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January 1997

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Volume 14, Number 1

SPACE TE LESCOPE SCIENCE INSTITUTE
Highlights of this issue:

Newsletter
Astronomy with HST

· AURA science and functional awards to Leitherer and Hanisch -- pages 1 and 23 · Cycle 7 to be extended
-- page 5

· Cycle 7 approved program listing -- pages 7-13

Climbing the Starburst Distance Ladder
C. Leitherer
Massive stars are an important and sometimes dominant energy source for a galaxy. Their high luminosity, both in light and mechanical energy, makes them detectable up to cosmological distances. Stars ~100 times more massive than the Sun are one million times more luminous. Except for stars of transient brightness, like novae and supernovae, hot, massive stars are the most luminous stellar objects in the universe. Massive stars are, however, extremely rare: The number of stars formed per unit mass interval is roughly proportional to the -2.35 power of mass. We expect to find very few massive stars compared to, say, solar-type stars. This is consistent with observations in our solar neighborhood: the closest really massive star is the O4 supergiant (~50 solar mass) Puppis at a distance of about 500 pc; large volumes need to be sampled to observe significant numbers of massive stars. Our Galaxy does not qualify as a starburst, which is a term denoting powerful star formation events in galaxies. Even the most luminous starforming regions in our Galaxy are tiny on a cosmic scale. They are not dominated by the properties of an entire population but by individual stars. Therefore stochastic effects prevail. Extinction represents a severe problem when a reliable census of the Galactic high-mass star-formation history is atempted, especially since massive stars belong to the extreme Population I, with correspondingly small vertical scale heights. Moreover, the proximity of Galactic regions -- although advantageous for detailed studies of individual stars -- makes it difficult to obtain integrated properties, such as total emission-line fluxes of the ionized gas. Nevertheless, observations in the Galaxy allow us to study individual massive stars in great detail -- an important consideration before venturing out to distant populations. The Carina region (= NGC 3372) hosts one of the more spectacular highmass star formation regions in the Galaxy. Its proximity of about 2 kpc permits detailed studies of the stellar content. Several O3 stars have been found in Trumpler 14/16. They are the earliest and most massive species in the MK classification scheme. HD 93128, HD 93129A, HD 93205, and HDE 303308 have masses around 100 solar masses. The enigmatic object Carinae is located in this region as

Figure 1. Composite B, V, I WFPC2 (PC) image of NGC 1741 obtained by P. Conti, in collaboration with the author and W. Vacca. Field size is 35 arcsec. North is up and east to the left. well. Car is a luminous blue variable (LBV), a short evolutionary phase when a substantial fraction of stellar mass is shed and ejected into the ISM.

Editor's Note: Each year AURA makes two awards to the staff of STScI, one for scientific achievement, and one for functional performance. This year's science award went to Dr. Claus Leitherer, who provided the accompanying article on his work. The functional award was to Dr. Robert Hanisch, and his article appears later in this Newsletter.

30 Doradus: the Rosetta Stone
High-mass star-formation regions in the Local Group of galaxies are excellent laboratories to study starbursts: their proximity (with respect to galaxies in the Hubble flow) permits detailed studies of individual
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ST ScI Newsletter

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Director's Perspective

Director's Perspective

T

he Cycle 7 TAC has now met and given its recommendations on the programs it reviewed that should be carried out on HST after the new instruments are installed. Notification letters to the PIs of all submitted proposals giving the TAC/panels recommendations should be received by early January. Not surprisingly, a number of Cycle 7 programs will make use of the long-slit and UV capabilities of STIS and the IR

capabilities of NICMOS to make observations that were not possible before, and which are certain to produce interesting research in a number of areas. The TAC, chaired this cycle by Dr. Mike Shull of the Univ. of Colorado, considered a number of large programs for implementation given that all of the previous Key Projects will soon have been completed, and it recommended time for one of them. To be carried out under the supervision of G. Gilmore of IOA, Cambridge, this program will obtain images of clusters in the Large Magellanic Cloud to construct color-magnitude diagrams of the systems. According to the new policy governing large programs recommended by the Institute Advisory Committee, the TACs of all succeeding cycles may recommend the allocation of time for up to as many as three large programs (>100 orbits) each cycle. Launch of the second HST servicing mission, STS-82, is soon upon us. Preparations have been proceeding nominally, and both instruments are ready for installation in the telescope. Concerted efforts have already been underway for some time among the HST Project, the Institute, and the NICMOS and STIS instrument teams to prepare for bringing the new instruments on- line and commencing with their in-flight calibration. As was done after the first servicing mission an Early Release Observations program will be carried out, coordinated by Dr. A. Saha, which should give early demonstration of the capabilities of the new instruments. Thus some scientific results from the refurbished HST should be forthcoming a few months after the mission. Institute staff are working with Goddard scientists and others to plan the next phase of studies for the Next Generation Space Telescope, the follow-up mission to HST recommended by AURA's "HST and Beyond" Committee. We have also decided to sponsor, jointly with GSFC, a conference devoted to the scientific program for a mission having the characteristics defined in the mission studies recently completed. Initial plans are to hold the meeting at Goddard in early April 1997; details will be available by the time of the Toronto AAS meeting in January. We hope for broad community participation to build appreciation for the promise of this mission.

Bob Williams, Mike Hauser

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January 199 7

Starburst Distance

from page 1

stars, yet their distance (with respect to Milky Way clusters) makes it possible to obtain integrated properties as well. Although more luminous than Galactic regions, they are still underluminous in comparison with the starburst prototypes below. Numerous studies of the Rosetta Stone 30 Dor (with its ionizing cluster NGC 2070, whose massive center is R136) exist. Crowding becomes severe for stellar spectroscopy in the central R136 region. HST allows spatially resolved aperture spectroscopy of individual stars. Ultraviolet spectra of several hot, luminous stars suggest temperatures above 40 000 K, luminosities around 106 LSun, and masses above 50 MSun. The wind properties are particularly outstanding. Strong P Cygni profiles of C IV, N V, and He II indicate high mass loss at rates of 10-5 MSun per year and above. These wind lines are strong enough to be detectable in even the most distant starburst galaxies, as will be discussed below. The interstellar environment in 30 Dor differs from that of smaller Galactic H II regions. Galactic regions, such as Trumpler 14/16 are not massive enough to form significant numbers of massive stars having strong stellar winds at the same evolutionary epoch, whereas in 30 Dor the collective effort of winds and supernovae is capable of initiating and maintaining large interstellar bubbles and supershells. The shell masses range from a few hundred to several thousand solar masses. The mechanical energy requirements are around 1051 erg. Supernovae, and possibly stellar winds, are the likely sources of energy. If 30 Dor were observed at 10 Mpc, only HST could perform spatially resolved imaging and spectroscopy of R136, which would subtend an angle of only 0.05 arcsec.

Figure 2. Ultraviolet spectral region of NGC 1741. Left: Observed spectrum taken with the GHRS. Right: Synthetic spectrum computed for a 5 Myr old instantaneous starburst following a Salpeter IMF. The main diagnostic lines of Si IV and C IV agree.

Starburst galaxies
Detailed spectroscopic studies of large numbers of individual stars are no longer feasible beyond a few Mpc:
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ST ScI Newsletter Science Institute ·HST Space Telescope · Astronomy with Newslette r

Starburst Distance

from page 3

even the visually brightest star in Trumpler 14, HD 93129A, would appear at 1 Mpc as a V=18.6 star (assuming no extinction). The closest examples of the so-called starburst galaxy class are found in this distance range. Starburst galaxies form large numbers of massive stars that have a global effect on the galaxy, both in terms of their radiant and their mechanical energy output. What would 30 Dor and the LMC look like if they were a factor of 1000 farther away? Figure 1 gives the answer. NGC 1741 is a luminous irregular at a distance of 50 Mpc, highly reminiscent of the LMC when seen on wide-angle photographs. It has two luminous H II regions at the NW end of the bar. The bar population is largely unresolved. NGC 1741 contains about 103 highly evolved Wolf-Rayet stars -- more WR stars than known individually in all galaxies of the Local Group combined.

Individual stars (or even clusters) can no longer be investigated at distances of ~50 Mpc and beyond. Stellar and nebular properties are derived from the integrated light. A GHRS spectrum of the starburst region containing the WR population is shown in Figure 2 (left). The most conspicuous stellar lines are C IV, Si IV, N V, and He II. These lines have broad absorptions and/or emissions due to their origin in stellar winds from hot stars and permit a study of the hotstar population. A theoretical spectrum is also shown in this figure (right). It was calculated with a population of massive stars following a Salpeter IMF for masses above ~15 MSun (lower mass stars may also be present), and extending up to ~100 MSun; about 104 O-type stars are inferred from the ultraviolet luminosity.

Star formation at the edge of the universe
We conclude with a brief look at the most distant star-forming galaxies known. They are the endpoint of our cosmic voyage, which began in the Carina star forming region. Few

starburst galaxies have been studied in detail at large redshifts. Detecting galaxies in their initial star-formation stage (often called primeval or protogalaxies) has been a major goal in observational cosmology during the past years. This goal has eluded almost everybody until very recently, when several groups independently announced the detection of promising candidate galaxies forming stars at high redshift. In all cases the presence of ultraviolet stellar-wind lines, such as those seen in Figure 2, was taken as evidence for massive stars. The Hubble Deep Field (HDF) is an HST program to image an indistinguished field at high Galactic latitude in four passbands as deeply possible. The image shows a plethora of distant field galaxies, many of them having complex and disturbed morphologies. Spectroscopy of these star-forming candidates is required for analysis, an effort reaching the limits of our current observational capabilities. Possibly these observations will find the first generation of massive stars ever formed in the universe.

HST Recent Release: A Survey of Quasar Host Galaxies
Quasars reside in a variety of galaxies, from normal to highly disturbed. When seen through ground-based telescopes, these compact, enigmatic light sources resemble stars, yet they are billions of light-years away and several hundred billion times brighter than normal stars. The following Hubble Space Telescope images show examples of different home sites of all quasars. But all the sites must provide the fuel to power these unique light beacons. Astronomers believe that a quasar turns on when a massive black hole at the nucleus of a galaxy feeds on gas and stars. As the matter falls into the black hole, intense radiation is emitted. Eventually, the black hole will stop emitting radiation once it consumes all nearby matter. Then it needs debris from a collision of galaxies or another process to provide more fuel.

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HST Programs and Observations

Duration of Cycle 7
R. Williams and P. Stanley
Most HST proposal/observing cycles have been approximately one year long. In fact, the community has expressed a desire for the Institute to try to fix established dates during the calendar year for the receipt of proposals, and we have adhered to this for the past two cycles. This becomes impractical in cycles for which there are servicing missions because of the fact that each servicing mission requires a 4-month period, called Servicing Mission Observatory Verification (SMOV), when the telescope and its new instruments and components must be brought on-line, thoroughly checked out, and initially calibrated. Maintaining the one year length of a cycle would therefore require that the science program of the cycle last only 8 months. A shortened science period for Cycle 7 would have required submission of proposals for Cycle 8 before much experience had been acquired with the new instruments STIS and NICMOS. We considered a shortened science program for Cycle 7 but the quality of proposals received and the oversubscription rate were so high that we felt it compelling to have Cycle 7 consist of a full year of science observations. With the nominal 4-month period devoted to SMOV following the SM2 launch, this leads to a slip in our schedule for Cycle 8. Cycle 7 science observations should commence in July, 1997, as we complete the schedule of Cycle 6 programs. The Call for Proposals for Cycle 8 is now scheduled to be issued in October, 1997, with a proposal receipt date in early February, 1998. We realize that the calendar used for Cycles 6 and 7 may have been more convenient for the writing and submission of proposals, but we have tried to establish new calendar dates for the proposal process in Cycle 8 that will also not be too inconvenient. Cycle 8 observing will run from November, 1998, to November, 1999.

Panel and TAC Members for Cycle 7
Telescope Allocation Committee
Mike Shull, Chair

TAC At-Large Members
TAC AT-Large Members Art Davidsen - JHU Anne Kinney - STScI Bohdan Paczynski - Princeton Anneila Sargent - Caltech Don York - U. Chicago

PANELS
AGN 1

The following individuals served on the Cycle 7 Time Assignment Committee. We thank them for their help in the difficult job of selecting the HST science program.

Bradley Peterson - Ohio State (Panel Chair) Buell Jannuzi - NOAO/KPNO Grzegorz Madejski - GSFC Simon Morris - Dominion Astro. Obs. John Mulchaey - Carnegie Obs. Marcia Rieke - U.Arizona/Steward Thomas Soifer - Keck Observatory Clive Tadhunter - U. of Sheffield, UK Mark Whittle - U.Virginia

AGN 2
Rachel Webster - U. of Melbourne, Australia (Panel Chair) Michael Eracleous - U. of CA, Berkeley Gary Ferland - U. of Kentucky Mauro Giavalisco - Carnegie Obs. Frederick Hamann - U. of CA George Rieke - U. Arizona Steward Obs Joseph Shields - U. of Ohio Stefan Wagner - Heidelberg, MPA, Germany Donald Schneider - Penn State Beverley Wills - U. of Texas

Binary Stars
Jonathan Grindlay - Harvard Obs (Panel Chair) Paul Hertz - Naval Research Lab Janusz Kaluzny - Warsaw Anthony Moffat - U. of Montreal Mirek Plavec - U. of CA Paula Szkody - U. of Washington Marten van Kerkwijk - Caltech Janet Wood - Keele University

Clusters
Richard Mushotzky - GSFC (Panel Chair) Thomas Broadhurst - UC, Berkeley Jack Burns - NMSU Hans Hippelein - MPIA Tod Lauer - KPNO/NOAO Gerard Luppino - University of Hawaii Ann Zabludoff - Carnegie Obs.
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ST ScI Newsletter SciencePrograms andNObservations Space Telescope · HST Institute · ewslette r

PANELS

from page 5

Cosmology
George Efstathiou - U. of Oxford-Astrophysics (Panel Chair) Arif Babul - NYU Lennox Cowie - U. of Hawaii Andrew Hamilton - U. of Colorado Saul Perlmutter - LBL Robert Schommer - CTIO Peter Schneider - MPI Joe Silk - U. of CA, Berkeley Gary Wegner - Dartmouth College

Edward Fitzpatrick - Princeton Thomas Henning - ESA (Jena, Germany) Elizabeth Lada - U. of Florida Manuel Peimbert - UNAM

Quasar Absorption Line
Craig Hogan - U. of Washington (Panel Chair) Stefano Cristiani - ESA Observatory Dipadova James Lowenthal - Lick Obs Michael Rauch - Caltech Gregory Shields - U. Texas Lisa Storrie-Lombardi - Carnegie Observatory Art Wolfe - U. of CA, San Diego

Cool Stars
Andrea Dupree - SAO (Panel Chair) Howard Bond - STScI David Gray - U. of Western Ontario Philip Ianna - U. Virginia Ruth Peterson - Lick Observatory Catherine Pilachowski - KPNO/NOAO Neill Reid - Caltech Klaus Strassmeier - Vienna U., Austria Nicholas Suntzeff - CTIO

Stellar Ejecta
Robert Fesen - Dartmouth College (Panel Chair) Dave Arnett - U. of Arizona, Steward Observatory Bruce Balick - U. of Washington William Blair - JHU Claes Fransson - ESA, Stockholm Obs Bruce Hrivnak - Valparaiso U. Margaret Meixner - U. of Illinois John Raymond - Cfa Steve Shore - IN U.

Galaxies 1
Rob Kennicutt - U. of Arizona, Steward Obs. (Panel Chair) Jay Frogel - OSU Jeff Kenney - Yale David Merritt - Rutgers Colin Norman - JHU/STScI Renzo Sancisi - Kapteyn Astronomical Ins Francois Schweizer - Carnegie/DTM Jacqueline van Gorkom - Columbia Dennis Zaritsky - UCSC

Stellar Populations
Gerard Gilmore - Inst of Astr. (Panel Chair) Bruce Carney - U. of North Carolina Eileen Friel - National Science Foundation Douglas Geisler - NOAO/KPNO Deidre Hunter - Lowell Obs Chris Sneden - U. Texas at Austin Donald Terndrup - Ohio State Monica Tosi - ESA, Bologna Obs Bruce Twarog - U. of Kansas

Galaxies 2
Rosie Wyse - JHU (Panel Chair) Stephane Charlot - IAP William Keel - U. Alabama Carmelle Robert - U. Laval Barbara Ryden - OSU John Salzer - Wesleyan David Sanders - U. Hawaii David Van Buren - Caltech

Solar System
Philip Nicholson - Cornell University (Panel Chair) Gordon Bjoraker - GSFC Wendy Calvin - USGS Flagstaff Anita Cochran - U. of Texas Jean Claude Gerard - U. of Liege Al Harris - JPL Hal Weaver - JHU Robert West - JPL

Hot Stars
Rolf-Peter Kudritzki - U. of Munich-I for A&A (Panel Chair) Bruce Bohannan - KPNO/NOAO Martin Cohen - U. of CA, Berkeley John Drilling - Louisiana St Mario Livio - STScI Wolf-Rainer Hamann - U. of Potsdam Gloria Koenigsberger - UNAM Rex Saffer - Villanova

Young Stars and Circumstellar Material
Charles Lada - SAO (Panel Chair) Fred Adams - U. of Michigan Mary Barsony - UC Riverside Chas Beichman - IPAC Ian Gatley - NOAO Bill Herbst - Wesleyan University Anne-Marie LaGrange - Grenoble Observatory Erick Young - U. of Arizona

Instellar Medium
Carl Heiles - U. of CA, Berkeley (Panel Chair) Donald Cox - U. WI-Madison

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AGN 1
Archival Study of Nuclear Morphology in Interactive Galaxies Testing the Supermassive Black Hole Paradigm in Nearby Radio-Quiet AGNs Spectra to Constrain the Dynamics of Clouds in the Narrow-Line Region of NGC 1068 Continuous Ultraviolet Monitoring of NGC 3516 The connection between the obscuring torus and masing disk in H_2O Megamasers Snapshot survey of the B2 sample of radio galaxies An Archival Study of Nearby, Low-Luminosity Active Galactic Nuclei Measuring Black Hole Masses in Broad-Lined AGNs Kinematics of the HAlpha Nuclear Disk in M81: A Search for a MBH in the Nearest LINER Intrinsic UV and X-ray Absorption in QSOs High Resolution IR Imaging Survey (IRIS) of the Centers of the Nearest Active Galaxies The Relation Between Quasar Luminosity and Host Galaxy Mass The Fueling of Active Nuclei: A NICMOS Snapshot Survey of Seyfert and Normal Galaxies The Nature of Nuclear Activity in Nearby Galaxies A New Technique for Photometry of Low Luminosity AGNs Using HST Reference Images Infrared imaging and polarimetry observations of the obscured nucleus of Centaurus A The nature of the compact infrared core sources in powerful FRII radio galaxies STIS Spectroscopy of Markarian 78 Kinematics of the Helical Jets in the Seyfert Galaxy ESO428-G14 The Molecular Torus and Ionized Gas in the Circinus Galaxy

Approved Observing Programs for Cycle 7

Borne Bower Cecil Edelson Falcke Fanti Filippenko Filippenko Ford Hamann Malkan McLeod Mulchaey Rix Romanishin Schreier Tadhunter Whittle Wilson Wilson

Hughes STX National Optical Astronomy Observatories University of North Carolina at Chapel Hill University of Iowa Astronomy Department, University of Maryland Universita di Bologna University of California, Berkeley University of California, Berkeley Johns Hopkins University Center for Astrophysics & Space Science University of California Smithsonian Astrophysical Observatory The Observatories of the Carnegie Institution of Washington Steward Observatory University of Oklahoma Space Telescope Science Institute University of Sheffield University of Virginia Astronomy Department University of Maryland

Continued

AGN 2

2 Secular Changes in the Jet of M87 High Redshift Reflection Nebulae The Stellar Content of Powerful Radio Galaxies: A NICMOS Survey of 0.8 < z < 1.8 3CR Sources Kinematics of Gaseous Disks in the Nuclei of Liners with Compact Flat Spectrum Radio Sources The cosmological evolution of quasar host galaxies FeII Emission in Quasars Testing the Nature of Type 2 LINERs Using UV Spectroscopy The Unusual Absorption Line System of PG 2302+029 -- Ejected or Intervening? Chemical Abundances in QSO Broad Absorption Line Regions A Search for Broad Absorption Lines in Narrow-Line Seyfert 1 Galaxies NICMOS Imaging Survey of Distant Radio Galaxies: Ellipticals at z > 2 ? NICMOS Observations of PKS1413+135 Quasar Candidates in the Hubble Deep Field Witnessing the Birth of Radio Galaxies: WFPC & NICMOS Observations of CSOs Polarization mapping of the infrared emission from the jet in M87 Microarcsecond Imaging of a Gravitationally Lensed QSO: 2237+0305 HST WFPC2 Observations of MilliJansky Radio Sources from the FIRST Survey

Biretta Chambers Dey Dressel Dunlop Ferland Ho Jannuzi Junkkarinen Leighly McCarthy McHardy Osmer Stocke Thomson Webster White

Space Telescope Science Institute Institute for Astronomy Kitt Peak National Observatory RJH Scientific, Inc. University of Edinburgh University of Kentucky Center for Astrophysics National Optical Astronomy Observatories University of California, San Diego Columbia University The Carnegie Observatories University of Southampton The Ohio State University University of Colorado, Boulder University of Hertfordshire University of Melbourne Space Telescope Science Institute

Binary Stars
The nature of the bright Supersoft X-ray Source RX J 0019+21 WFPC2 Observations of Astrophysically Important Visual Binaries High-Speed UV Spectroscopy of the Ultracompact Binary 4U 1626--67/KZ TrA Narrow band imaging of jets and bipolar outflows from symbiotic stars High resolution UV spectroscopy of the extra-ordinary central star of Abell 35 The Dense Core of M30

Beuermann Bond Chakrabarty Corradi Drew Edmonds

Universitaets-Sternwarte Goettingen Space Telescope Science Institute Massachusetts Institute of Technology Instituto de Astrofisica de Canarias Astrophysics Group, Imperial College Space Telescope Science Institute

January 1997

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ST ScI Newsletter
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HST Programs and Observations

Espey Grindlay Harrison Kaper Knigge Margon Margon McClintock Rousseau Sams Schmidt Shara Shara Still Teeseling Vrtilek

The Johns Hopkins University Harvard University New Mexico State University European Southern Observatory Space Telescope Science Institute University of Washington University of Washington Smithsonian Astrophysical Observatory Universitaets-Sternwarte Goettingen Max Planck Insitute fuer Astrophysics Steward Observatory, University of Arizona Space Telescope Science Institute Space Telescope Science Institute University of St. Andrews Universitaets-Sternwarte Goettingen Smithsonian Astrophysical Observatory

Improved Emission Line Diagnostics of Symbiotic Stars Deep Survey for CVs and Compact Binaries in the Collapsed Core Cluster NGC6397 The Distances to Dwarf Novae, and the Calibration of the Technique of Infrared Spectroscopic Parallax Raman scattering and X-ray ionization in LMC X-4, Cyg X-1, and LMC X-1 Demystifying the SW Sex stars The Nature of Two New Optical Counterparts of Globular Cluster X-ray Sources Intense Galactic X-ray Sources in Crowded Fields Black Hole A0620-00 and Advection-Dominated Accretion UV Cyclotron Spectroscopy of the High-Field Polar UZ Fornacis Jet Polarization and Emission lines in the Galactic Microquasar GRS1915+105 Probing the 230 MG Accreting Magnetic White Dwarf in AR Ursae Majoris Recovery and Characterization of Old Novae in the Globular Clusters M80 and M14 An Archival Search for Erupting Dwarf Novae in Globular Clusters High resolution imaging of magnetically-propelled ejecta from the cataclysmic variable AE Aqr van Ultraviolet spectroscopy of the supersoft X-ray source RX J0439.8-6809 High Resolution Ultraviolet Spectroscopy of Hercules X-1/HZ Herculis

Approved Observing Programs for Cycle 7

Clusters of Galaxies

Continued

Blandford Broadhurst Dalcanton Donahue Fabian Ferguson Franx Fruchter Keel Mackie Owen Ratnatunga Rosati Saunders Squires

Caltech Astronomy Dept The Observatories of the Carnegie Institution of Washington Space Telescope Science Institute Institute of Astronomy, University of Cambridge Space Telescope Science Institute Kapteyn Institute Space Telescope Science Institute University of Alabama Smithsonian Institution Astrophysical Observatory NRAO Carnegie Mellon University Johns Hopkins University Mullard Radio Astronomy Observatory Center for Particle Astrophysics

Galaxy Masses from Cluster Arcs Modeling Cluster Mass Distributions Elliptical Galaxy Evolution at High Redshift: IR Imaging of 100 Distant Clusters Warm Molecular Hydrogen in Cluster Cooling Flow Nebulae The central mass profile in the lowest redshift cluster lenses Intergalactic Stars in the Virgo Cluster Fundamental Plane, Morphology-Density Relation, and Lensing in the z=0.83 Cluster MS1054--03 The Luminosity Function and Evolution of Rich Clusters to z ~ 1.0 The Age and Content of a (Proto)Galaxy Cluster at z=2.39 Structural Properties of Brightest Cluster Galaxies in the HST Archive The Impact of Cluster Substructure on Galaxies: A Case Study in Abell 2125 Quantitative Morphology of Cluster Galaxies : Evolutionary Trends Probing Low Density Cluster Environments at Moderate-to-High Redshifts The most powerful gravitational lens Dark Matter Distribution in A2218 from Gravitational Lensing

Cosmology
Improved Hubble Constant from the 0957+561 Gravitational Lens Spheroidal Galaxy Evolution The Nature of Faint, Blue, I-K>4 Galaxies: Age or Dust? A study of the gravitational lensing potential in MG 0414+0534 Deep UV Imaging of the Hubble Deep Field IR Surface Brightness Fluctuations of Fornax Cluster Galaxies High-resolution IR and optical imaging of the fields around a large sample of z > 4.5 quasars The Nature of Galaxies in the HDF from HST Structural and Keck Kinematical Measurements NICMOS observations of JVAS/CLASS gravitational lenses Determination of the Extragalactic Distance Scale Spatial Structures and Masses of Faint Field Galaxies Survey of Gravitational Lenses as Cosmological Tools Calibration of the Cepheid P-L Relation with Observations of the Maser-Host Galaxy NGC 4258 NICMOS Extragalactic Parallel Grism Survey The Nature of Red Outlier Galaxies: Age vs Dust

Bernstein Broadhurst Davis Falco Ferguson Graham Hu Illingworth Jackson Kennicutt Koo Lehar Maoz McCarthy Moustakas

University of Michigan University of California, Berkeley University of California Smithsonian Astrophysical Observatory Space Telescope Science Institute University of California, Berkeley University of Hawaii, Institute for Astronomy Lick Observatory, University of California, Santa Cruz Jodrell Bank, University of Manchester Steward Observatory Lick Observatory, University of California, Santa Cruz Smithsonian Astrophysical Observatory University of California, Berkeley The Carnegie Observatories University of California


Moller Perlmutter Readhead Sandage Schmidt Shara Smail Tanvir Tonry Tsvetanov Turner Windhorst Yahil Zepf

Space Telescope Science Institute Lawrence Berkeley Laboratory California Institute of Technology Observatories of the Carnegie Institution of Washington Mount Stromlo and Siding Spring Observatories Space Telescope Science Institue Durham University Institute of Astronomy Institute for Astronomy Johns Hopkins University Princeton University Observatory Arizona State University, Dept. of Physics & Astronomy University at Stony Brook University of California, Berkeley

STIS images of 48 damped LyAlpha galaxies Cosmological Parameters Omega and Lambda from High-Redshift Type Ia Supernovae NICMOS observations of the gravitational lens 1608+656 Calibration of Nearby Type Ia Supernovae as Standard Candles: The Next Three-Year Step The Hubble Diagram for Distant Supernovae: Measuring Cosmic Deceleration and Global Curvature The nature of the extragalactic UV background An Unbiased Redshift Survey of Ultra-Faint Galaxies The distance to M96 from H-band Cepheid observations The SBF Hubble Diagram The Surface Brightness Fluctuations and Globular Cluster Populations of Virgo Ellipticals Gravitational Lensing Enhanced NICMOS Imagery of a Young, Rapidly Evolving Faint Blue Galaxy NICMOS imaging of MuJy radio sources with R>= 29: The birth of AGN in pregalactic objects at z>=6-10? Image Reconstruction and Photometry of the Hubble Deep Field Determining Peculiar Motions by Observing Cepheids at 3,000 km/s

Approved Observing Programs for Cycle 7

Cool Stars

Continued

Basri Bennett Boehm-Vitense Bookbinder Brown Clayton Dupree Edvardsson Evans Franz Golimowski Henry Jordan Leinert Linsky Lopez Parsons Peterson Peterson Peterson Reid

University of California University of Colorado Astronomy Department, University of Washington Smithsonian Astrophysical Observatory California Institute of Technology Louisiana State University Smithsonian Astrophysical Observatory Uppsala Astronomical Observatory Smithsonian Astrophysical Observatory Lowell Observatory Johns Hopkins University Space Telescope Science Institute University of Oxford, Department of Physics (Theoretical Physics Max-Planck-Institut fuer Astronomie JILA Observatoire de la Cote d'Azur Computer Sciences Corporation Astrophysical Advances Astrophysical Advances Astrophysical Advances California Institute of Technology

Ultraviolet Line Eclipses by Extra-Solar Planets The 1997/98 Eclipse of VV Cephei Chromospheres and transition layers in Hyades and Pleiades F stars Eclipse Mapping of the Touchstone Binary System YY Gem A Search for Zodiacal Dust around Bright Nearby Stars Dust Formation Around R Coronae Borealis Stars: Where is the CO? Direct Imaging of Betelgeuse Boron in the extreme Pop II star HD 140283 The Mass of the Classical Cepheid ADS 14859 The Masses of the Brown Dwarf Candidate GL 623B and of the Low Luminosity Binary GL 831 A Near-Infrared Search for Very Low Mass Companions to Stars within 10 pc of the Sun Calibrating the Mass-Luminosity Relation at the End of the Main Sequence Epsilon Eri: Structure and Non-Thermal Heating Infrared spectroscopic study of the very low mass triple system LHS 1070 Physical Processes in Stellar Atmospheres: Comparative Analysis of the Sun and Alpha Cen A Infrared Imaging of the Dust Shell Structures of the Mira Stars o Ceti and R Leo Fixing the Mass of the Bright Giant HD 173764 Chromospheric Activity in Old Stars: Halo Subdwarfs' Variability Mass Loss in Globular Cluster Giants: NGC 6752 Chromospheric Activity in Old Stars: HD 106516 Low-mass Halo Binaries

Galaxies 1

Allen Bershady Carollo Crotts Geisler Heap Ibata Ibata Kuijken O'Connell Odewahn

Space Telescope Science Institute A Photometric Atlas of the Bright Galaxies , in the Deepest HST Fields The Pennsylvania State University The Internal Kinematics of Distant Spiral Galaxies: Evolution of the Mass-to-Light Ratio Johns Hopkins University The nuclear kinematics of kinematically distinct cores Columbia University Understanding Halo Microlensing and Variable Stars in M31: 1) Snapshot Survey of Candidates Kitt Peak National Observatory The Metallicity Distribution of the Globular Cluster Systems of Giant Elliptical Galaxies NASA/Goddard Space Flight Center UV Spectral Dating of Galaxies Dept. of Physics & Astronomy, Univ. of British Columbia Proper Motion of the Sagittarius Dwarf Galaxy Department of Physics and Astronomy, University of British Columbia Velocity Structure in High Redshift Galaxies Kapteyn Institute Nuclear kinematics and stellar population gradients in the recent merger remnants NGC 7252 & NGC 3921. University of Virginia Spatially-Resolved Spectroscopy of the UVX in Elliptical Galaxies Arizona State University Fourier-Based Neural Network Galaxy Classifiers: Archival studies of field galaxy evolution

January 1997

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ST ScI Newsletter
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Olszewski Peacock Peletier Richstone Silk Stiavelli van der Marel Zaritsky

Steward Observatory, Univ of Arizona Royal Observatory Edinburgh Kapteyn Astronomical Institute University of Michigan University of California, Berkeley Space Telescope Science Institute Hubble Fellow, Institute for Advanced Study University of California, Santa Cruz

Absolute Proper Motions of Nearby Dwarf Spheroidal Galaxies Structures and colours of the oldest galaxies at redshift 1.5 The formation of bulges of spiral galaxies: , Central visual-infrared color gradients Black Holes and the Centers of Galaxies The Globular Cluster Luminosity Function Near-IR properties of the bulges of spiral galaxies Nuclear brightness profiles of merger remnants: do mergers form ellipticals ? A Search for Extended Stellar Galactic Halos

HST Programs and Observations

Galaxies 2
The inner region of the starburst galaxy NGC5102. The Rise of Blue Nucleated Galaxies: Evidence for Merger-Induced Evolution? Star Formation, Mass Distribution and Dark Matter in Galaxies at z ~ 0.6 From Globular Clusters to Tidal Dwarfs: Structure Formation in Tidal Tails Star Formation in a Protogalaxy Candidate at z=2.72 Structures of Starburst Galaxies Heap NASA/Goddard Space Flight Center Do Massive Star Clusters Form in Young and Weak Galaxy Interactions? Sizes and Structures of Faint Blue Compact Galaxies that are New Candidates for Proto-Spheroidal Galaxies The Stellar Content Of Giant HII Regions Dwarf Elliptical Galaxy Snapshot Survey II The Fossil Starburst in M82 Young Globular Clusters in Merger Remnants -- Part 4 Spiral Structure and OB Star Formation in M51

Approved Observing Programs for Cycle 7

Beaulieu Bershady Casertano Charlton Ellingson Gallagher Evolution of Galaxies Keel Koo Leitherer Miller O'Connell Schweizer Scoville

Johns Hopkins University Penn State University Space Telescope Science Institute The Pennsylvania State University University of Colorado University of Wisconsin-Madison

Morphological and Spectral

University of Alabama Lick Observatory, University of California, Santa Cruz Space Telescope Science Institute Department of Terrestrial Magnetism University of Virginia Carnegie Institution of Washington California Institute of Technology

Continued

Hot Stars
The White Dwarf Luminosity Function in NGC 188 Sakurai's Novalike Object: Real-Time Monitoring of a Stellar Thermal Pulse NGC 2363 V1: a rare case of major LBV eruption The Masses of the O-type Binary 15 Monocerotis UV Spectroscopy of Wolf-Rayet-Type Central Stars in the Magellanic Clouds Resolving sdB binary systems HST observations of the DAB white dwarf HS 0209+0832: testing explanations for the DB gap The Changing Wind Structure of the Erupting SMC WN/LBV system HD 5980 The Wind-momentum Luminosity Relationship for M31 and M33 B-supergiants Dust Formation in Hot Stellar Winds: Infra-Red Imaging of the Wolf-Rayet Binary WR137 LONG SLIT OBSERVATIONS OF THE WR CENTRAL STAR OF THE LMC-PN N66 A Continuing Snapshot Survey for Compact Stellar Groups and Clusters around Wolf-Rayet Stars White Dwarf Stars in Visual Binaries: Testing Stellar Degeneracy Evidence from Boron for Massive Star Evolution Compact Stellar Groups in the 30 Doradus Nebula and their Nebular Environment Parallax, Proper Motion, and Spectral Energy Distribution of an Isolated Old Neutron Star A Critical Test of Crystallization in White Dwarf Stars

Bolte Bond Drissen Gies Hamann Heber Jordan Koenigsberger Kudritzki Moffat Pena Shara Shipman Venn Walborn Walter Winget

University of California, Santa Cruz Space Telescope Science Institute Universite Laval Georgia State University Lehrstuhl Astrophysik, Universitaet Potsdam Astronomisches Institut der Universitaet Erlangen- Nuernberg Universitaet Kiel, Institut fuer Astronomie und Astrophysik Instituto de Astronomia UNAM Universitaets-Sternwarte Muenchen Universit e de Montr eal Instituto de Astronomia, Universidad Nacional Autonoma de Mexico Space Telescope Science Institute University of Delaware Macalester College Space Telescope Science Institute State University of New York University of Texas at Austin

ISM
Interfaces Between Hot and Cold Gas: The Superbubble N51D in the LMC High-Velocity Gas and Dust Evolution in Chamaeleon Clouds Studies of the Characteristics of the Interstellar Medium in the Carina Nebula

Bomans Boulanger Danks

University of Illinois at Urbana-Champaign Institut d'Astrophysique Spatiale Hughes STX/GSFC


Guhathakurta Haller Herbig Holberg Keenan Linsky Meyer Rubin Savage Sembach Walsh Walter Walterbos Walterbos

UCO/Lick Observatory, University of California, Santa Cruz Steward Observatory, University of Arizona University of Hawaii University of Arizona The Queen's University of Belfast JILA Northwestern University NASA Ames Research Center University of Wisconsin-Madison The Johns Hopkins University Space Telescope European Coordinating Facility South Carolina State University New Mexico State University New Mexico State University

Probing the Fine-Scale Structure and Colors of Interstellar Cirrus Clouds Distribution of Forbidden Iron Fe II Emission at the Galactic Center Imagery of IC 349 A STIS Probe of Unique ISM Lines-of-Sight Having Measured H and He Ionization Fractions Spectroscopy of the interstellar medium in the Magellanic Bridge Exploring the Outer Heliosphere with STIS The Physical Characteristics of Small-Scale ISM Structure HST Observations of Orion -- Probing the Origin of Abundance Anomalies in H II Regions Abundances and Physical Conditions in the Low and Intermediate Velocity Gas Toward Mu Columbae The Origin of Highly Ionized Gas in the Milky Way and Its Relationship To Large Galactic Structures Parallel high resolution imaging of diffuse objects in the Magellanic Clouds UV-Optical Spectra and Imagery of the Bubble Nebula NGC 7635 Massive Stars as Ionization Sources for Diffuse Ionized Gas in Spiral Galaxies The Stellar Populations Inside Expanding HI Shells in the Spiral Galaxy M33

Approved Observing Programs for Cycle 7

Quasar Absorption Lines

Continued

Barcons Bechtold Bregman Burles Cohen Cote Deharveng Hogan Lanzetta Lowenthal Malkan Pettini Reimers Smette Steidel Stocke

Instituto de Fisica de Cantabria (CSIC-UC) Steward Observatory, University of Arizona University of Michigan University of California San Diego University of California, San Diego ESO Laboratoire Astronomie Spatiale University of Washington State University of New York at Stony Brook UCO/Lick Observatory University of California Royal Greenwich Observatory Hamburger Sternwarte Kapteyn Astronomical Institute California Institute of Technology University of Colorado, Boulder

CIV in extensive gaseous halos of QSO Lyman alpha absorbing galaxies Molecular Hydrogen in the Damped LyAlpha Absorber of Q1331+170 Cooled Gas in X-Ray Emitting Elliptical Galaxies Measurement of the Cosmological Baryon to Photon Ratio Observations of a BL Lacertid with a Unique Absorption Line System Galaxy Rotation Curves at Large Radius using Ly-alpha Absorption Lines A snapshot survey for UV bright Quasars at redshift below 3 Helium Absorption by Protogalactic Gas The Chemical Content of the Universe at z < 1.6 H-alpha Imaging of an Elusive Damped Ly-alpha cloud at z=0.6 The Nature of the Damped LyAlpha Absorbers -- A New Study of Young Galaxies The Primordial Abundance of Deuterium From a Metal-Poor Damped Lym= an=20 Alpha System STIS Snapshot Search for UV-bright High Redshift Quasars Gravitational Lensing by Damped Ly-Alpha Absorbers NICMOS Imaging of QSO Absorption--Selected Galaxies at z > 1 Origin and Physical Conditions in the Local Ly-alpha Forest

Stellar Ejecta
Spatially-resolved FUV Spectra of the Primary Shock in the Cygnus Loop Hyperfine Induced Transitions as Probes of Low Density Plasmas STIS observations of Eta Carinae: Good spectral coverage at last Observations of Circumstellar UV Absorption Lines from the Neutral Envelopes of Planetary Nebulae Abell 39 -- The Theoretician's Nebula Confronts The Theoreticians A WFPC2 Search for Surviving Binary Companions in SN Ia Remnants High-Resolution Imaging of Ejecta Knots in the Cassiopeia A SNR Sher #25 in NGC 3603: A Galactic counterpart of SN 1987 A's progenitor Expansion Parallax Distances to Planetary Nebulae Far UV Echelle Spectroscopy of Ejecta in SN1006 Collimation of Astrophysical Jets: The Proto-Planetary Nebula He 3-1475 Continuation of Temporal Monitoring of the Crab Synchrotron Nebula High Resolution Imaging and Spectroscopy of Cool Hypergiants Near the Top of the HR Diagram SINS: The Supernova INtensive Study - Cycle 7 Unscrambling the Egg and Other Young Planetary Nebulae Infrared H_2 imaging of the highly symmetric proto-stellar jets HH212 and HH111

Blair Brage Davidson Dinerstein Ferland Fesen Fesen Grebel Hajian Hamilton Harrington Hester Humphreys Kirshner Latter McCaughrean

Johns Hopkins University University of Lund University of Minnesota University of Texas at Austin University of Kentucky Dartmouth College Dartmouth College Astronomisches Institut der Universitaet Wuerzburg United States Naval Observatory JILA University of Maryland Arizona State University University of Minnesota Harvard College Observatory NASA Ames Research Center Max-Planck Institute for Astronomy

January 1997

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ST ScI Newsletter
·

Morse O'Dell Panagia Ringwald Sahai Winckel

University of Colorado Rice University Space Telescope Science Institute The Pennsylvania State University Jet Propulsion Laboratory, California Institute of Technology Instituut voor Sterrenkunde, K.U.Leuven

The Distribution of Heavy Elements in Supernova Ejecta Spectrophotometry and Imaging of Cometary Knots in the Helix Nebula The TRUE three-dimensional structure of the Eta Carinae nebula A Snapshot Survey of Nova Shells CRL2688: The Rosetta Stone for the Evolution of AGB Red Giants into Bipolar Planetary Nebulae Van Understanding the Red Rectangle and its central binary HD 44179

HST Programs and Observations

Approved Observing Programs for Cycle 7

Stellar Populations

Continued

Bennett Bragaglia Cook Da Costa Fullton Landsman Lennon Massey Meylan Oestlin Paresce Seitzer Skillman Smecker-Hane Sosin Tosi van Altena van Altena Worthey WYSE

University of Notre Dame Osservatorio Astronomico Bologna Lawrence Livermore National Laboratory Mt Stromlo & Siding Spring Observatories Space Telescope Science Institute Hughes STX Universitaets-Sternwarte Munich National Optical Astronomy Observatories European Southern Observatory Astronomiska observatoriet European Southern Observatory University of Michigan University of Minnesota University of California University of California, Berkeley Osservatorio Astronomico di Bologna Yale University Yale University University of Michigan Johns Hopkins University

Snapshot Survey of Microlensed Source Stars White Dwarf Distance and Precision Age for Globular Clusters Halo Microlens Source Systems and their Underlying Stellar Backgrounds The Horizontal Branch of the M31 Dwarf Spheroidal Companion And III Ages of extreme metallicity globular clusters near the Galactic Center A Complete Sample of Hot Post-AGB Stars in Globular Clusters Understanding high-redshift and starburst galaxies: A UV spectroscopic survey of O-stars in the SMC The Evolution of Massive Stars as a Function of Metallicity: Closing the Loop Observationally Precise Astrometry in the Core of the Globular Cluster 47 Tuc: A Complete Census of High-Velocity Stars A Search For Old Stars in IZw18 Searching for Low Mass Stars: the Mass Function at the Hydrogen Burning Limit Extragalactic Open Clusters: A Catalog of Clusters in M31 and M33 Star Formation Histories of Dwarf Irregular Galaxies II: the Old Populations of IC 1613 and Sextans A The Star-Formation History of the Large Magellanic Cloud A Snapshot Survey of Galactic Globular Clusters NGC 1705: a Benchmark for Galaxy Evolution Tangential Velocities of Globular Clusters: Preliminary Analysis for First-Epoch Material Internal Velocity Distribution in Globular Clusters NICMOS Imaging of Red Giants in M32 The Low Mass Stellar Luminosity Function in Dwarf Spheroidal Galaxies

Solar System
H-Lyman Alpha Emission from the Upper Atmosphere of Uranus Study of Jovian Dynamics by Combining Global and Temporal HST Observations with Galileo Data Albedos and Sizes of Planetary Ring Particles HST Far-UV Imaging and Spectra of Jupiter's Aurora Coordinated with GALILEO Triton's Atmospheric Structure: Problems with Present Models Triton's Distorted Atmosphere A Campaign to Determine the CO and CO_2 Abundances in Cometary Nuclei Saturn's Rings Mapping of the H_2 Emission and Color Ratio in the Jovian Aurora Composition and Heterogeneity of Io's Volcanos from Polarimetry of Their Thermal Emission Jovian Planetary Waves Synoptic Monitoring of Seasonal Phenomena on Mars The nucleus of comet 55P/Tempel-Tuttle, the parent of the Leonid Meteors Spatially resolved multispectral investigation of Titan's troposphere and stratosphere Mineralogic Mapping of Asteroid 4 Vesta Saturn's Satellites: Alteration of the Surface by Ion Irradiation on Enceladus and Tethys Spatial Distribution of Ozone and Sulfur Dioxide on Ganymede and Europa The mass ratio of Charon to Pluto Global Mapping of Molecular Oxygen on Ganymede Multispectral Investigation of Dynamics and Cloud Structure on Neptune

Ballester Beebe Bosh Clarke Elliot Elliot Feldman French G erard Goguen Harrington James LAMY Lemmon McCarthy Noll Noll Olkin Spencer Sromovsky

University of Michigan New Mexico State University Lowell Observatory University of Michigan Massachusetts Institute of Technology Massachusetts Institute of Technology The Johns Hopkins University Wellesley College Universite de Liege Jet Propulsion Laboratory NASA Goddard Space Flight Center/National Research Council University of Toledo Laboratoire d'Astronomie Spatiale Lunar and Planetary Laboratory The University of Arizona Space Telescope Science Institute Space Telescope Science Institute Lowell Observatory Lowell Observatory University of Wisconsin


Tomasko Weaver Weaver West Wolff Zappala

Lunar and Planetary Lab Johns Hopkins University Johns Hopkins University Jet Propulsion Laboratory, California Institute of Technology Space Science Institute Osservatorio Astronomico di Torino

Uranus' Vertical Haze Structure and its Variation with Latitude Investigating Volatile Depletion in Two Periodic Comets: 2P/Encke and 103P/Hartley 2 Systematic Investigation of C/1995 O1 (Hale-Bopp) : Part 3 Jovian Global Photometry During the Galileo Epoch A New Look at Martian Ice Clouds A search for main-belt binary asteroids

Approved Observing Programs for Cycle 7

Young Stars and Circumstellar Material

Continued

Brandner Carr Figer Ghez Hartigan Hartmann Kalas Lagrange Mathieu McCaughrean Meyer Mundt Najita Padgett Reipurth Simon Simon Stapelfeldt Terebey Weintraub Wood Zinnecker

Astronomisches Institut der Universitaet Wuerzburg Naval Research Laboratory University of California, Los Angeles University of California Los Angeles Space Physics & Astronomy, Rice University Smithsonian Astrophysical Observatory Max-Planck-Institute for Astronomy laboratoire d'Astrophysique; BP53X University of Wisconsin - Madison Max-Planck-Institute for Astronomy Max--Planck--Institut fuer Astronomie Max-Planck-Institut fuer Astronomie Center for Astrophysics Jet Propulsion Laboratory European Southern Observatory State University of New York State University of New York Jet Propulsion Laboratory California Institute of Technology Vanderbilt University University of Wisconsin Astrophysikalisches Institut Potsdam

An HST/NICMOS search for young brown dwarfs and giant planets Water in Protoplanetary Disks Compact Young Clusters and the r^-2 Cusp near the Galactic Center Circumbinary Disks: Tracing the Mass and Energy Transfer in Young Binary Systems The Interaction of Accretion Disks with Protostellar Binaries The Dusty Environments of Protostars NICMOS and WFPC2 Imaging of a New Beta Pic-like Circumstellar Dust Disk STIS observations of Beta Pictoris Dynamical Masses for the Stars in the Pre-Main- Sequence Spectroscopic Binary 045251+3016 Multi-wavelength imaging of circumstellar disks in the Orion Nebula Probing the Very Low Mass IMF: Brown Dwarf Stars in Star--Forming Regions Spectroscopic Imaging of CW Tau -- Clues to the Structure and Collimation of T Tauri Star Winds The IMF Below 1M odot in Young Clusters: 1.9Mum H_2O Band Imaging of IC348 NICMOS Imaging of Young Stellar Object Circumstellar Nebulosity Thackeray's globules in IC 2944: HAlpha imaging with WFPC2 Orbits of Pre-Main Sequence Binaries The Nature of T Tau S T Tauri Star Snapshot Survey: A Census of Protoplanetary Disks The Small Scale Structure of Protostellar Disks and Infall Envelopes Coronagraphic, Polarimetric Imaging of T Tau with NICMOS The Morphology Of Protostellar Environments The low-mass pre-MS stellar content of the 30 Dor starburst cluster

Country

Total 1298 297

Australia Belgium(*) Brazil Canada Chile China Denmark(*) France(*) Germany(*) India Israel Italy(*) Japan Mexico Netherlands(*) New Zealand South Africa Spain(*) Sweden(*) Switzerland(*) United Kingdom(*) United States

(*) ESA member state

GO and AR Statistics of PI by country

14 3 2 31 2 2 1 37 78 2 7 33 4 4 23 1 3 18 13 4 105 911 3 2 0 4 1 0 0 5 24 0 0 4 0 2 4 0 0 2 3 0 15 228

Submitted Approved

January 199 7

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ST ScI Newsletter SciencePrograms andNObservations Space Telescope · HST Institute · ewslette r

Proposal Statistics by Panel
AGN1 AGN2 Proposals Received
GO SNAP AR 80 8 5 90 6 10 65 9 3 79 5 10 75 8 4 47 3 8 79 7 15 76 6 3 66 3 1 49 1 6 68 6 2 92 2 1 104 4 6 88 0 7 86 4 1 1144 72 82

BIN

COS

CS

CLUS

GAL1

GAL2

HS

ISM

QAL

SE

SP

SS

YS

TOTAL

Proposals Accepted
GO SNAP AR 14 3 3 14 0 3 20 0 2 22 0 7 18 3 0 9 1 5 12 2 5 11 1 2 14 2 1 13 1 3 13 3 0 21 1 0 16 2 2 24 0 2 20 1 1 241 20 36

Primary Orbits Requested
1243 1859 923 2475 1062 1230 1750 1304 810 822 1957 1241 2452 1203 1403 21734

Panel Fraction of Total Accepted
8% 9% 4% 13% 5% 5% 8% 4% 4% 3% 8% 7% 9% 5% 7% --

Primary Orbits Accepted
253 301 148 442 169 174 280 144 148 103 255 218 289 157 223 3304

Fraction of Orbits Accepted/Requested
20% 16% 16% 18% 16% 14% 16% 11% 18% 13% 13% 18% 12% 13% 16% 15%

ESA PIs Accepted
2 3 8 4 4 3 4 1 4 3 6 5 6 3 8 64

ESA Primary Orbits Accepted
7 68 30 49 29 56 49 12 38 15 59 21 94 14 94 635

Fraction of ESA Orbits Accepted
3% 23% 20% 11% 17% 32% 18% 8% 26% 15% 23% 10% 33% 9% 42% 19%

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January 199 7

Preparatory Support Available For Funded Programs
Ray Beaser
Many Cycle 6 General Observers using the WFPC2 and the FOC had their Programs delayed until after the servicing mission in February. Due to a funding shortage, no preparatory grants were awarded for Cycle 6 funded Programs. Funds for those Programs were to be released only after the first observation was obtained for each Program. However, we heard from numerous investigators that funding delay is creating substantial financial problems. After reviewing the improved funding situation for the current fiscal year, the Director decided to authorize preparatory funding of up to 10% of the approved allocation for GOs who need to prepare for the receipt of Cycle 6 data. We realize that this will not solve the financial problems of GOs, but we hope it will be of some help. E-mail will be sent shortly to the GOs who are affected informing them of the availability of preparatory funding. GOs may send their requests for preparatory funding directly to the E-mail address of the Grants Administration Branch: grantinfo @stsci.edu. The request should include a description of the specific preparatory activities which need to be accomplished prior to the receipt of data. Please note that because of the improved availability of funding, the Director also approved the award of 10% preparatory funding for Cycle 7 General Observers.

Electronic Submission of Performance Reports
Ray Beaser
In a continuing effort to improve our procedures and to decrease the administrative burden on investigators, interim and final Performance reports may be submitted electronically to the following address:
goarperform@stsci.edu

Reports sent by e-mail to the above address are automatically sent to the Grants Administration Branch and to several scientists for review. An automatic reply will be sent acknowledging the receipt of the report. If you need a performance report template, please send e-mail to the above address typing "send template" in the subject line. If you have any questions concerning the submission of the report, please send e-mail to grantinfo @stsci.edu or call (410) 338-4200.

HST Recent Release: Hubble Images Reveal Supersonic Comet-like Objects in the Heart of Galaxy
Researchers analyzing the Hubble Space Telescope's dramatic pictures of the Cartwheel galaxy have discovered immense comet-like clouds of gas speeding through the heart of the galaxy at nearly 300 km s-1. This close-up image of the galaxy's nucleus reveals the comet-like knots of gas. These knots are mostly confined to the core's left side and appear as white streaks inside the blue ring. The "heads" are a few hundred parsec across; the tails are more than ~1 kpc light-years long, the longest of which is nearly 15 kpc. The structures look like comets because they probably were spawned by a collision between high-speed and slower-moving material. This collision created an arrowhead-shaped pattern called a bow shock, which is similar to the wake of a boat speeding across a lake. Credits: Curt Struck and Philip Appleton (Iowa State University), Kirk Borne (Hughes STX Corporation), and Ray Lucas (Space Telescope Science Institute), and NASA

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ST ScI Newsletter Science Institute · Mission r Space Telescope · Second Servicing Newslette

Second Servicing Mission

SM2

HST's Second Servicing Mission--Overview
Carl Biagetti
Launch of NASA's Space Shuttle Discovery is currently scheduled for 13 February 1997. Discovery is the name of Orbiter Vehicle No. 103 and the Shuttle flight is listed as STS-82. At the highest level, the mission has two primary goals: 1) the enhancement of HST's science capabilities by installation of two new orbital replacement instruments (ORIs), and 2) enhancement of HST's long-term scientific productivity through the replacement of failed or degraded orbital replacement units (ORUs) with new technology units. The two new ORIs are of course NICMOS and STIS, both designed as HST axial instruments. NICMOS is an advanced infrared camera, developed by the University of Arizona, that will enable the HST to exceed the sensitivity and spatial resolution in the near-IR of both present and planned ground based facilities. STIS, developed by the NASA's Goddard Space Flight Center (GSFC), enhances HST's spectrographic capabilities by providing simultaneously wide spectral coverage and high spectral resolution, including long-slit imaging with an emphasis on the ultraviolet. More technical information on the development status of these two new instruments is found elsewhere in this newsletter. NICMOS will replace the FOS in HST's instrument bay 2. STIS will replace the GHRS in bay 1. Both NICMOS and STIS are equipped with their own special optics designed to correct for the spherical aberration of HST's primary mirror, and, as a result, will not require the correction provided by the Corrective Optics Space Telescope Axial Replacement (COSTAR), which was installed during the first servicing mission in December, 1993. Therefore, after a nominal SM2, COSTAR's only purpose will be the optical correction for the Faint Object Camera (FOC). The FOC and the Wide Field Planetary Camera 2 (WFPC2), which also has its own corrective optics, along with NICMOS, STIS, and the Fine Guidance Sensor (FGS) system, will form the new complement of HST science instruments (SIs). In addition to STIS and NICMOS, there are a variety of ORUs which provide the upgrades for failed or degraded units. First, FGS-1 will be replaced with an upgraded flight spare. All three FGSs have shown, to one degree or another, evidence of degradation that implies the need for eventual replacement of at least one of them in order to maintain the FGS system's astrometric and vehicle guiding capabilities. (See the last issue of this Newsletter for more details on the FGS problems the decision to replace FGS-1.) The flight spare is upgraded with an adjustable mirror designed to compensate for the spherical aberration of HST's primary optics. The Data Interface Unit No. 2 (DIU-2) will be replaced with an upgraded version of the same device. The DIUs provide common command and data interface between the Data Management Unit and other HST equipment. During SM1, DIU-2 suffered a Side-A failure caused by an over-voltage state resulting from a power conditioning unit (PCU) relay failure. The replacement unit will have over-voltage protection circuitry to help prevent the recurrence of this type of problem. The HST's data recording and playback systems will be extensively serviced. The current system consists of three Engineering/Science Tape Recorders (ESTRs), each with a capacity of about 1 .2 gigabits, used to record and play back HST science and engineering telemetry. ESTR-1 has exhibited several tape-speed anomalies and ESTR-2 had experienced problems with reliability of track 2 recording before, experiencing what is apparently a hard failure. These anomalies, combined with the increased data demands during NICMOS and STIS operations, dictate an upgrade to a new system. Current plans are to replace ESTR-2 with a flight spare and ESTR1 with a solid state recorder (SSR). The SSR is a prime example of a "new-technology" upgrade. It will have a 12-gigabit capacity and will offer the considerable operational advantages of simultaneous record and playback and simultaneous recording of science and engineering data to a single device. Finally, the Solar Array Drive Electronics No. 2 (SADE-2) will be replaced by the original SADE-1 unit, removed during SM1 and refurbished with heat sinks to prevent the recurrence of problems it experienced on orbit. SM2, as currently planned, is a tenday mission with a seven-person crew led by Commander Ken Bowersox (See the October issue of this Newsletter for more on the crew members and their September visit to the Institute). The shuttle launch is scheduled for 13 February 1997. The current launch window is between 7:59 to 9:00 UT (2:59 - 4:00 am EST). A little less than two days after launch, the HST will be configured for capture while the Space Shuttle approaches for rendezvous, capture, and berthing. On flight day 4, the astronauts will begin the first of four scheduled six-hour extravehicular activities (EVAs), one per day, during which they exit to the Shuttle bay to go about the work of HST refurbishment. The first EVA is dedicated to the installation of both STIS and NICMOS, in that order. (Note that these activities include the removal of the GHRS and FOS during the same EVA.) The second EVA
continued page 17

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January 199 7

Space Telescope Imaging Spectrograph (STIS) Update
Stefi Baum
After an extended (4.5 month!) period of ground characterization and testing, STIS passed its preship review and was packed up and shipped to Kennedy Space Center on December 10. At the Cape, STIS will go through its final paces before insertion in the Shuttle for its February 13, 1997, launch. The final months of STIS's ground calibration were carried out at GSFC, in both air and nitrogen purge. The science data obtained during the ground calibration showed that STIS should meet or exceed its scientific expectations, almost across the board, with the detectors performing beautifully, the measured sensitivities as predicted to within ~20%, the optical performance (Line Spread Functions and Point Spread Functions) outstanding, and the throughput at Lyman-alpha showing no signs of temporal degradation due to contamination. The extended period of STIS operations also provided an opportunity to test the STIS Flight Software. Problems were identified and fixed, with several open areas still under investigation. During the GSFC ground calibration, extensive work was done characterizing and trying to optimize the CCD performance, as well as obtaining much needed CCD and NUV-MAMA data to build the basic reference files for calibration (e.g., flats, darks, dispersion solutions). Considerable effort was devoted to trying to understand the nature of the fringing and extended PSF halo seen at long ( > ~8000 å) wavelengths with the CCD, to optimize observing strategies for NIR observations. Excellent high signal-to-noise flat fields were produced for the NUVMAMA. For the FUV-MAMA, the lack of additional calibration time in vacuum and the slightly different nature of the detector suggest that only rudimentary flats will be available for the FUV-MAMA at launch. A more complete set of flats for the FUVMAMA will be obtained once STIS flies, most likely early on in the Cycle 7 calibration program. Plans for the Servicing Mission Orbital Verification (SMOV), to be carried out between deployment and June, 1997, are in full development now. STIS will be characterized on orbit in an extensive SMOV with roughly 50 proposals, and ~350 orbits (predominantly internals) planned, leading up to the July 1, 1997, start of Cycle 7 science. Characterization on orbit starts first with the CCD and is followed a month later with the start of MAMA characterization, once sufficient vacuum is obtained to allow turn on of the MAMA high voltage. STIS was heavily subscribed for Cycle 7 science, with fully 1/2 of the accepted GO proposals being STIS prime. At STScI, we have been preparing for the STIS GO era, with contact scientists now assigned to all the proposals and activity to ready our ground systems for STIS science continuing at a near-frenzied pace. To allow us time to react to the many changes coming out of STIS's extended ground calibration and to give us time to ready our systems and our understanding for GOs, STIS GOs will find staggered CCD and MAMA Phase II deadlines. CCD-only STIS Phase II proposals are due on March 25, with STIS MAMA (or MAMA plus CCD) proposals due later: May 1, 1997. STIS GOs can expect to receive updates with our latest knowledge and advice roughly 6 weeks prior to the Phase II deadlines. Just two months to launch and six months to the first STIS GO science now!

SM2 Overview

from page 16

includes the installation of the new FGS and its associated optical control electronics kit, thereby achieving the highest-priority mission items within the first two EVA periods. ESTR-2 will also be replaced during the second EVA. EVA 3 is dedicated to the DIU-2 replacement and the SSR installation. The SADE-2 replacement will be

performed in EVA 4, the last of the planned EVAs. As a result, all refurbishments are scheduled for completion by the end of flight day seven. The next day, HST is unberthed and, after its aperture door is re-opened, is released and separated from the Shuttle. NASA's Goddard Space Flight Center (GSFC) re-

establishes control of the observatory while the Shuttle stays aloft for two more days, de-orbiting and landing about ten full days after launch. The mission thus designed allows for one contingency EVA and one deployment contingency.

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ST ScI Newsletter Science Institute · Mission r Space Telescope · Second Servicing Newslette

NICMOS
K. Noll
The successful installation of the Near Infrared Camera and MultiObject Spectrograph (NICMOS) on HST will add significant new infrared observing capabilities to the observatory. Preparations for the inauguration of this new instrument are continuing. NICMOS successfully passed centifuge testing at Goddard Space Flight Center and has been returned to the test facilities at Ball Aerospace. Both optics and electronics tests have confirmed nominal performance. Installation of flight software and testing for the set of pre-defined MULTIACCUM sequences (see below) has been completed. Current plans are for NICMOS to arrive at Cape Canaveral by the end of December. After additional testing NICMOS will proceed to the payload processing facility in mid-January. A final cool down to 50 K will take place 5 days prior to launch. Updated information on preparing NICMOS proposals was mailed to successful cycle 7 proposers. This information is also available on the STScI World Wide Web site under the NICMOS page. (The NICMOS home page can be found at http://
www.stsci.edu/ftp/ instrument_news/NICMOS/ topnicmos.html ) In the update the

new MULTIACCUM sequences were described, recommendations for thermal background observations were made, and small revisions to suggested

parallel observing strategies were announced. Based on a review of accepted proposals, we now expect that the MULTIACCUM readout mode will be the most heavily used of the available readout modes. Observers will be required to use one of a set of sixteen pre-defined readout sequences in order to receive calibrated dark frames for their observations. These sequences have been designed to cover the complete range of desireable observing sequences and are described in detail both in the Phase II proposal instructions and in Instrument science reports, both available on the STScI WWW site. Observations using NICMOS longward of 1.7 microns will be background limited. It will be possible to remove thermal backgrounds by obtaining background measurements using either dithering or chopping patterns to move the telescope is steps as large as 24 arcminutes. Although we will not be able to measure the stability of the thermal environment in the telescope until after launch, we currently recommend that observers who work at background-limited wavelengths obtain a background measurement after every 5 minutes of on-source integration. Updated recommendations based on on-orbit performance will be posted on the STScI WWW site under the NICMOS instrument page.

Because NICMOS has a limited lifetime, it is important to maximize the scientific return by taking advantage of all significant observing opportunities. Observers who are making long exposures of ten minutes or more in a single camera are required to add parallel observations in the remaining two cameras. Details of how to do this are contained in the NICMOS Instrument Handbook and the GO update, both available on the STScI WWW site. An cut-and-paste example of a completed attached parallel program and other example programs are available on the NICMOS Web pages. NICMOS observers, like those using other instruments on HST, will be supported by a designated contact scientist (CS) and a program coordinator (PC). The CS will be one of the NICMOS instrument scientists and will be able to help with questions concerning instrument capabilities and observing strategies. The PCs are members of PRESTO, the scheduling branch within STScI, and are experts in the use of RPS2 proposal processing software. The PCs will also handle most of the detailed preparation and scheduling of your proposal. Both the CS and PC will be familiar with your proposal and should be the first people you turn to for help.

Late News: As this Newsletter goes to press an addition has been made to SM2 plans.

A late addition to EVA3 is the swap out of Reaction Wheel #1 with a flight spare. This change-out is occasioned by recent glitches with RW1 that have resulted in observatory safings. While the spacecraft can operate with only 3 of its complement of 4 reaction wheels, slewing takes much longer with an overall loss of observing efficiency. And since it cannot operate with only 2 reaction wheels, which are designed as orbital replacement units, the decision has been made to make the relatively straightforward changeout in the third EVA. A reboost of HST's orbit using the Vernier Reaction Control System jets will be attempted in three separate steps, after each of the last three EVAs. The lower thrust of the VRCS system is necessitated by the fact that the solar arrays remain deployed during the servicing mission. The reboost, expected to amount to approximately 5 or 6 miles, is expected to minimize the reboost needed in the 1999 mission, which occurs during the solar maximum.

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January 1997

Instrument News
FGS Status
FGS3 astrometry performance is nominal. The completed cycle 6 calibrations include the red transfer reference scans, the spatial and long-time-scale dependence of the transfer function, and the monthly position-mode stability checks (for field angle distortion monitoring). Blue transfer reference scan calibrations and some special servicing mission calibrations will execute in January. The Space Telescope Astrometry Team (STAT) is continuing to monitor the position mode stability. We graciously welcome Ed Nelan who has joined Olivia Lupie as an FGS instrument scientist. His work for the Astrometry team over the last several years has been crucial and and Ed will be instrumental in implementing the STAT Pos mode pipeline (semi-automated reduction of Position mode data) at the STScI. FGS3 performance issues which are under investigation are the optical field angle distortion stability (STAT), and temporal stability of the S curves (STAT, STScI). Plans for 1997 include introduction of FGS data paper products which incorporate jitter and diagnostic data, enhancement of the STScI Trans mode pipeline, installation of the POS mode pipeline, and recalibation of the astrometer after the servicing mission. The new FGS (FGS1R) has been shipped to Cape Kennedy to await the February shuttle launch. Ground tests were nominal and performance is expected to exceed that of FGS3 primarily due to the introduction of a special folding flat mirror for optical alignment. The new FGS will be commissioned during the orbital verification period and science assessment tests will ensue. If proven to have greater astrometric capability, the new FGS will be available for Trans mode in cycle 8 and Pos mode in late cycle 8 or 9. The calibration of FGS3 will be maintained for several more cycles.

Faint Object Spectrograph
Tony Keyes
The FOS has continued to perform well. Usage has continued at quite high levels in order to complete Cycle 6 programs prior to SM97. During the past three months FOS ACQ/PEAK acquisitions have again been affected by loss-of-lock events associated with FGS1. PRESTO is preferentially biasing away from FGS1 for FOS observations, however FGS1 occasionally must be used. Approximately 5% of visits since mid-October have been lost or seriously affected by FGS1-related loss-of-lock problems. Unfortunately, the Oct/Nov cycle 6 FOS/BL flat field and photometric monitor visits were lost completely due to loss-of-lock events. These calibrations will be repeated as soon as possible. As we enter the period of final on-orbit calibration measurement for the FOS, please refer to the FOS Web pages for updates relating to the status of instrument calibration.

Goddard High Resolution Spectrograph
D. Soderblom
The group within STScI that supports the GHRS is diminishing because of the needs of STIS. After February 28, 1997, the GHRS Group will consist of myself as Instrument Scientist and Lisa Sherbert as Data Analyst. Our work in 1997 is intended to provide the information that archival users of GHRS data will need in the future. Those plans will be discussed further in the next Newsletter. We are now redetermining the sensitivity and vignetting functions for grating G140L. A GO discovered a problem with the current sensitivity calibration files that lead to discrepancies in standard star spectra of ~5% over scales of ~50 å, with deviations of ~10% in some cases. New calibration files are being created, and all of this will be presented in greater detail on our Web page. We are also now working on: · A comprehensive examination of wavelength calibrations since Cycle 2. · Calibration of the wavelength offsets between the LSA and SSA. · Sensitivity and vignetting for grating G140M.

Faint Object Camera
M. Voit
As the February servicing mission approaches, the FOC's performance has been virtually trouble-free. The f/96 camera continues to gather high-resolution imaging data, and during the last six months we have returned the f/48 camera to regular service. Several programs have successfully used the f/48 spectrograph and its 0.06 x 12 arcsec slit to gather spectra with unprecedented spatial resolution.
For up-to-date information on HST's science instruments, check ST ScI's web pages. You may also wish to subscribe to one or more STANs (Space Telescope Analysis Newsletters). Subscriptions are done through a listserver, the instructions for which may be found on each instrument's web page.

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ST ScI Newsletter Science Institute · Newslette r Space Telescope · Instrument News

Instrument News
WFPC2
B. Whitmore
A new model for the WFPC2 polarization characteristics has been developed by John Biretta. Measuring the true polarization of a source with WFPC2 is challenging because the pickoff mirror introduces considerable instrumental polarization into the image. This and other instrumental effects are included in the new model. Comparisons between the model and limited on-orbit data suggest accuracies of 1 to 5 % can be attained, depending on the filter and observing configuration. A Web page has been created which describes this model, and it will be updated as our understanding of the calibration evolves. There are also two Web tools which can be used to calibrate polarization observations with the above model. A bug has been discovered in the pipeline calibration software for a small fraction of WFPC2 images. This bug was introduced in the December 1994 version (version 1.3.0.7) of the CALWP2 program, and affects the processing of all single-chip, non-PC images produced by the non-standard (engineering only) options READ=2, READ=3 or READ=4. As a consequence of the bug, the calibration proceeds as if the first group represents the PC (DETECTOR=1), regardless of the detector actually used. As a result, the pixel noise may be larger than in a correctly reduced image, and an offset zero point of several percent may exist. Also, images taken with partially rotated, quad, or Woods filters may have an incorrect vignetting function applied, which may result in significant non-uniformity of the background and of the throughput. A new version of the calibration routine CALWP2 is now being tested, and should become available in January. Meanwhile, if you have singlechip images in one of the WF cameras, and you suspect the incorrect calibration program was applied, please contact help@stsci.edu. PIs of affected programs have been notified.

HST Recent Release: Springtime Dust Storm Swirls at Martian North Pole
Two Hubble Space Telescope images of Mars, taken about a month apart on September 18 and October 15, 1996, reveal a state-sized dust storm churning near the edge of the Martian north polar cap. The polar storm is probably a consequence of large temperature differences between the polar ice and the dark regions to the south, which are heated by the springtime sun. The increased sunlight also causes the dry ice in the polar cap to sublime and shrink. Top (September 18, 1996) - The salmon colored notch in the white north polar cap is a 1,000 km long storm -- nearly the width of Texas. The bright dust can also be seen over the dark surface surrounding the cap, where it is caught up in the Martian jet stream and blown easterly. The white clouds at lower latitudes are mostly associated with major Martian volcanos such as Olympus Mons. This image was taken when Mars was more than 300 million km from Earth, and the planet was smaller in angular size than Jupiter's Great Red Spot! Bottom (October 15, 1996) - Though the storm has dissipated by October, a distinctive dust-colored comma-shaped feature can be seen curving across the ice cap. The shape is similar to cold fronts on Earth, which are associated with low pressure systems. Nothing quite like this feature has been seen previously either in ground-based or spacecraft observation. The snow line marking the edge of the cap receded northward by approximately 200 km, while the distance to the Red Planet narrowed to 275 million km. Credit: Phil James (University of Toledo), Steve Lee (University of Colorado) and NASA

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January 199 7

HST Data Archive

Archive Branch News
Megan Donahue

Upgrade Your StarView in February
StarView 5.0 will be available by mid-February, 1997. All users of the distributed version of StarView are asked to update their version at that time. The new version has screens for STIS and NICMOS. The format of the database and the screens must accommodate the STIS and NICMOS data structures, such as "products," "intermediate products," and "associations." We rarely require all users of StarView to upgrade, but these changes are significant, so that backwardcompatibility would have been very expensive. We will notify all active users of the archive of the upgrade

requirement, but only users of the distributed version are affected. The distributed version of StarView is faster than using it through archive.stsci.edu, and installation is only a matter of copying over the executables appropriate to your system. No recompilation is required! Access the new StarView from the WWW page http://
archive.stsci.edu/ dist_starview.html. While

New Phase II Data Distribution
In completing your Cycle 7 Phase II proposals, note that the new data distribution default is electronic retrieval. We will automatically notify you when your data are ready for retrieval from the Hubble Data Archive within 24 hours of its arrival, making it available days earlier than the typical tape delivery. If your internet link is slow, or the quantity of HST data is large, you can opt to receive an Exabyte or DAT tape. We have gone from only one data distribution medium (Exabyte) in Cycle 6 to three (electronic, Exabyte, or DAT) in Cycle 7, so do not neglect to select your preferred data distribution option in your Phase II proposal.

you're there, register as a distributed StarView user so we can keep you informed of any changes or new releases of distributed StarView.

HST Recent Release: Hubble Images Reveal Jupiter's Auroras
These images, taken by the Hubble Space Telescope, reveal changes in Jupiter's auroral emissions and how small auroral spots just outside the emission rings are linked to the planet's volcanic moon, Io. The images represent the most sensitive and sharply-detailed views ever taken of Jovian auroras. The images were taken by the telescope's Wide Field and Planetary Camera 2 between May 1994 and September 1995. Credits: John T. Clarke and Gilda E. Ballester (University of Michigan), John Trauger and Robin Evans (Jet Propulsion Laboratory), and NASA.

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ST ScI Newsletter Science Institute ·andewslette r Space Telescope · Public Outreach N Education

Public Outreach and Education

Public Outreach on the World Wide Web
P. Pengra
In response to this growing interest in the World Wide Web, the Office of Public Outreach is setting up a new Hubble Space Telescope site specially designed for the public. The site, called the Hubble Space/Time Explorer, features the telescope and science images, but is stylistically distinct from the Space Telescope Electronic Information Service (STEIS) familiar to most astronomers. (See the other Web article in this issue for news on these other STScI Web pages.) At the very top level, we've put links for kids, teachers, and reporters, and we've provided a quick way to get to the latest Hubble pictures and news. The glowing "network" design that begins at the top with the constellation of stars framing the telescope (shown on the right) is carried forward into other page designs, such as the ones for kids, the picture gallery, and Amazing Space. Amazing Space is an on-line collection of educational resources for teachers and students. It includes student activities (described in the last edition of this newsletter) featuring the Hubble Deep Field, Solar System Trading Cards, the Second Servicing Mission, and Stars. The new site will soon include a search capability so that site visitors can readily find what they're looking for. And to make sure that frequent visits don't slow down the primary work of the Institute, the site will be supported by a dedicated server. Check it out. The URL is:
http://www.stsci.edu/pubinfo

The Internet is everywhere. And "surfing" has become a national pastime.

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January 199 7

Institute News

Saving Lives with IRAF: Innovative Uses of Astronomical Software
R. Hansich and R. White
Over the past year and a half, we have been collaborating with JHU computer scientist Steven Salzberg and Georgetown University radiologist Matthew Freedman to explore the application of astronomical image processing methods and automated detection and classification algorithms to the analysis of digitized mammograms. An early diagnostic for the likely development of breast cancer is the appearance in a mammogram of faint, point-like objects called microcalcifications. These objects can be difficult to see, however, especially since virtually all analysis of mammograms is by visual inspection of an x-ray film. When microcalcifications occur superimposed on regions of structural complexity, even experienced radiologists can overlook them. Moreover, clinical experience has shown that as smaller and smaller microcalcifications are detected (and they are even more difficult to detect by visual inspection), they continue to serve as a good diagnostic of the eventual development of cancer. We got involved with this work owing to the intervention of Ben Snavely, program manager for advanced technologies and instrumentation in the Astronomy Division of the National Science Foundation. Ben's previous experience in developing medical imaging equipment at Kodak, combined with his work at NSF, led him to believe that there may be some benefit from applying image processing methods developed in astronomy to medical image analysis problems. He made the introductions between those of us at STScI, JHU, and Georgetown, and supported our initial work with an exploratory research grant. Of the wide variety of medical image analysis problems, our interest was drawn to the detection of microcalcifications in digitized mammograms owing to the similarity with detection of faint cosmic ray hits in CCD images. There are some significant differences, however. First, in mammography one does not have the advantage of using separate, independent exposures to isolate spurious events like cosmic rays. The microcalcifications are true objects, and would appear the same in multiple exposures, at least to the extent that two exposures can be made under identical conditions. Standard mammography involves two separate images of the breast, taken from two viewpoints. In principle one can correlate features in these two perspectives, but the geometry of the two views is non-trivial to determine empirically. Thus, the problem of microcalcification detection relies primarily on developing a suitable high-pass filter. The high-pass filter must not be biased against the detection of microcalcifications in regions of the image with low image intensity. The filtering approach that we have developed involves three steps. The first is to compute a conventional unsharp mask by median-windowsmoothing the image and subtracting the smoothed image from the original. The second step is to fit a normalization function to the distribution of locally-computed variances versus the image median intensities. These variances are a measure of the "structural noise" in the image, which increases linearly with intensity above some low-level noise background and up to some saturation value. The unsharp-masked image is then divided by the normalization function to create an image in which the pixel intensities are an unbiased measure of that pixel's deviation from the local median. Some sample variance normalization functions are shown in Figure 1. This filtered image is then processed by the DAOPHOT "find" routine to identify the strongest point-like objects. Because the cancer diagnostic involves the detection of clusters of microcalcifications rather than isolated objects, we compute distance measurements for each object to its nearest neighbor objects. The object list with distance measurements is then classified by Steven Salzberg's decision-tree algorithm to identify likely microcalcification clusters using a training set of microcalcification clusters identified by experienced radiologists. One of our initial results is shown in Figure 2. At left is the original mammogram, and at right is our filtered version of the image in which the confusing background structures have been removed. In both images the microcalcification clusters identified by radiologists have been overlaid. We detect microcalcification clusters where the radiologists do, and also see some clusters that the radiologists may have missed. The next step in this project is to expand the suite of test data sets and compute the receiver operating characteristic (ROC) curves for our filtering and detection methods. Ideally one will detect true microcalcification clusters only, missing none and having a minimal number of false positives. To date, most automated microcalcification detection algorithms have failed to find 5 to 10% of the true clusters, and they tend to include a
continued page 26

Editor's Note: Dr. Hanisch is the 1996 recipient of the AURA Achievement Award for functional work at STScI. I asked him to provide this description of some of the work that led to that award.

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ST ScI Newsletter Science Institute Space Telescope · Institute News

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Newslette r

New Design for the STScI Web Site
Dick Shaw and Harry Payne
Those of you who visit the STScI Web site http://www.stsci.edu/ will notice a set of new, high-level pages. These pages were released at the beginning of 1997 after extensive discussion and experimentation by members of the Institute's STEIS Steering Committee. These pages give World-Wide Web has become one of the primary means through which STScI reaches its user community. The community we serve through the Web has also changed and expanded dramatically. The STScI Web site is now one of the most popular on the Internet and has come to serve the needs and interests of a very broad audience, including students, educators, the broadcast and print media, and the general public. The Web site usage statistics show that the vast majority (typically more than 90%) of the roughly 200,000 daily requests come from this broader audience, rather than from members of the professional astronomy community that were the focus of the previousgeneration Web pages. Interestingly, the average daily volume of information retrieved from the STScI Web site rivals the volume of data retrieved from the Hubble Data Archive, and sometimes exceeds it by a factor of up to five. Serving so many resources to such a large and diverse audience puts ease of navigation at a premium, and necessitates a clearer statement of identity, which is reflected in the new Web design. The goals were to create a clean, well-organized site, to better accommodate the needs and interests of the public, to add a number of navigation aids, to be friendly towards non-graphical browsers and users reaching us over low-speed connections, and to put important and interesting information of a timely nature into prominent locations. The new Web pages, in their sum, now contain links to all the previous (and many new!) Web resources. Though these links are arranged somewhat differently than before, the intention is that information and other resources are now easier to locate.

New Resources
Members of the scientific community, especially users of HST, will find most links of interest by following either the link to "Science Resources" or to "Observing with HST" from the new home page. The latter link brings together the resources that observers need in all phases of their programs, from the Call for Proposals for each cycle, proposal preparation resources, details of the science instruments, to the data reduction and analysis pages. This page (as with many of the higher level pages) will feature important announcements, deadlines, and news items near the top, just under the banner. Users of HST may wish to establish a "bookmark" in their browser to this page. Their are also new navigation aids to find resources, including a search engine, a "Topics" page and an index, which are all accessible from the "banner" at the top of all the high-level pages. These navigation aids provide different, but complementary views of Institute Web resources. The "Topics" page presents a large number of links on one page, in the form of a table where the column headings correspond to the major links offered on the home page. This flatter view of the STScI Web space should make it easier for you access a resource when you know where it is, with traversing a hierarchy of pages to get to it. The "Index" page is arranged like a book index, in that the links are arranged alphabetically by topic, and many of the links are present more than once. This page is more appropriate when you know what category of information you want, but do not necessarily know what path to take to find it. Neither the "Topics" nor the "Index" page lists all possible STScI Web resources, but focus instead on higher-level pages that provide links to the primary resources (e.g., the manuals, the software distributions, etc.). The STScI "search" facility will enable you to find any
continued page 27

a new look to the Institute's Web presence, and present what we hope is a Web site that is informative, enriching, and in keeping with the best interests of the STScI mission. The previous design served us well for two years, which is an eternity in the Web provider community. During that time, the state of the art in Web site design and navigation technologies has advanced considerably. The STScI Web site has grown substantially during that period as well: the number of HTML pages, manuals, images, etc. offered through STScI grew from a few hundred in the early 1990s to over 30,000 internal and external resources at the end of 1996. There is every reason to believe this growth will continue. Thus, in just a few years the

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January 199 7

The 1997 STScI May Symposium: The Hubble Deep Field
M. Livio, STScI
Our May Symposium this year is on the Hubble Deep Field. The intent is to cover all the types of objects in the HDF, namely, galaxies, stars, and substellar objects. The confirmed invited speakers are listed to the right. The symposium will take place at the Institute, on May 6-9, 1997. The deadline for registration is April 1, 1997, and the registration fee is $150. Those wishing to attend should contact the following as soon as possible: Cheryl Schmidt, Symposium Coordinator Space Telescope Science Institute 3700 San Martin Drive Baltimore, MD 21218, USA. Tel. (410)338-4404 Fax (410)338-4767 e-mail: schmidt@stsci.edu For further information see:
http://www.stsci.edu/ftp/ meetings/may97/ announcement.html

Speaker
Allan Sandage Andy Fruchter Richard Ellis Kenneth Kellermann Garth Illingworth Lennox Cowie Judith Cohen Michael Rowan-Robinson Mike Fall Simon Lilly Charles Steidel Simon White Mauro Giavalisco Rogier Windhorst Kenneth Lanzetta John Bahcall Matthias Steinmetz Steven Kawaler Harry Ferguson Joseph Silk Piero Madau George Efstathiou Mark Dickinson Guinevere Kauffmann Mike Brown Roger Blandford Megan Donahue James Peebles

Tentative Topic of talk
A Historical Overview Technical Aspects of the HDF An Introduction and Motivation Radio Observations in the HDF Kinematics of HDF (and other) distant galaxies Review of results from redshift surveys Review of angular and redshift clustering of HDF and other deep surveys ISO observations of the HDF Cosmic Chemical Evolution: HDF & QSO abs. lines HDF and its relation to previous redshift surveys Spectroscopy of z>2 galaxies Galaxy luminosities and number densities at high redshift from hierarchical models Galaxy ages and morphologies of z>2 galaxies Results from parallel surveys and other deep HST surveys Review of photometric redshifts Stars in the HDF Model predictions for clustering and morphologies at HDF depths White Dwarfs in the HDF Selection effects and robust measures of galaxy evolution in the HDF Disk galaxy and dwarf galaxy evolution Global measures of star-formation history from the HDF Are hierarchical models vindicated or vitiated by deep HST observations? Evolution of the luminosity function at high z Semi-Analytic models of galaxy formation Search for Sub-Stellar Objects in the HDF Gravitational Lensing Educational uses of the HDF Conference Summary

Notice: STScI recently issued a preprint containing poster papers from last May's symposium titled "The Extragalactic Distance Scale." Unfortunately, for technical reasons, two posters were not included. Those have now been put into a small separate edition. Libraries interested in obtaining the new preprint should contact the STScI library. The e-mail address is library@stsci.edu.

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ST ScI Newsletter Science Institute Space Telescope · Institute News

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Newslette r

Tenure for Abhijit Saha
Abhijit Saha was recently granted tenure as Associate Astronomer at STScI. He came to STScI as an Assistant Scientist in 1988, joining a newlyformed User Support Branch. In 1990, Abhijit became an Assistant Astronomer, in recognition of his research accomplishments. In 1992, Abhijit took over as Chief of USB and was promoted to Associate Astronomer. He now splits his functional time between SMO, the Servicing Mission Office, and OPO, the Office of Public Outreach. He is coordinating the Early Release Observations that will be done with STIS and NICMOS next year. He is also Deputy Editor of the PASP. Born in Calcutta India, he comes from a family with many scientists and academics, including his parents, grandfather, aunts, and uncles (but the Saha of equation fame is not among them). He has a brother in theoretical astrophysics. Doubtless this background influenced Abhijit to study physics at St. Stephen's College at the University of Delhi. This was also his route to pursue astrophysics, an interest that was seeded early and made concrete after reading Patrick Moore's "The Amateur Astronomer" at age 14. He obtained both bachelor 's and master 's degrees in Delhi, during which studied General Relativity and was introduced to formal astronomy. He attended two summer schools at the Indian Institute of Astronomy, where contact with M. K. V. Bappu and others reinforced the choice of astronomy as a career. He then came to Caltech to work on his Ph.D. He finished in 1983, after completing work on RR Lyrae stars as probes of the Galactic halo, supervised by J. B. Oke. Abhijit has continued to work on RR Lyrae stars as probes of various astronomical problems, first as a postdoc at Kitt Peak, then as a Carnegie Fellow at the Observatories of the Carnegie Institution of Washington, in Pasadena. He is currently working on the cosmological distance scale with HST data as part of two different investigation teams and involved in a major effort to establish Cepheid-based distances to all galaxies (where possible) within approximately 3 Mpc, using ground-based facilities. Abhijit reads on philosophy and comparative religion when he has the chance, and is fond of music and theatre, especially the absurd and avant garde. He is a keen enthusiast of cricket, which he misses, and considers a sacrifice to his cultural migration.

IRAF

from page 23

large number of false positive detections. Our collaborators at Georgetown University have begun assembling a much more extensive mammography database, which includes complete follow up studies to allow more accurate measurements of the diagnostic value of microcalcification detection. We have submitted a proposal to the Army Breast Cancer Research Program to follow up on what has been, thus far, a demonstration of the potential value of applying our knowledge of astronomical image processing methods to the downto-earth problem of diagnosing breast cancer.

ST-ECF Newsletter
The Space Telescope -- European Coordinating Facility publishes a quarterly newsletter which, although aimed principally at European Space Telescope users, contains articles of general interest to the HST community. If you wish to be included in the mailing list, please contact the editor and state your affiliation and specific involvement in the Space Telescope Project.

Robert Fosbury (Editor)
Space Telescope -- European Coordinating Facility

Karl Schwarzschild Str. 2
D-85748 Garching bei MÝnchen Federal Republic of Germany

E-Mail: rfosbury@eso.org

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January 199 7

New Web Design

from page 24

Calendar
Cycle 7
Phase II proposals due Start of science observations Check the Cycle 7 Phase II Proposal Instructions 1 July 1997
(approximate)

Cycle 8 (tentative):
Call for Proposals issued Phase I proposals due October 1997
(tentative)

February 1998
(tentative)

Second HST Servicing Mission Launch 13 Feb 1997, 07:59 UT (tentative) Meetings and Symposia
STScI May Workshop The Hubble Deep Field Space Telescope Users Committee 6 to 9 May 1997 12 to 13 May 1997

New on the WEB
Some items on STScI's web pages you may find of interest:

1 2 3

First and foremost, check out the all-new STScI Web design (see articles on pages 22 and 24). Results from the Medium Deep Sur vey can be found at: http://archive.stsci.edu/mds/index.html For information on the 1997 Summer Student Program at STScI, see the previous Newsletter, and on the Web look under "About STScI" then "STScI and the Astronomical Community"

Institute Web resource; the advantages of this utility over generic Web search engines are that the search is limited to the "stsci.edu" domain, and our master search index is updated more frequently. There is one other navigation aid of note. The higher-level pages contain two textual navigation bars near the bottom of each page: one allows direct access to the home page or to the navigation aids described above, and the other provides access to "sibling" pages without first following a link to a higher-level, "parent" page. Note also that you can always reach the STScI home page by clicking on the STScI logo in the banner at the top of an inside page. We expect that the STScI Web pages will continue to evolve (indeed some aspects, such as the home page graphic and the news items, were designed to be updated several times per year), though always in response to the needs and interests of our Web communities. The new Web pages attempt to balance the needs of our largest audience -- students, educators, amateur astronomers, reporters, and interested members of the general public -- with those of the audience our institution was created to serve: the international community of professional astronomers. They are all important to us, and we are grateful for their continuing interest in STScI and the Hubble Space Telescope. STScI invites you to offer your thoughts to us about these new pages, or about any aspect of the STScI Web site. Please direct your comments to the webmaster@stsci.edu, or click on the "user comments" link near the bottom of the home page.

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Contents
Astronomy with HST Climbing the Starburst Distance Ladder .............................. 1 Director 's Perspective ........................................................... 2 HST Programs and Observations Duration of Cycle 7 .............................................................. Panel and TAC Members for Cycle 7 ................................... Approved Observing Programs for Cycle 7 ......................... GO and AR Statistics of PI by country ................................. Proposal Statistics by Panel .................................................. Preparatory Support Available For Funded Programs .......... Electronic Submission of Performance Reports ...................

How to contact us:
First, we recommend trying our Web site: http://www.stsci.edu You will find there further information on many of the topics mentioned in this issue. Second, if you need assistance on any matter send e-mail to help@stsci.edu or call 800-544-8125. International callers may use 1-410-338-1082. Third, the following address is for the HST Data Archive:
archive@stsci.edu

5 5 7 13 14 15 15

Second Servicing Mission HST's Second Servicing Mission--Overview ..................... 16 Space Telescope Imaging Spectrograph (STIS) Update ....... 17 NICMOS ............................................................................... 18 Instrument News ..................................................................... 19 HST Data Archive Archive Branch News ........................................................... 21
Public Outreach and Education

Fourth, if you are a current HST user you may wish to address questions to your Program Coordinator or Contact Scientist; their names are given in the letter of notification you received from the Director, or they may be found on the Presto Web page (http://presto.stsci.edu/public/propinfo.html). Finally, you may wish to communicate with members of the Space Telescope Users Committee (STUC). They are: Fred Walter (chair), SUNY Stony Brook,
fwalter@sbast1.ess.sunysb.edu

Public Outreach on the World Wide Web ............................. 22

Institute News Saving Lives with IRAF: Innovative Uses of Astronomical Software .......................... 23
New Design for the STScI Web Site .................................... 24 The 1997 STScI May Symposium: The Hubble Deep Field ........................................................ 25 Tenure for Abhijit Saha ........................................................ Calendar ................................................................................ New on the WEB .................................................................. How to contact us: ................................................................ 26 27 27 28

John Bally, U. Colorado John Clarke, U. Michigan Alex Filippenko, U.C. Berkeley Bob Fosbury, ESO Marijn Franx, Kapteyn Astron. Inst. Laura Kay, Barnard College Regina Schulte-Ladbeck, U. Pittsburgh Ted Snow, U. Colorado Rodger Thompson, U. Arizona John Trauger, JPL Will van Breugel, Lawrence Livermore The Space Telescope Science Institute Newsletter is edited by David Soderblom, to whom correspondence may be sent (soderblom@stsci.edu). To record a change of address, please contact Ms. Nancy Fulton (fulton@stsci.edu). Design and layout: John Godfrey

AC SP E TELESCOPE SCIENCE INSTITUTE

NON PROFIT U.S. POSTAGE P A I D PERMIT NO. 8928 BALTIMORE MD

3700 San Martin Drive, Baltimore Maryland 21218

STScI N-97-01