnitude. To date, we processed
most of the available plate material to produce a database of
almost 2 terabytes. We released interim versions of the GSC-II
to Hubble, Gemini, and Very Large Telescope operations, which
benefit from the improved quality and sky coverage. As more
fields become available, Hubble operations will use them to
provide automated bright object protection.
We coordinated a study of guide star availability for NGST.
In this study, theoretical galaxy models were extended to the
infrared and compared to available ground-based infrared observations for validation. These results will help define the NGST
guidance system performance requirements. We currently believe
that GSC-II correlated with the Two Micron All Sky Survey catalog will provide a sufficient density of guide stars for NGST.
Next Generation Space
Telescope Division
We collaborate with NASA to develop the scientific,
technical, and operational vision for the Next
Generation Space Telescope (NGST). We are responsible
for developing the NGST Science and Mission
Operations Center, with which we will operate the
telescope and implement its science program.
We share a great challenge: to construct and operate Hubble’s
successor at a fraction of Hubble’s cost. We also share an
unprecedented opportunity: to use state-of-the-art technology to
achieve Hubble-like performance at infrared wavelengths, with
which to observe the birth of the first stars and galaxies. The
Next Generation Space Telescope (NGST) is a joint endeavor of
three international partners: NASA, the European Space Agency
(ESA), and the Canadian Space Agency (CSA).
We are members of the NASA project team for NGST. This
‘badgeless’ partnership has been the foundation of our successful
relationship with NASA on this complex program. Our staff play
essential roles, providing leadership in optical design, technology
development, science operations, and instrument design.
In 2000, working with NASA’s Project Scientist for NGST
and the Ad-hoc Science Working Group for NGST, we helped
define a core set of instruments for NGST based on the highest
priority science goals in the NGST Design Reference Mission.
This process made heavy use of the Institute’s NGST Mission
Simulator to study trade-offs between the various parameters
affecting NGST sensitivity and the schedulability of observations. We provided scientific oversight of requirements for the
point designs of the three instruments included in the Integrated
Science Instrument Module during feasibility studies (Phase A).
We analyzed the likely calibration programs for NGST instrumentation to understand the potential need for on-board lamps
and parallel observations. We studied the requirements for
NGST detectors, the likely effect of cosmic rays on those detectors, and the design of the read-out electronics.
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With The Johns Hopkins University, we established a new
laboratory for testing infrared detectors. Our main goal for the
lab, called the Independent Detector Testing Laboratory (IDTL),
is to test all detector types considered for use on NGST. The
team will compare prototype HgCdTe (mercury cadmium
telluride) and InSb (indium antimonide) detectors to support
the selection of the flight detector technology in late 2002.
The lab will also help the wider community to develop better
infrared detector arrays for astronomy.
We made improvements to the NGST Mission Simulator,
which has proven a useful tool for developing the operations
concept and conducting cost-performance trades. We improved
the granularity of the reference observing program and the fidelity
of the observatory model. With NASA’s approval, we released
source code for NGST Mission Simulator to the two prime
contractors to facilitate competition-sensitive studies of their
observatory concepts.
The Ad-hoc Science Working Group completed the terms
of its charter and was disbanded. We assisted NASA in the solicitation and selection of a smaller, more senior, interim group to
represent the interests of the international science community
prior to the selection of the U.S. science team and the creation
of the flight Science Working Group. The Interim Science
Working Group reports to NASA Headquarters and will review
plans for the selection of the prime contractor and the Science
Working Group. We assist the Interim Science Working Group
and recommend science and technical issues for their consideration.
We worked with the Office of Public Outreach to coordinate
special sessions at the American Astronomical Society meetings
to publicize the recommendations of the Ad-hoc Science
Working Group and the progress of the NGST technology
development. We have posted NGST studies on Institute and
NASA web sites and advertised them on list servers.
(http://www.ngst.nasa.gov/doclist/bytitle.html)
We developed an Operations Concept Document, which
we will update throughout the development phase of the NGST
project to remain current with the NGST design and operational
characteristics. Ultimately, the document can become the basis
for developing formal operations plans and designs.
We analyzed a variety of issues with potential impacts on
design concepts for the potential prime contractors. These issues,
which had arisen in the project working groups, included
observatory performance, stray light, communications, and
image quality.
As part of the core NGST project team, we participated
in meetings preparing for the selection of the prime contractor
and the next phase of the NGST development. We also helped
NASA develop the key mission performance goals prior to
solicitation of the prime contractor proposals.
We helped NASA project management develop a management philosophy and scale of the NGST mission to achieve a
low life-cycle cost. We addressed the allocation of work between
the prime contractor, NASA, the international partners, and the
Science and Mission Operations Center. We performed a study
of low-cost operations, which identified the development aspects
that are key to reducing NGST operations costs. We helped
NASA rescope and recost NGST to bring development plans
within schedule and cost guidelines.
NGST GoTeam
NGST Team meeting
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Engineering and Software
Services Division
We are responsible for all software development and
engineering support at the Institute.
We are organized in four departments: Science User Systems,
Planning and Scheduling Systems, Ground Systems, and Mission
and Flight Engineering. Our staff consists of scientists, engineers,
and software professionals dedicated to developing quality software and delivering expert engineering with the sole aim of
enhancing science return to the astronomical community. By
combining all the Institute’s software and engineering teams
within one division, we secure efficiencies through innovation,
commonality, and sharing.
In 2000, the community made increased use of our software
systems and our software and hardware expertise. Our customers
included astronomy missions beyond Hubble and the Next
Generation Space Telescope (NGST). We look forward to the
continuing, wider deployment of our systems in support of science.
We take pride that the systems developed for the Hubble Space
Telescope are enabling scientific discoveries the world over.
Science User Systems Department | We develop
and support the software used by scientists to prepare
their Hubble programs for execution and to analyze their
data after the observations.
With science and user software systems gathered into one
department, we have the opportunity to develop a more consistent external interface for our observing community. We consist
of two groups: the Science Software Group and the Astronomer’s
Proposal Software Team.
Science Software Group | We develop calibration
and data analysis software for use by the instrument
groups, the pipeline data processing team, Hubble
archive users, and Hubble observers.
In 2000, we tested the first version of the Advanced Camera for
Surveys (ACS) calibration package by which all ACS data will
be calibrated. Because it will produce a significantly larger data
volume than previous instruments, ACS presents challenges
for data storage and transmission to observers over the Internet.
To ease these tasks, we developed a new compressed image
format by which most ACS images can be compressed by a
factor of ten while still permitting analysis tools to have easy
access to the data.
We created a new set of tools for analyzing infrared data
from the Near Infrared Camera and Multi-Object Spectrograph
(NICMOS). These tools compensate for the quirks of NICMOS
data, thereby increasing the scientific value of both archival
and the new data to be acquired after the next servicing
mission. We will incorporate the new tools into the NICMOS
calibration pipeline.
We successfully completed the preliminary design review for
the Cosmic Origins Spectrograph (COS) pipeline. We began a
design for the Wide Field Camera 3 (WFC3) pipeline.
We completed the first version of a new data analysis command language called PyRAF. The new system, which is based
on the freely available and widely used Python scripting language,
supports all of our existing data analysis tasks (including scripts
written in the old command language). PyRAF is more open
and extensible than the old system. It is fundamentally more
powerful for both astronomers and programmers. We distributed
a public beta release of PyRAF, which is in use at many sites
around the world.
Astronomer’s Proposal Software Team | We
develop the software used by astronomers to plan their
Hubble observations and to describe how the spacecraft
should carry them out.
Our current proposal preparation software is RPS2 (Remote
Proposal Submission Two). It aids astronomers in preparing their
programs by ensuring correct syntax, verifying the legality of
instrument configurations, and determining that the program is
feasible for scheduling.
Our primary development project is the Astronomer’s
Proposal Tools (APT) system for preparing proposals for Hubble
and other observatories. APT provides a more modern interface
to our existing tools, along with new capabilities that make
proposal preparation easier.
In 2000, we enhanced RPS2 to provide more helpful diagnostics and advice to users, which means fewer RPS2 processing
errors. We also coupled the Guide Star Selection System with
RPS2, which now permits astronomers to determine when their
targets have no available guide stars and to modify their programs
to solve the problem. Observers were able to use this feature to
prepare their Cycle 9 proposals.
We released the initial version of APT including the Visual
Target Tuner (VTT), which allows observers to plan their observations through an interactive graphical interface. The VTT was
also integrated with the StarView interface, providing Hubble
archive users better information about Hubble observations of a
given astronomical object. We developed the APT exposure time
calculator, which proposers use to determine the observing time
needed to achieve their scientific goals. We also developed a tool
for observers and Institute staff to help them check the vicinity
of Hubble targets for bright ‘spoiler’ objects, which might ruin
data or even damage an instrument.
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Planning and Scheduling Systems
Department | We are responsible for planning and
Spacecraft Scheduling and Commanding
Team | We provide software, analysis, and documen-
scheduling software products currently used for Hubble,
tation support to the planning and scheduling area of
the Far Ultraviolet Spectroscopic Explorer, Chandra,
the Hubble ground system.
and NGST, as well as several large ground-based optical
observatories. We also support the development of
products such as APT and the Grants Management
System (GMS).
Our department consists of three development teams and a
testing team providing services to our entire division. With the
Institute’s engineering talent on planning and scheduling systems
gathered within our department, we provide our customers a
high standard of support, taking full advantage of the skills
within our software groups.
Planning Development Team | We develop frontend planning and scheduling software.
We are responsible for the applications known as Spike,
Transformation, and the Parallel Observation Matching System
(POMS). Spike produces long-range plans for Hubble and has
been modified to produce both long-range plans and short-term
schedules for other missions. Transformation feeds downstream
planning and scheduling applications with data from Phase 2
proposals. POMS identifies opportunities to place parallel
science observations on prime science timelines.
In 2000, we changed Spike to support the operations of
the Far Ultraviolet Spectroscopic Explorer (FUSE). We delivered
the Spike system to the Subaru observatory to handle their
observation planning. We also prototyped a Spike tool to streamline short-term scheduling on Hubble.
We continued to redesign Transformation into a new data
product, called TransVerse, which will be more easily maintained
and adapted to a changing spacecraft. We completed a study
for Qwik-Trans, which demonstrated that TransVerse will significantly improve speed in the proposal preparation process.
SESD Lab
We are responsible for developing and maintaining the Payload
Operations Control Center Application Software Support
(PASS). PASS supports Hubble’s weekly scheduling, including
antenna management, recorder management, command management, and Tracking and Data Relay Satellite System (TDRSS)
communications schedules.
In 2000, we updated PASS software to new standards and
incorporated load checking algorithms to ensure error-free
command loads for Hubble for the first time. We began the
large task of converting the PASS software from the VMS platform to Unix.
The year started with the PASS software successfully supporting the concurrent demands of the Y2K century crossover
and the servicing mission. The PASS upgrades for the new
onboard computer installed during the servicing mission worked
flawlessly. We completed the TDRSS scheduling project, which
included PASS software upgrades and tests of our interface
with a new TDRSS network system. We completed a reference
selection system for the fixed-head star tracker, which simplifies
operations by providing the needed information earlier in the
scheduling process.
Scheduling Development Team | We provide the
short-term scheduling system for operating Hubble and
other missions.
Our software products for Hubble include the Science Planning
and Scheduling System, the Science Commanding System,
the New Guide Star System, and the Moving Object Support
System. For NGST, our team provides the NGST Mission
Simulator, which is a web-based suite of tools containing a
model of the NGST observatory and its environment, which
are used to develop the NGST Design Reference Mission.
In 2000, we made 17 software releases of which 6 were
major. These releases closed over 100 Operational Problem
Reports and also provided useful enhancements. We supported
the Hubble Division’s conversion of their operational scripts to
Python and provided significant software development resources
to the Grants Management System (GMS).
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Software Testing Team | We provide quality
software testing. We are committed to improving the
quality and productivity of testing as a fundamental
process at the Institute.
The software testing team is a new group, created in March 2000.
We supported the operational release of major software
systems, including OPUS (the Observation support/Post-observation data processing Unified System), Science Planning and
Scheduling System, and special projects such as TransVerse and
GMS. We also developed the Integrated Test Environment to
support testing of several planning and scheduling subsystems.
Ground Systems Department | We are responsible
for the development and maintenance of the Institute’s
science ground system, including archives, post-observation data processing, and a supporting infrastructure of
databases and software systems.
Our department comprises the Archive Team, Data Processing
Team, Systems Infrastructure Team, and Database Developer
Team. The teams within the Ground Systems Department maintain expertise in the hardware, operating systems, and databases
used throughout the Institute. While our department’s primary
focus is on the Institute’s high-volume, high-reliability data
processing servers, we also support the various hardware and
software platforms used by other engineering departments.
Our systems are used in several missions other than Hubble,
including the International Gamma-Ray Astrophysics
Laboratory (INTEGRAL), the Space Infrared Telescope Facility
(SIRTF), the Chandra X-Ray Observatory, and FUSE.
Archive Team | We develop, deploy, and upgrade
the systems used for archival scientific research.
We are responsible for the software for Hubble’s Data Archive
and Distribution Service (DADS), Multimission Archive at
STScI (MAST), and the AutoBulk system, which generates the
updates from the Hubble archive for our mirror sites at the
Space Telescope European Coordinating Facility, the Canadian
Astronomy Data Centre, and the National Astronomical
Observatory of Japan. We are also responsible for the StarView
user interface, which provides the international astronomy
community with a sophisticated browser to the Institute’s archive
catalog holdings.
In 2000, we worked with the Data Processing Team on the
On-the-Fly-Calibration (OTFC) project, which was released to
the community in January. OTFC calibrates science data as it is
requested from the archive, which ensures that the end-user
receives the benefit of the most up-to-date calibration algorithms
and reference files. OTFC also benefits the Institute, because the
archive must no longer ingest the calibrated data; only the
uncalibrated (raw) data is stored, which reduces costs for storage
media and minimizes usage of the jukebox storage systems.
We released a more automated version of the AutoBulk
system creating the CD-R versions of the Hubble data for our
sister archive sites. We readied the archive for the newer magneto-optical (MO) media. We released a Java-based version of the
StarView interface for the Hubble archive, which offers the user
greater platform compatibility, flexibility, and control.
Data Processing Team | We are responsible for the
routine data processing and calibration pipelines.
Our pipelines include the standard production pipelines that
unpack, format, edit, process, and calibrate the raw data received
from Hubble. Our other pipelines include the OTFC, the
Astrometry Science Data Pipeline, and the Observatory
Monitoring System pipeline, which processes telemetry data
for jitter files and spacecraft events.
In 2000, we deployed the OTFC system, which has proven
reliable, responsive, and valued by users. All data from the Space
Telescope Imaging Spectrograph (STIS) and Wide Field
Planetary Camera 2 (WFPC2) are now being recalibrated as they
are retrieved from the archive. Likewise, we no long store the
calibrated data for these instruments in the archive, reducing
the throughput needs and the archive size.
The OFTC system is based on OPUS, which is a process
flow control system now used for several different missions
and applications.
We improved OPUS in two major ways in the year 2000.
We created a fully documented Application Programmers
Interface to OPUS. This allows the Institute and other OPUS
application developers more easily to integrate their processing
steps into an OPUS pipeline. Our second improvement was to
implement an enhanced monitoring mechanism, which provides
OPUS operators better visibility into the flow of data through
the pipeline. The new mechanism also offers the advantage of
being completely platform independent (it is Java based), which
allows the operators to use their preferred desktop to manage
an OPUS pipeline.
We implemented the pipeline elements for ACS. Because
ACS will generate significantly larger data volumes than previous
Hubble instruments, we improved the operational data processing systems by adding higher performance servers and more disk
capacity.
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Systems Infrastructure Team | We investigate,
Mission and Flight Engineering Department |
test, and deploy new technologies, products, and tools
We are responsible for the health and safety of the
used on the science ground system components. We
Hubble science instruments, the stored commanding
develop the application programming interfaces used to
of the Hubble instruments, and systems engineering
access databases and support the system for tracking
of software systems at the Institute. Our department
problem reports and work requests on the science
consists of the Engineering Team and the Systems
ground systems.
Engineering Team.
In 2000, we focused on deploying Grants Management System,
offering enhanced tools both for the grant proposer and the
grant administrator. These tools improve the reporting, tracking,
and distributing of grants.
We supported Hubble’s Control Center System on the
design and development of the data warehouse report generator.
We also set up the tracking system and databases for quality
evaluation needed by the historical data load project.
We have in-depth engineering knowledge of the Hubble flight
hardware and flight software, useful to understand the operational needs of the Hubble mission. On this basis, we provide
systems engineering services to projects at the Institute and
GSFC. For example, we contributed to the assessment of the
WFPC2 shutter anomaly, which threatened the utility of its
most scientifically productive instrument. We performed systems
engineering for the NGST project based on our understanding
of the Hubble spacecraft and ground system.
Database Development Team | We manage the
proposal, planning, and grants databases for the Hubble
Engineering Team | We maintain engineering knowl-
program. We also manage the archive databases, which
edge of the Hubble instruments and spacecraft hardware.
index all of the science data holdings of the Institute.
We monitor the health and performance of the science
We provide the Institute’s engineering expertise in the
instruments and track the status of limited-life items
design, maintenance, and evolution of database systems,
within the instruments.
assisting engineering teams, operations staff, and science
users throughout the Institute with their database applications and needs.
In 2000, we supported the myriad database updates and entries
accompanying a new Hubble proposal submission cycle. We
continued to improve these front-end systems with the goal of a
seamless flow of data from the proposer to the appropriate entries
in the planning, administrative, grants, and archival databases.
We provided the necessary updates to the archive catalogs to
enable the transition from the 12" optical platters to the newer
5" magneto-optical media. We also updated the archive catalogs
in support of the OTFC and OTFR projects and to include the
ACS as a new instrument.
The Database Development team supported the Hubble
Operations Department in migrating their various database
reports to a Unix environment.
We work with the science and operations staff to improve the
quality of science data returned from Hubble. We analyze instrument anomalies and ensure their safe recovery from safing
events. In advance of servicing missions to Hubble, we work
with NASA personnel to define the operational requirements
of new hardware. During the servicing mission, we provide 24hour support. We operate an instrumentation laboratory, which
maintains the guide star plate scanning machines and supports
instrumentation projects of Institute astronomers.
In 2000, we supported the anomaly review boards that
investigated the WFPC2 shutter anomaly and the increase in
STIS read noise following the last servicing mission. We performed evaluations of the electrical and mechanical systems to
look for contributing factors. We supported the real-time
recovery of the instruments following the hardware sun-point
safe-mode event, NICMOS multibit error, and WFPC2 shutter
anomalies. We conducted a limited-life analysis on the WFCP2
Selectable Optical Filter Assembly. We executed several tests on
the ACS operations bench to verify ground system throughput,
ACS CCD set points, anomalous MAMA recovery, CCD Charge
Transfer Efficiency analysis, CCD post-flash, and servicing
mission orbital verification proposals.
Our instrument laboratory staff contributed to the design of
the Infrared Multi-Object Spectrograph, which is being built in
collaboration with GSFC for ground-based astronomical observations. We designed, fabricated, and tested a detector fan-out
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board for use in characterizing infrared detectors at GSFC for
WFC3. We supported the creation of an infrared detector testing
facility at the Institute.
We began work on a contract with the Wilmer Eye Institute
of The John Hopkins University to develop an improved device
for characterizing eye abnormalities.
Systems Engineering Team | We provide systems
engineering support to software system projects at the
Institute. We ensure that the software projects conform to
the science operations requirements.
We are responsible for creating the instructions that specify the
stored command loads for executing Hubble science operations.
We implement, test, document, and maintain all instructions
and database elements required for commanding science
operations. We also define, document, and maintain the software
requirements for the front-end ground system. These requirements specify the transfer of information from the proposal to
command load. We support on-orbit Hubble operations by
reviewing or creating implementation plans for non-standard
and engineering proposals, such as those for the orbital verification program that follows each servicing mission.
In 2000, we worked with the ACS, COS, and WFC3
instrument teams to define the science requirements and instrument designs to ensure the instruments can be operated by
the Institute’s software systems. We completed the command
instructions for the ACS and ran several end-to-end tests on the
ACS operations bench. We incorporated commands for the
Aft Shroud Cooling System into the reconfiguration rules for
ACS and STIS. We incorporated commands for the NICMOS
Cooling System into the NICMOS reconfiguration rules. We
successfully implemented an installation procedure for WFPC2
flight software patches to remedy the shutter anomaly. We also
began work on the COS and WFC3 command instructions.
We contributed to the system requirements for science and
engineering telemetry processing in the new control center
software developed at GSFC. We provided systems engineering
support to a variety of other software projects at the Institute,
including APT, OTFC, OTFR, TransVerse, Data Quality
Alerts (AlertObs), and the Dual Solid State Recorder capability.
We supported the NGST Software and Operations
Working Group efforts to create the second revision to the
Ground to Flight Interface Requirements Document. We also
made significant contributions to the Institute’s NGST
operations concept.
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we provide
business services
Administration Division
We provide business and administrative services to the Institute in
the areas of finance, human resources, accounting, contracts, grant
administration, procurement, facilities management, property
administration, administrative support, and staff support services.
he Administration Division is organized into branches,
groups, and offices according to our major functions and
responsibilities. We strive for a strong customer service
orientation, aware that we are involved directly or indirectly in
almost every endeavor of the other organizational units of the
Institute, as well as in the careers of Institute staff and the funded
research of Hubble observers. We constantly seek new ways to
improve our performance and increase customer satisfaction.
T
Administrative Support Group | We are a functional
unit of administrative staff deployed by matrix assignments
Administration Division managers discuss a process
to the operating divisions. Our Division Administrators and
Administrative Assistants provide administrative support
of all kinds. We also facilitate coordination between the
Administration Division, Institute management, and the
divisions.
In 2000, we developed the ST ScI Survival Guide, a comprehensive
orientation package for new employees and a useful compendium
of materials for all staff. We will maintain the Survival Guide as a
working document by continual review and improvement. The
guide is available on the web at http://www.stsci.edu/stsci/diva/.
We began a volunteer program to cover staff absences and
address periods of individual work overload. This program has
virtually eliminated the need for purchasing temporary help, and it
has broadened the perspectives of administrative staff by exposure
to areas outside their assigned divisions.
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d i v i s i o n
Finance Branch | We maintain all Institute financial
Contracts and Sponsored Programs Office |
records, prepare and monitor performance against
We support Institute staff in preparing proposals and in
indirect budgets, and produce management financial
administering awarded grants and contracts.
statements. We track property, make travel arrangements
for Institute staff and visitors, and ensure that procurements of products and services are competitive.
During 2000, in addition to providing customary services and
supporting the seamless reorganization of the Institute, we
undertook a variety of process improvements. We incorporated
credit cards into our purchasing processes, which increased procurement efficiency while retaining proper accounting controls.
We performed a major upgrade of our Costpoint accounting
software and supported its integration with the Grants
Management System (GMS).
We undertook several self-improvement reviews with an
eye toward customer service and efficient operations. Among
the outcomes were improvements to our purchasing, travel,
and property functions, as well as finalized plans for multiplatform compatibility for our electronic timecard service.
In 2000, we helped prepare 131 new, continuation, or supplemental proposals for grant or contract funding for our staff. Of
these, 91 were for Hubble research funding. As of December 31,
2000, 316 grants and contracts (other than the Hubble Prime
Contract) were in place, representing $23.1 M in value. During
the year, 60 new awards were received.
Grants and Contracts Branch | We provide contract
and grant administrative services for the Institute.
Some of the participants in our Bring Your Child to Work Day
Our services include preparing budgets for grant proposals,
tracking compliance with the terms of grants and contracts, and,
in conjunction with the AURA corporate office, interpreting
regulations. Our branch is divided into two offices, the Grants
Administration Office and the Contracts and Sponsored
Programs Office.
Human Resources Department | We provide a
wide range of personnel services to Institute staff and
management, including recruitment and employment,
relocation, salary administration, benefits administration,
development of Equal Employment Opportunity/Affirmative
Grants Administration Office | We provide funds
Action plans, employee-management relations, and
to Hubble General Observers and Archival Researchers
various forms of training, including the newly defined
to support their scientific research based on Hubble
Management Training Program.
observations. Also, we facilitate the financial review of
submitted budgets and make funding recommendations
to the Director for final approval.
From inception of the Hubble program, we have awarded over
$160M for 4,021 grants to General Observers and Archival
Researchers. In 2000, we awarded 492 grants worth about
$14M. In addition to the Hubble analysis grants, this includes
funding for the NASA headquarters grant program entitled the
Initiative to Develop Education through Astronomy and Space
Science (IDEAS).
In 2000, we participated in the testing of GMS, the new
electronic, web-based software system to manage the grants we
administer. The baseline release was completed in September
2000. We began activating grantee accounts in the system for the
Cycle 10 budget input in February 2001. The primary goals of
GMS are to expedite the process of allocating funds for research
programs and to reduce administrative effort in awarding and
administering grants.
In 2000, we enhanced recruitment efforts to include three additional activities: increased advertising on the Internet to reach
a more diverse applicant pool, purchasing résumé databases to
provide an additional recruitment source, and participating in
numerous job fairs throughout Maryland. These efforts resulted
in 72 AURA hires, including 35 regular and 22 temporary
employees. Additionally, 10 students were placed in student
intern positions as part of our ongoing affirmative action effort
to provide training and to develop future employment opportunities for women and minorities. Even though the Institute-wide
turnover increased from 10.4% to 15.3% in 2000, our rate still
compares favorably with the national average of 18%.
We enriched our offerings in management training by
including new topics: technical project management and technical leadership.
We sponsored a series of employee programs, including
the annual Family Day, Bring Your Child to Work Day, United
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Way campaign, and Red Cross blood drives. In addition, we
researched and negotiated an improved medical insurance
option, which was offered to all employees during a summer
open enrollment period.
Our human resource operations remained fully compliant
with regulatory requirements, resulting in no Equal Employment
Opportunity complaints being filed during the year.
Facility Operations Group | We manage the
Institute’s facility operations, comprising the 130,000
square foot Muller building and a 300-car parking facility.
We also contribute logistical support services to our
off-site leased office space at the Rotunda and The Johns
Hopkins University’s Bloomberg Building.
In 2000, we completed the construction of Hubble’s Science
Institute Mission Operations Room (SIMOR) facility in the
main computer area on the first floor of the Muller Building.
Elsewhere in the Muller Building, we continued the scheduled
replacement of major mechanical equipment, which will
ensure the continued safe, reliable, and efficient operation of
the building.
Staff Support Services Group | We provide a
variety of services, including security, housekeeping,
parking administration, food services, document
reproduction, and other logistical support.
In 2000, we upgraded the system that controls facility access,
expanding it to include new zones and tightening control of
the SIMOR. We conducted more than 150 staff relocations,
including many due to the Institute reorganization. Our Central
Copy Center processed more than 4.1 million document impressions. We provided logistical support for numerous special events
at the Institute, including colloquia, the annual May Symposium,
and the Hubble Fellowship Symposium.
Staff support services
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we maintain
the information
infrastructure
Computing & Information Services Division
We install and support all Institute computing and networking
facilities and maintain the infrastructure of the Institute’s information systems. We also lead a number of interdivisional committees
in planning for future needs.
ur Computing Services Operations Department provides
support for computers, networking, and security. Our
Information Systems and Technology Department provides
information services, support for application software, and leadership for evaluating computer technology Institute-wide.
With the assistance of the interdivisional Computer
Planning Committee, we develop the annual computer augmentation
plan, which identifies the top priorities for computer hardware and
software purchases for a three-year period. Similarly, we coordinate
the material and equipment budgets of divisions and offices,
allowing us to identify cost savings through coordinated purchases.
To enhance our service orientation in 2000, we developed
a formal service level agreement with our customers to clarify what
systems we support, how we provide support, and what the user’s
role is. We met with the management of each division and office
to discuss the needs and expectations of each group and to review
the agreement.
Our Help Desk is our main point of contact with most
Institute staff. We implemented significant Help Desk improvements in 2000 based on recommendations from an internal review
and study of industry models. Within the first few months of the
new Help Desk operations, we exceeded our goals for call closure.
Help Desk operations are supported by a database-driven information service, visible to users through a dynamically updated web
site. (http://cisd.stsci.edu)
We supported the move of the Hubble Flight Operations
Team into the Institute by developing floor plans for the computer
room, transitioning hardware and software maintenance, developing
a system management strategy for the equipment, and providing
data validation of systems prior to shipment from Goddard Space
Flight Center. Flight operations based at the Institute began in
October 2000 and have run smoothly.
O
The ribbon cutting of CISD’s all new Help Desk
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We devoted more resources to ensuring the security of all
Institute systems in light of the increasing number of reported
threats and vulnerabilities. We work closely with NASA to
update security assessment plans, run security scans on all systems,
and review proposed changes to our computing environment.
We conducted the first technology evaluation of Institute
e-mail services, documenting the requirements, reviewing current
e-mail technology and standards, estimating the total cost of
ownership for various options, and recommending a new architecture for e-mail. We expect this new architecture will reduce
maintenance effort, improve reliability, and provide substantially
improved services for Institute staff.
We worked with Institute divisions to improve internal and
external information services. For example, we helped develop
new versions of the ACS, NICMOS, and STIS web pages, where
Hubble observers can now more easily find instrument information. From the information provider’s standpoint, the new pages
require less effort to change information. We are deploying this
approach across the Institute.
In 2000, we introduced a number of process improvements.
We now protect computer data using an automated backup
system, reducing the effort needed for routine backups and
decreasing the time to recover from data loss. We installed
an electronic fax system to permit staff to send and receive faxes
from their workstations. With the Administration Division,
we deployed an electronic timecard system, now available to
most Institute staff. We instituted a web-based system for leave
notification used by staff to communicate planned absences
to colleagues.
Also in 2000, we phased out the VMS Science Cluster.
VMS is now used solely for a few legacy operational systems.
We have begun a systematic program of upgrading PC systems
to Windows 2000 and Sun workstations to Solaris 8.
The Help Desk’s inaugural party
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we promote
scientific research
Science Directorate
We promote scientific research at the Institute, perform scientific
reviews and oversight, conduct observing time allocation, and
facilitate the communication of Hubble discoveries within the
scientific community as well as to public audiences.
The Science Directorate comprises the Science Division, the
Science Policies Division, and the Office of Public Outreach, and
manages additional support functions such as library services.
The primary responsibility of the Science Directorate is to
ensure a vigorous research environment at the Institute. This is
achieved by maintaining a preeminent scientific staff and sponsoring colloquia, workshops, fellowships, and a visitor’s program to
keep our scientists current.
The Science Directorate carries out the work needed to
recruit scientists, to evaluate them for promotion, to mentor young
scientists, to assign scientists to appropriate functional work, to
monitor the science of the missions, to support the various Institute
oversight committees, to manage the solicitation and peer review
of Hubble proposals, and to foster public understanding of science
through the Office of Public Outreach. The Science Recruitment
Committee oversees the work involved in hiring scientists, and
ultimately recommends candidates for new hires to the Senior
Science Staff and the Director. The Science Personnel Committee,
carries out the same tasks with respect to promotion and tenure
of scientists already at the Institute.
T
Hubble Fellows and Science Division Staff
at the Hubble Fellows Symposium
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Science Division
We foster the Institute as a research environment.
We supervise the functional assignments of scientists.
We promote the career growth of scientists.
We have three main goals. First, we strive to enhance the atmosphere of scientific excellence at the Institute through leadership
and initiatives. Second, we seek to provide the optimal staff
resources to other divisions by assigning AURA and ESA scientists to functional positions. Third, we foster the careers of
staff scientists, especially junior scientists, through a variety of
services, including cultivating research opportunities, providing
mentoring and professional development advice, and conducting
the annual research evaluation.
In assigning scientists to functional duties, we support division managers in their search for the best person for any position
available. We try to identify the most suitable candidates, taking
the whole career and the implications of a transfer into account.
We conduct a variety of programs to host scientific visitors
at the Institute. Our Collaborative Visitor Program supports
collaborators on research projects with Institute staff members,
typically for visits of one to four weeks. Our Journal Club
Visitor Program supports external scientists who come to give
one or more seminars during visits of typically one to two weeks.
Our Distinguished Visitor Program supports internationally
known astronomers to join the Institute for typically one month.
In 2000, we hosted one Distinguished Visitor, approximately
forty-five Collaborative Visitors, and twenty Journal Club Visitors.
We manage the Hubble Fellowship Program by selecting
new Fellows and conducting the annual appraisal for the ongoing Fellows. We arrange for the Hubble Fellows to present their
research results at a symposium held at the Institute in the fall.
We manage the Institute Postdoctoral Fellowship Program. Just
as for the Hubble Fellows, we select the Institute Fellows based
on the strength of their research proposals. Also, we host other
postdoctoral fellows and graduate students, who are at the
Institute carrying out research projects guided by members of
the scientific staff.
In 2000, we supported thirty Hubble Fellows nationwide
and hosted one at the Institute. We supported two Institute
Fellows. We hosted approximately twenty-one postdoctoral
fellows and thirteen graduate students, about half of whom were
enrolled in the Physics and Astronomy Department of The
Johns Hopkins University (JHU). The others were enrolled at a
variety of other foreign and domestic educational institutions.
We manage the Director’s Discretionary Research Fund
(DDRF), which supports short- and long-term staff research
projects as well as infrastructure investments to bolster the
Institute’s research capabilities.
We supported approximately seventy DDRF projects in
2000 with a total of $300,000, mainly to fund graduate students
and postdoctoral fellows and to enable long-term initiatives.
Each spring, we conduct a symposium on a major area
of astronomy where important new research developments are
occurring. These events have become prestigious in the astro-
nomical community for their timely choice of topics and the
quality of the invited speakers. Drawing typically 100-200 scientists to the Institute, the symposia have been praised for their
organization. We also conduct smaller-scale workshops on
specific scientific issues and topics.
We chose a broad area for the 2000 spring symposium:
“A Decade of HST Science.” About 150 participants heard invited
reviews on the major achievements of Hubble during its first ten
years. Cambridge University Press published the proceedings.
In July 2000, we hosted a topical workshop entitled “Blazar
Demographics and Physics,” which brought together about fifty
experts to address key issues related to our understanding of
these enigmatic objects.
We started a new series of informal meetings focused on hot
topics in astronomy. We designed the meeting format to foment
debate: a brief presentation of a new result followed by ample
time for freewheeling discussion. We set several objectives for
the ‘hot topic’ series, including better shared understanding of
the topic, generating new ideas, and possibly forming new
collaborations. We selected “Planets in Clusters” as the first
topic, and the discussions were well received.
We created five scientific interest groups, four of which—
Solar System and Planets, Stars and ISM/IGM, AGN and
Starbursts, Galaxies and Cosmology—expanded on topics of
the previously existing journal clubs. A fifth group, Scientific
Instrumentation, was entirely new. The leader of each group was
tasked with coordinating the group’s activities, such as organizing
workshops and seminars, identifying research opportunities, and
mentoring junior scientists.
We constituted ‘agenda groups’ to address career-related
issues for all categories of our science staff, from graduate students
to senior astronomers. The agenda groups developed a variety of
issues affecting the productivity of Institute scientists, ranging
from computer needs for graduate students to the implications
of International Traffic in Arms Regulations (ITAR) for ESA
astronomers. We coordinated the management of such issues at
regular meetings between the Division office and representatives
of the agenda groups. In 2000, we resolved about two-thirds of
the issues raised.
We conducted a pilot implementation of the new process to
evaluate the scientific research of Institute staff on an annual
basis. Staff scientists presented a brief summary of their scientific
achievements for the past year. A committee including the
Associate Director for Science, the Science Division Head, and
the chair of the Science Personnel Committee evaluated the
documentation and identified the top one-sixth science achievers
on both the tenure and parallel tracks. We awarded these scientists a salary increase and gave verbal feedback to all scientists.
We developed a mentoring program to serve junior scientists on both the tenure track and parallel track. We articulated
afresh the expectations in the mentor-‘mentee’ relationship. We
reviewed existing relationships and encouraged all scientists to
involve themselves in the mentoring program.
We performed a statistical study of timecards to determine
the amount of time that members of the scientific staff spend on
research. We found that tenure-track astronomers spend an average of about 40% of their time doing research, whereas 50% is
nominally available to them. For parallel track astronomers, the
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Science staff monthly meeting
fraction was also smaller than the nominal value of 20%. We
have encouraged division managers to protect staff research time.
We intend to revisit the issue on a regular basis.
We provided both monthly and annual reports of science
highlights from Hubble to NASA Headquarters and the Hubble
Project at the Goddard Space Flight Center. These highlights
included topics ranging from planetary nebulae to black hole
event horizons.
Science Policies Division
We manage the allocation of all Hubble Observing
time. We are the Institute point of contact with oversight committees. We conduct the selection process
for the Hubble science program and establish science
metrics to evaluate its success.
We have three standing advisory committees with terms of reference outside the Institute, and two that are creations of the
Director. The Space Telescope Institute Council (STIC), our
primary management oversight committee, is selected by and
reports to the AURA Board of Directors. The Institute Visiting
Committee (IVC) evaluates the productivity and working conditions of the staff. The IVC is selected by the Space Telescope
Institute Council and reports to NASA through AURA. The
Space Telescope Users Committee (STUC) is selected by and
reports to both the Institute Director and the NASA Project
Scientist on matters related to the utility of the telescope and the
quality of Institute services. The Telescope Allocation Committee
(TAC) is appointed by the Director to evaluate observing proposals and recommend an allocation of Hubble orbits to selected
programs. Finally, the Space Telescope Advisory Council (STAC)
is available to the Director for advice on any subject related to
the Hubble science program.
The STIC met in February, June, and November 2000.
STIC approved two cases for promotion to tenure and two
to the Senior Scientist level. It reviewed Institute initiatives
including the strategic planning process.
STIC met at ESA headquarters in June to continue a tradition of
fostering close links with our European partners on Hubble and
the Next Generation Space Telescope (NGST). This meeting
was timed to highlight ESA’s formal approval of participation in
the NGST project, which occurred in the fall.
STUC met twice in 2000, in April and October. STUC
supported the decision taken by NASA to delay the installation
of the cooling system for Hubble’s Aft Shroud until the last servicing mission. STUC members provided advice on the priorities
of future Institute developments affecting the user community.
They also tested software products for data analysis that the
Institute recently developed, and they gave valuable feedback on
the Astronomer’s Proposal Tools.
The ‘Interim’ IVC (IIVC) met in April 2000 to review the
Institute’s progress toward its annual goals and objectives and to
survey the perspectives of the Institutes staff. They noted that
Hubble continued to produce excellent science and that public
interest in Hubble remained very high. The IIVC viewed the
Institute as the key contributor to the scientific effectiveness
of the Hubble program. The IIVC found the scientific output of
the staff to be on a par with that of the top universities and
research institutions.
Science Program Selection Office | We conduct
the selection process for the Hubble science program.
Our roles in selecting the Hubble science program include issuing an annual Call for Proposals to the astronomical community,
organizing the proposal review, handling proposals for Director’s
Discretionary observing time, and formulating relevant policies.
Our goal is to enable the most important Hubble observations—
those with lasting impact on the field of astronomy—while
maintaining equity of opportunity to every proposer.
The Cycle 10 TAC and review panels met in November,
2000. The TAC reviewed proposals of 100 orbits or larger and
reviewed panel recommendations on smaller proposals to ensure
overall scientific balance between the various subdisciplines.
The panels allocated orbits to all proposals requesting fewer than
100 orbits. We encouraged medium-sized proposals (15-99
orbits) by subsidizing them in the panel reviews with extra
orbits. To encourage more submissions of larger proposals, we
had advertised these incentives in advance, including in the
Call for Proposals and the Institute Newsletter.
There were nine panels, four for Galactic astronomy, four
for extragalactic astronomy, and one for Solar System research.
Every category except Solar System had two, redundant panels,
virtually eliminating conflicts of interst and providing two
independent determinations of science priorities. We found the
same proposal acceptance rates for proposers who served as
reviewers as for those outside the process.
The TAC recommended a total of 7 large programs, for
about 20% of the total allocated prime orbits. Medium-sized
proposals participated strongly in Cycle 10, accounting for about
34% of the requested orbits and a similar percentage of the
allocated orbits. Overall, the acceptance rate was largely independent of proposal size.
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The Library
Office of Public Outreach
The Institue maintains a library with a large collection primarily
for astronomical research. The staff of three supports the physical
collection and Internet access to online journals and other computer-based resources.
At the end of 2000, our physical inventory included over
13,000 monograph and journal volumes plus hundreds of
CD-ROMs, reels of microfilm, and pieces of microfiche. This
year, we added electronic versions of two important science
magazines, Science and Nature, as well as electronic titles from
the Optical Society of America.
Use of our web pages continues to be heavy. We receive
many lending requests from other libraries—about ten for every
request we make to borrow.
We maintain the Hubble Bibliography, which at the end
of 2000 contained a total of 3137 papers making original use of
Hubble data. (http://ntweb.stsci.edu/STEPsheet/) We have
been working with librarians at other observatories to develop
standard criteria for inclusion of papers in telescope bibliographies in order to produce comparable statistics.
We develop astronomy-related educational products
and services and deliver them to classroom students,
the public, and the astronomical community. We
support individual scientists in developing educational
contributions based on their research.
Our goal is to bring the excitement—and to demonstrate the
relevance—of scientific discovery and technological advance to
the public. Our scope includes formal and informal science
education, public outreach, news products, the Origins
Education Forum, grants for education initiatives, and outreach
to the astronomical community for the Next Generation Space
Telescope (NGST).
Our development strategy is to engage scientists and engineers actively in our programs, harnessing their knowledge to
educate the public. We act as catalyst by teaming with educators,
students, and members of the general public to create educational
resources for wide distribution.
Our three community support programs are the Origins
Education Forum, education grants programs, and science
community outreach for NGST.
In 2000, we introduced a new version of our public web
site, HubbleSite and debuted our travelling exhibition, Hubble
Space Telescope: New Views of the Universe. We supported NASA’s
early-release of science observations following the successful third
servicing mission. We helped create the NASA Space Science
Education Resource Directory.
Formal Education Program | We develop educational materials that address national education standards
and are relevant to K-12 curricula. We provide pre-service
and in-service teacher training on the use of space
The Library
science educational materials in the classroom.
The heart of our effort is the Amazing Space program, which
revolves around a five-week summer workshop involving K-12
teachers, graphic artists, writers, web developers, education
evaluators, and Institute scientists and technology experts. The
workshop participants collaborate in developing online interactive modules based on Hubble, which are designed to harness
students’ fascination with space to improve their math, science,
and technical skills. After testing, we distribute these materials
nationally. We also demonstrate the materials at the professional
meetings of both teachers and astronomers, such as the National
Science Teachers Association, the National Council of Teachers
of Mathematics, the Association of Science Technology Centers,
and the American Astronomical Society. (http://amazingspace.stsci.edu/)
In 2000, we worked on two new modules for Amazing
Space. “Planet Impact” will deal with the effects of cosmic collisions, and a second module will be a mathematics activity about
random sampling and statistics using the Hubble Deep Field.
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Informal Science Education Program | We bring
the excitement of scientific discovery and technological
accomplishment to a wide audience through science
museums, planetaria, libraries, and the Internet.
OPO news team meeting
Online Outreach and Public
Information Program
We host a variety of Internet sites tailored to different audiences.
The Internet is developing into a prime source of information
for most citizens. The general public and the news media use
our sites to get first-hand information about Hubble and its
discoveries.
In 2000, our web sites received over 400 million hits in over
14 million user sessions.
In April 2000, we introduced HubbleSite, designed to
appeal to the general public. (http://hubble.stsci.edu/)
HubbleSite offers background information about the telescope’s
systems, its discoveries, and the people who use it. It hosts a
gallery of Hubble images, material from the travelling exhibitions,
and a section for Hubble-based educational games and activities.
By the end of the year, HubbleSite had received in excess of
119 million hits from over 2 million user sessions.
We responded to over 5000 e-mail and more than 1000
postal requests from the public, usually for hardcopy materials
such as photos, slides, or pamphlets.
The public’s natural curiosity about space, astronomy, and
technology creates a valuable opportunity to disseminate Hubble
results. Science museums regularly feature Hubble images and
consult with us. By frequent request, we advise science museums
and planetaria on making the most effective use of Hubble
materials in their exhibits and productions.
In 2000, we completed our collaboration with the
Smithsonian Institution to develop a traveling exhibition
entitled Hubble Space Telescope: New Views of the Universe. We
debuted the exhibition at the Adler Planetarium in Chicago in
June 2000. We introduced a smaller version of the exhibit in
Saginaw, Michigan in September. We incorporated exhibit
materials into HubbleSite to share parts of the experience with
the Internet user.
We developed ViewSpace, a series of PC-based multimedia
presentations that address the specific requirements of planetaria
and science centers and distributed them to the public.
ViewSpace combines images, digital movie and animation files,
text, and music. It plays continuously in a darkened exhibition
alcove or planetarium lobby. ViewSpace emphasizes the beauty
and wonder of Hubble imagery while placing the images in
spatial and conceptual contexts. We derived the content from
Hubble news releases and other material in our archive.
ViewSpace is now running in over fifty institutions throughout
the United States.
OPO news proof reading
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The News Program | We develop press releases,
photo releases, and Space Science Updates to
disseminate Hubble discoveries via print, electronic,
and broadcast media.
Over the years, we have crafted an effective process for producing
press events and press information packages to empower mass
media channels to disseminate Hubble news. This service is
available at various levels to all Hubble observers, to assist them
in publicizing their research.
On average, we issued over three press or photo releases
per month in 2000. We distributed electronic versions of these
releases to over 500 news organizations. We make the press
release archive available over the Internet at
http://oposite.stsci.edu/pubinfo/pr.html.
We held our annual science writers’ workshop in conjunction with the Institute’s spring symposium, which in 2000
celebrated Hubble’s tenth anniversary. We prepared a press package, a video, a special slide set, and a web site, all devoted to
summarizing Hubble’s key accomplishments over its first decade
of operation.
We facilitated about 400 science articles in major U.S.
newspapers. We also supported some 600 broadcast-media reports
and about 300 magazine articles. We also supported the production
of a Space Science Update entitled “The Secret Life of Galaxies.”
Origins Education Forum | We operate a forum to
coordinate the education and public outreach efforts of
all of the NASA missions within the Origins Theme.
NASA’s Origins Theme includes such missions as SIRTF,
SOFIA, NGST, Keck, FUSE, Hubble, and the Astrobiology
Institute. Our Origins Education Forum serves as a central
‘jump station’ for public information about these missions and
their scientific results. (http://origins.stsci.edu)
Through the Origins Education Forum, we foster collaborations between missions and match up scientists and educators for
collaborative projects. We strive to make more effective use of
NASA education funding by avoiding duplications of effort
and by identifying areas particularly in need of education and
public outreach materials.
Our special expertise in evaluating educational products and
processes has allowed us to establish a well-developed set of
methodologies and models. We offer our evaluation service to
member missions of the Origins Forum and share our evaluation
expertise with other institutions.
In 2000, we developed a partnership with the Sun-Earth
Connection Education Forum to develop the Space Science
Education Resource Directory. This is an easily searched, userfriendly online catalog of NASA space science products for use
in classrooms, science museums, planetariums, and other settings. (http://teachspacescience.stsci.edu/)
The OPO Audio-Visual Lab
Education Grant Programs | We empower
individual scientists to conduct their own education and
public outreach programs.
We manage the Initiative to Develop Education through
Astronomy and Space Science (IDEAS) program for NASA.
This program provides funding and other support for scientists
to produce educational resources and services.
In 2000, we received 33 IDEAS proposals, of which 15
were accepted for funding. The proposals originated in 21 states,
of which 11 received funding. The total funding distributed
in this cycle was $369,000. The suite of successful IDEAS programs has broad scope, variously intending to reach students,
teachers, museums, libraries, and the general public.
(http://ideas.stsci.edu/)
We also manage an education grants program for Hubble
observers. In Cycle 9, we funded 7 proposals from 6 states with
a total of $64,624.
Next Generation Space Telescope Science
Community Outreach | We provide the astronomical
community with information about NGST. We introduce
the public to NGST, presenting it as the follow-up mission
to Hubble.
In 2000, we sponsored events and prepared exhibit materials
about NGST for American Astronomical Society meetings. We
highlighted the science goals and recent progress in technology
development for NGST.
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J. R., Oosterloo, T., Price, R. M., Putman, M. E., Ryder,
S. D., Sadler, E. M., Staveley-Smith, L., Stewart, I.,
Vaile, R., Webster, R., & Wright, A. E. 1999, “New
Galaxies Discovered in the First Blind HI Survey of the
Centaurus A Group,” ApJ, 524, 612
Science Publications List
This list includes refereed papers published or submitted between October 1999 and
September 2000 by Institute staff (or by visitors, if a substantial portion of the work was
done at the Institute). Some papers published in this period may have been included as
“submitted” or “in press” in the previous annual report.
Adami, C., Holden, B., Castander, F. J., Nichol, R. C.,
Mazure, A., Imer, M. P., Postman, M., & Lubin, L.
2000,“The CFH Optical PDCS survey (COP) I: The
Data,” AJ, in press
Alcock, C., et al. 2000 “The MACHO Project LMC
Variable Star Inventory. IX. Frequency Analysis of the
First Overtone RR Lyrae Stars and the Indication for
Nonradial Pulsations,” ApJ, 542, 257
Alard, C., et al. 2000, “Mass-losing Semiregular
Variable Stars in Baade’s Windows,” ApJ, submitted
Alcock, C., et al. 2000, “The MACHO Project Microlensing Efficiency Calculation Pipeline,” ApJ, in press
Albrow, M., et al. 1999, “Caustic- Crossing Binary
Microlensing Events,” ApJ, submitted
Alcock, C., et al. 2000, “The MACHO Project:
Microlensing Optical Depth toward the Galactic Bulge
from Difference Image Analysis,” ApJ, 541, 734
Albrow, M., et al. 1999, “A Complete Set of Solutions
For Caustic-Crossing Binary Microlensing Events,”
ApJ, 522, 1022
Albrow, M., et al. 1999, “Limb-Darkening of a K Giant
in the Galactic Bulge: PLANET Photometry of MACHO
97-BLG-28,” ApJ, 522, 1011
Afonso, J., Cram, L., & Mobasher, B. 2000, “On the
Star Formation Rate and Luminosity Evolution of
Galaxies” ApJ, 536, 68
Afonso, J., Mobasher, B., & Hopkins, A. 2000, “A
Complete Micro-Jy Radio Survey,” Ap&SS, in press
Albrow, M., et al. 1999, “Limits on Stellar and
Planetary Companions in Microlensing Event OGLE1998-BUL- 14,” ApJ, submitted
Albrow, M., et al. 1999, “The Relative Lens-Source
Proper Motion in MACHO 98-SMC-1,” ApJ, 512, 672
Albrow, M., et al. 2000, “Detection of rotation in a
binary microlens: PLANET photometry of MACHO
97-BLG-4l,” ApJ, 534, 894
Albrow, M., et al. 2000, “PLANET observations of
microlensing event OGLE- 1999-BUL-23: limb darkening
measurement of the source star,” ApJ, submitted
Alcock, C., et al. 1999, “Calibration of the MACHO
Photometry Database,” PASP, 111, 1539
Alcock, C., et al. 2000, “Binary Microlensing Events
from the MACHO Project,” ApJ, 541, 270
Alcock, C., et al. 2000, “Halo Lensing or LMC
Self-Lensing? Insights from the Hubble Space
Telescope Color-Magnitude Diagram of MACHO
Microlensing Source Stars,” ApJ, submitted
Alcock, C., et al. 2000, “MACHO 96-LMC-2: Lensing of
a Binary Source in the LMC and Constraints on the
Lensing Object,” ApJ, submitted
Alcock, C., et al. 2000, “MACHO Project Limits on Dark
Matter in the 1-30 Solar Mass Range,” ApJ, submitted
Alcock, C., et al. 2000, “Searching for Periodicities in
the MACHO Lightcurve of LMC-X2,” MNRAS, 316, 729
Alcock, C., et al. 2000, “The MACHO Project 9 Million
Star Color-Magnitude Diagram of the Large Magellanic
Cloud,” AJ, 119, 2194
Alcock, C., et al. 2000, “The MACHO Project:
Microlensing Results from 5.7 Years of Large
Magellanic Cloud Observations,” ApJ, 542, 281
Alcock, C., et al. 2000, “The MACHO Project Sample
of Galactic Bulge High Amplitude delta-Scuti Stars:
Pulsation Behavior and Stellar Properties,” ApJ, 536, 798
Afonso, C., et al. 2000, “Combined Analysis of the
Binary-Lens Caustic-Crossing Event MACHO 98-SMC1,” ApJ, 532, 340
Aloisi, A., Clampin, M., Diolaiti, E., Greggio, L.,
Leitherer, C., Nota, A., Origlia, L., Parmeggiani, G., &
Tosi, M. 2000, “The Red Stellar Population in NGC
1569,” AJ, submitted
Aloisi, A., Clampin, M., Greggio, L., Leitherer, C., Nota,
A., Origlia, L., & Tosi M. 2000, “NICMOS reveals the
Details of the Old Stellar Population in the Core of NGC
1569,” in A Decade of HST Science, eds. M. Livio, K.
Noll & M. Stiavelli (Cambridge Univ. Press), in press
Barnes, D. G., Staveley-Smith, L., de Blok, W. J. G.,
Oosterloo, T., Stewart, I., Wright, A. E., Banks, G. D.,
Bhatal, R., Boyce, P. J., Calabretta, M. R., Disney, M.
J., Drinkwater, M. J., Ekers, R. D., Freeman, K. C.,
Gibson, B. K., Green, A. J., Haynes, R. F., te Lintel
Hekkert, P., Henning, P. A., Jerjen, H., Juraszek, S.,
Kesteven, M. J., Kilborn, V. A., Knezek, P. M., Koribalski,
B., Kraan-Korteweg, R. C., Malin, D. F., Marquarding,
M., Minchin, R. F., Mould, J. R., Price, R. M., Putman,
M. E., Ryder, S. D., Sadler, E. M., Schröder, A., Stootman,
F., Webster, R. L., Wilson, W. E., & Ye, T. 2000, “The HI
Parkes All Sky Survey: Southern observations, calibration and robust imaging,” MNRAS, in press
Baron, E., Branch, D., Hauschildt, P. H., Filippenko, A.
V., Kirshner, R. P., Challis, P., Jha, S., Chevalier, R.,
Fransson, C., Lundqvist, P., Garnavich, P., Leibundgut,
B., McCray, R., Michael, E., Panagia, N., Phillips, M.,
Pun, J., Schmidt, B., Sonneborn, G., Suntzeff, N., Wang,
L. F., R. V., & Wheeler, J. C., 2000, “Preliminary
Spectral Analysis of the Type II Supernova 1999em,”
ApJ, in press
Bate, M. R., Bonnell, I. A., Clarke, C. J., Lubow S. H.,
Ogilvie, G. I., Pringle, J. E., & Tout, C. A. 2000,
“Observational implications of precessing protostellar
discs and jets,” MNRAS, 317, 773
Baumgartner, W. H., Horner, D., Gendreau, K. C.,
Scharf, C. A., Molnar, S., & Mushotzky, R. F. 1999, “A
Catalog of X-ray Cluster Redshifts,” A&AS, 195, 1004
Beckwith, S. V. W. 2000, “Vom Urknall zum Leben die
Entstehung von Komplexität im Universum,” in Wie
entstehen neue Qualitäten in komplexen Systemen? ed.
G. Plehn & R. Gerwin, (Vandenhoeck & Ruprecht), 29
Beckwith, S. V. W., Henning, Th., & Nakagawa, Y.
2000, “Dust Properties and Assembly of Large Particles
in Protoplanetary Disks,” in Protostars and Planets IV,
eds. V. Mannings, A. P. Boss, & S. S. Russell,
(University of Arizona Press), 533
Bell, E. F., Barnaby, D., Bower, R. G., De Jong, R. S.,
Harper, D. A., Hereld, M., Loewenstein, R. F., &
Rauscher, B. J. 2000, “The Star Formation Histories of
Low Surface Brightness Galaxies,” MNRAS, 312, 470
Alves, D. 2000, “K-Band Calibration of the Red Clump
Luminosity,” ApJ, 539, 732
Bennett, J., Donahue, M., Schneider, N., & Voit, G. M.
1999, The Cosmic Perspective: Brief Edition, (AddisonWesley Longman)
Alves, D., Bond, H. E., & Livio, M. 2000, “Hubble Space
Telescope Observations of the Planetary Nebula K 648
in the Globular Cluster M15,” AJ, 120, 2044
Biersdorfer, P., Lisse, C. M., & Olson, R. 2000,
“Laboratory Simulation of Cometary X-ray Emission,”
Science, submitted
Alves, D., Bond, H. E., & Onken, C. 2000, “CCD
Photometry of the Globlular Cluster NGC 5986 and its
Post-Asymptotic-Giant-Branch and RR Lyrae Stars,”
AJ, in press
Birriel, J. J., Espey, B. R., & Schulte-Ladbeck, R. E.
2000, “Simultaneous UV and Optical Observations of
Direct and Raman-scattered OVI Lines in Symbiotic
Stars,” ApJ, in press
Alves, D. & Nelson, C., 2000, “The Rotation Curve of
the Large Magellanic Cloud and the Implications for
Microlensing,” ApJ, in press
Blair, W. P., Morse, J. A., Raymond, J. C., Kirshner, R.
P., Hughes, J. P., Dopita, M. A., Sutherland, R. S., Long,
K. S., & Winkler, W. P. 2000, “HST Observations of
Oxygen-rich Supernova Remnants in the Magellanic
Clouds.” II.: Elemental Abundances in N132D and
1E0102. 2-7219 ApJ, 537, 667
Armitage, P. & Livio, M. 2000, “Black Hole Formation
via Hypercritical Accretion,” ApJ, 532, 540
Ayal, S., Livio, M., & Piran, T. 2000, “Tidal Disruption of
a Solar Type Star by a Supermassive Black Hole,” ApJ,
in press
Bakos, G., Sahu, K. C., & Nemeth, P. 2000, “Revised
Coordinates and Proper Motions of the Stars in the
Luyten Half-Second Catalog,” ApJS, in press
Banks, G., Disney, M. J., Knezek P. M., de Blok, E.,
Kilborn, V., Barnes, D. G., Bhatal, R., Ekers, R. D.,
Freeman, K., Gibson, B. K., Haynes, R. F., Henning, P.,
Jerjen, H., Kilborn, V., Koribalski, B., Malin, D. F., Mould,
Blair, W. P., Sankrit, R., Raymond, J. C., & Long, K. S.
1999, “Distance to the Cygnus Loop from Hubble
Space Telescope Imaging of the Primary Shock Front,”
AJ, 118, 942
Bohlin, R. C. 2000, “Comparison of White Dwarf
Models with STIS Spectrophotometry,” AJ, 120, 437
Böker, T. & Allen, R. J. 1999, “Imaging and Nulling with
the Space Interferometer Mission,” ApJS, 125, 123
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Budavari, T., Szalay, A. S., Connolly, A. J., Csabai, L, &
Dickinson, M. 2000, “Creating Spectral Templates from
Multicolor Redshift Surveys,” AJ, 120, 1588
Donahue, M. & Voit, G. M. 1999, “Omegam from the
Temperature-Redshift Distribution of EMSS Clusters of
Galaxies,” ApJ, 523, L137
Georgakakis, A., Mobasher, B., Cram, L., & Hopkins, A.
1999, “The Pairing Fraction of Faint Radio Sources: The
Phoenix Survey,” MNRAS, 310, L15
Calzetti, D., Armus, L., Bohlin, R. C., Kinney, A. L.,
Koornneef, J., Storchi-Bergmann, T., & Wyse, R. F. G.
2000, “The Dust Content and Opacity of Actively StarForining Galaxies,” ApJ, in press
Donahue, M., Voit, G. M., Scharf, C. A., Gioia, I. M.,
Mullis, C. R., Hughes, J. P., &, Stocke, J. T. 1999, “The
Second Most Distant Cluster of Galaxies in the
Extended Medium Sensitivity Survey,” ApJ, 527, 525
Georgakakis, A., Mobasher, B., Cram, L., Hopkins, A.
Lidman, C., & Rowan-Robinson 1999, “Optical and
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