February 1996 • Volume 13, number 1

SPACE TELESCOPE SCIENCE INSTITUTE Highlights of this issue: • New Key Projects — page 1 • Hubble Deep Field — page 3 • Cycle 6 HST Programs Newsletter — pages 12-22

New HST Key Projects Telescope Allocation Committees to observing time (100-150 orbits/year) for Cycles 7-9 limit the amount of observing time over a 3-year period. Our plan is to by Bob Williams allocated per proposal so as to collect these ideas and discuss them accomodate as many programs as with a newly convened Advisory We have just finished a very possible. Some of the most important Committee during the month of March successful year of scientific accom- scientific objectives, those for which 1996, and to use this Committee’s plishments with the HST, as evidenced the HST itself was built, require recommendations as topics for new by the number and impact of HST- extensive and uniform studies to reach Key Projects which will be solicited in related articles in the astronomical definitive conclusions. the Call for Proposals for Cycle 7, to journals. The Institute is currently Throughout 1983-1985 the STAC be issued in the late Spring of 1996. working with the HST Project at surveyed the astronomical opportuni- The success of this activity will Goddard Space Flight Center, the STIS ties for research with HST, with the depend largely on the scientific input and NICMOS Principal Investigators specific task of identifying those we receive from the astronomical and their teams to prepare for the programs which were of outstanding community, and therefore we strongly Second Servicing Mission, scheduled scientific importance, which could encourage you to send us your views. for the early months of 1997. only be carried out by HST, and which To facilitate your response to this The selection process for the required a large amount of observing request for suggestions for those topics observing programs to be executed in time. Another important consideration to which Key Projects should be Cycle 6 has now been completed, and was the creation of valuable and devoted, we have established a page on we have already begun our prepara- uniform databases for broad archival the World Wide Web : http:// tions for the Call for Proposals for studies. The STAC obtained commu- www.stsci.edu/ftp/proposer/cycle7key/ Cycle 7, which begins in July 1997. nity input and made their recommen- keyprojects.html. We look forward to This early start is necessary so that we dations to the Institute to implement receiving your thoughts and ideas on may inform the community of the three Key Projects for which “propos- this matter. unique new capabilities that STIS and als to carry-out these projects would be NICMOS will provide. particularly welcome”. These projects As part of these preparations, we were the Determination of the intend to initiate a new round of Key Extragalactic Distance Scale, the Hourglass Nebula Projects to take full advantage of the Quasar Absorption Lines Survey, and The new scientific opportunities provided the HST Medium Deep Survey. planetary nebula by STIS and NICMOS, as well as Proposals for each of these three topics those still available through the use of MyCn 18 were reviewed and selected by the as seen the instruments that will remain on Cycle 1 TAC, and their progress and with board after the Second Servicing allocations have been reviewed in each HST’s Mission (WFPC 2, FOC, FGS). Key of the following cycles. The Quasar WFPC2 camera. Projects were recommended to the Absorption Line Survey was com- Institute by the 1983 Space Telescope pleted in Cycle 3, and the remaining Advisory Committee (STAC) as a way two Key Projects will be formally to ensure that large-scale projects completed at the end of Cycle 6. directed to answering fundamental The purpose of this article is to questions in astronomy would be solicit your ideas for new and carried-out with HST. The concern was fundamental astronomical problems that the inevitably high oversubscrip- that should be tackled with HST and tion rate on HST would lead the which would require large amounts of SpaceST ScI NewsletterTelescope Science • Director’s Institute Perspective • Newsletter

Director’s Perspective have been granted time on HST. chaired by Alan Dressler. NASA by Bob Williams & Mike Hauser Because of the decrease in GTO time headquarters has asked Goddard Space and increasing efficiency of telescope Flight Center (GSFC) and the Institute At the moment, the HST project and operations, GO proposers in Cycle 6 to lead a study of large telescope the Institute are passing through a have more available time than in any technologies for space. The intent is to period of stability and productivity previous cycle. The development of the identify ways in which a 4m class with the telescope and instruments, a two new instruments, STIS and telescope, IR optimized and passively period in which we have not had any NICMOS, to be installed in HST in the cooled, might be launched into orbit at notable incidents or safe modes in 1997 Servicing Mission is proceeding, a project cost well below that of HST. almost a year. The data coming out of as reported elsewhere in this issue. Dr. John Campbell, the HST Project the telescope are proving to be of Commensurate with the new capabili- Manager, is leading the study, and he significance to a wide variety of ties provided by these instruments, the will be assisted by John Mather of problems in astronomy, and the Institute plans to initiate a process by GSFC and Peter Stockman of the steadily increasing data in the HST which new Key Projects will be Institute. Technical experts from archive are clearly being valued and defined and selected beginning in GSFC, Marshall Space Flight Center, used by the community as an important Cycle 7. Information on this process Jet Propulsion Laboratory, and other resource. It is also pleasing to see the can be found elsewhere in this issue organizations will participate in this very positive view of the HST being and also on the Institute home page on study, and a panel of senior scientists presented by the press. We are now the WWW. The community should be from the astronomical community will well into Cycle 5 observations, and aware of an important new initiative in be convened to provide scientific have allocated most of the GO data which the Institute will help shape oversight. The study should be reduction funds for these programs. follow-up missions to HST. In completed within two years. The The Cycle 6 TAC recently met and anticipation of the recommendations of results will provide the basis for made its recommendations for the ‘HST and Beyond’ Committee development of the next generation telescope time, in which roughly 400 large optical/IR telescope in orbit. GO of the 1025 proposals submitted

Deep Images

On the left we can see the image of the Hubble Deep Field (HDF) from one of the Wide Field chips. For comparison on the right is a 4000 sec V image of the cluster of galaxies CL 0939+4713 in the V band. In this black and white printed image of the HDF you can’t appreciate its incredible detail. We invite you to see the full color version or to retrieve the actual files from http://www.stsci.edu/ftp/observer/hdf/hdf.html

2 February 1996

8 adjacent “flanking fields” shortly Fig. 1. The drizzling software is still 6 NGC 891 The Hubble 4 Radio Thin 2 Disk

0 2 Halo NW 0

Flux Density [MJy/beam] Halo 2 SE

0

125 4000 FIR III

III V x 100 I x III before and after the main observations. being modified and improved, but will 3000 x III x III x x V

75 x V x I 2 V II 000 x x I V Deep Field project x x x 50 V I I x

Flux Density [MJy/sr] V x 1000 x III I O3 O4 O 5 O6 O7 x O8 O9 I I 25 Spectral Type B0 B1

0 4 2 0 -2 -4 H.C. Ferguson The data were released January 15, make its way into STSDAS over the Relative Distance Along Major Axis [ '] While many were home feasting, after three weeks of intensive effort to next several months. HST spent the holidays staring at a process, register, and co-add the As anticipated, study of the HDF single non-descript patch of sky, now images. The processed data are images and followup observations are known as the Hubble Deep Field available via ftp from stdatu.stsci.edu now proceeding at a vigorous pace. (HDF). The project arose out of the in the directory /pub/hdf, and details of The images are being used by desire to use a large portion of the observations and data reduction can astronomers at STScI and elsewhere to be found on the observer page of the study the stellar luminosity function in director’s discretionary time effectively Science News to further studies of galaxy evolution. STScI web site (http://www.stsci.edu/). the galactic halo, to measure the While several deep images at high Version 1 of the data reduction used optical extragalactic background, to galactic latitude had been obtained about 80% of the available data. By the search for weak lensing due to large scale structure, to quantify the morphology of faint blue galaxies and of high-redshift protogalaxies, and to study the clustering of galaxies at the faintest observable levels. Redshifts of several galaxies have already been obtained at the Keck observatory. Infrared Imaging and further spectros- copy will be obtained by various groups this spring from Keck, KPNO, and Calar Alto. We invite all groups and individuals participating in HDF research to make their plans and results known through “HDF Clearinghouse” on the World-Wide Web. This service is simply a set of links to web locations at other institutions, where HDF research can be described. To partici- pate, simply create a web page and Figure 1. Example of a simple shift and combine (left) and the result of the send its address to [email protected]. "drizzling" technique (right) to obtain the final image. Observers interested in making their already with the telescope, it was clear the time this newsletter appears, data available through the HST archive that significantly more information on version 2 of the reduced data should be are also encouraged to contact us. the faintest galaxies could be obtained available. This version will use nearly by (1) targeting a field in the continu- all of the available data, combined with ous viewing zone and (2) observing more nearly optimal weighting. Probing Globular through a variety of filters. It was also One of the innovations developed Clusters’ Cores with clear that such images would have a for the HDF was the use of “drizzling” wide variety of uses, and that immedi- to combine frames taken at different the FOC ate release of the data to the astronomi- positions. For each HDF filter, by Guido De Marchi (ESO) cal community would stimulate a great observations were made at nine The FOC has had a strong impact in deal of research. Following the different pointing positions in an the field of dynamics and stellar recommendation of a special Institute irregular pattern covering a space of evolution in dense cores of galactic + Advisory committee that met in March - 1.3 arcsec from the central position. globular clusters (GCs). Thanks to its 1995, a working group was constituted The drizzling technique was developed high spatial resolution, less than 0.05" within STScI, with help from members by Andy Fruchter and Richard Hook to FWHM) and UV sensitivity (115— of the ST-ECF, to plan and carry out correct for geometric distortion during 300nm), it can effectively probe the the observations. The details of the image combination phase, while core population of even the densest planning issues were highlighted in simultaneously improving the clusters in search of dynamically articles in the previous issues of the resolution and doing as little injustice induced abnormalities. STScI and ST-ECF Newsletters. as possible to the noise. A comparison The presence of a central cusp in the The bulk of the observations were of images combined with integer pixel surface brightness or density radial carried out from 18-29 December, shifts and images combined and profile of a GC has usually been 1995, with the addition of 10 orbits on subsampled using drizzling is shown in interpreted as the signature of a 3 SpaceST ScI NewsletterTelescope Science • Science Institute News • Newsletter

“collapsed” state of the core, i.e. of a projected density distribution of turn- core’s color magnitude diagram. With very advanced evolutionary state. With off mass stars (0.8 Mo• , those contribut- the FOC for the first time, these its unprecedented resolving power the ing the most to the total light) is fitted strange populations can be studied in FOC makes it possible to measure the by several different models going from detail right where they are produced. distributions of stars in GC cores with a power-law function all the way to the The first example of this application a much greater accuracy than could be center, to a King-type model with a was the discovery made soon after done from the ground. We should then small core radius (~ 1.8"). Similarly, launch by the FOC of a centrally expect to be able to understand the 47 Tuc has seen its core radius drop by concentrated population of BSS in 47 cluster dynamical history much better. more than a factor 2 to ~ 10" as a result Tuc (Paresce et al. 1991), followed by Yet, FOC’s higher resolution has of high resolution observations. similar findings in all the clusters revealed that the most concentrated Intuitively, one would think that obeserved thereafter (M15, NGC6254, cores are indeed so small that there are going to fainter magnitudes would NGC6397, NGC6752, M3, Ω Cen). increase the sample by adding stars These results consistently suggest a less massive than those above the turn- BSS source rate which is actually off, and therefore improve in a enhanced in crowded environments statistical sense the determination of due, most likely, to mergers of main the dynamical state. Because of their sequence stars as a consequence of lower masses, however, these fainter direct collisions involving single and objects have a radial distribution which binary stars. The latter are particularly differs from that of the brighter stars, important in the dynamical evolution and their number decreases rather than of a cluster, in that their presence may increasing at fainter magnitudes, as a retard or prevent collapse from result of mass segregation (see below). occurring at all, but they can also These difficulties although discourag- power the re-expansion of the core ing, had long been predicted by after collapse by energy transfer to theoretical studies. Collapse may also other stars. involve only certain types of heavier The sensitivity of the FOC to the stars that decouple from the system UV light makes this instrument leaving the profile of other objects particularly efficient at revealing unchanged. Understanding the interacting binary systems in GC cores. dynamical state of the cluster on the Besides the two dozen BSS, which are basis of these profiles therefore supposed to have a binary origin, two Figure 1. Near UV Objective Prism image of a region becomes tremendously difficult, if at cataclysmic variables have been found of ~ 11" × 11" in the core of 47 Tuc obtained with the all possible. in the core of 47 Tuc. The first, V1 FOC before the servicing mission. The prism generates, With the FOC, one can look for (Paresce, De Marchi & Ferraro 1992), at the position of each star, a dispersion figure (the oblique features seen on the frame), whose length stellar populations whose characteris- is likely the UV counterpart to the depends on the spectral energy distribution of the tics deviate from those expected from a variable X-ray source X0021.8-7221. object: the bluer the longer. The NUV prism is mostly normal evolutionary sequence of If it is, then it is almost certainly an efficient in the range 190-400 nm. Longward of 400 nm single, coeval, and isolated stars. The asynchronously rotating DQ Her type the low dispersion causes the light from the objects to specifics of the collapse process binary with a period of around 6 hours. concentrate in a bright spot (red-end). Short, stubby images are the spectra of red objects in the core immediately suggest that such The second one, V2 (Paresce & De (particularly red giants with temperature ~4,000K. populations would preferentially Marchi 1994), is the first dwarf nova The prominent feature crossing the frame from side to inhabit the central core regions where detected at outburst right in the core of side is the spectrum of the dwarf nova V2 at outburst, they are formed in greatest abundance. a GC. The astounding low-resolution the bluest object in the field. The spectra obtained with The very high densities reached even spectrum of this object obtained with the NUV prism have medium resolution (~0.5nm at 250nm), and are particularly useful at estimating the for a short time in the core coupled to the FOC’s near-UV Objective Prism UV continuum of blue objects. the relatively low stellar velocities (Figure 1) clearly shows the signature automatically ensure a copious of an eruption typical of dwarf novae production of binaries by 3-body (Fλ α λ-2.3). dynamical or 2-body tidal capture and Four blue variable objects have been not enough stars to characterize their their evolutionary products such as found in the core of NGC6397 (De structure. The concept of density blue straggler stars (BSS), stripped red Marchi & Paresce 1994b), most likely becomes then meaningless, as the giant cores, contact binaries, etc. These the UV counterpart to multiple X-ray distribution of masses can not be populations would tend to cluster sources discovered with ROSAT (Cool approximated by a fluid. The cluster physically in the core and parametri- et al. 1993), with fluxes typical of M15 is one of these elusive objects: its cally in the blue-UV region of the cataclysmic variables. Their broad- 4 February 1996 band UV spectra are compatible with with respect to the outer regions, as is temperatures in the range 15 - evident in Figure 3. 20,000K, as expected for accretion The drop observed in the core LF of disks around interacting binaries. these clusters further confirms their Finally, the FOC has shown that the advanced evolutionary state. In the core of M15 harbors a tightly concen- near future, with STIS, radial velocity trated group of about 15 very blue measurements will become possible objects (bluer than the BSS), which also for main sequence stars in dense could be the result of catastrophic cores. Coupled to proper motion encounters between red giants and determinations, they will allow a compact stars, probably in binaries, firmer discrimination between pre- and that would strip the extended gaseous post-collapse phases. Studying the envelope of the former revealing a hot, properties of the local stellar popula- blue core (De Marchi & Paresce tion in GCs, however, will remain one 1994a). Similar but less numerous of the most powerful ways of investi- objects are also seen at the center of gating the dynamical history of these NGC6752 (Shara et al. 1995). fascinating objects. With this cornucopia of exotic objects in their cores, it is no longer References necessary to rely on the ambiguous Cool, A., et al. 1993, ApJ, 410, L103 surface brightness profiles to define De Marchi, G., & Paresce, F. 1994a, Figure 2. Deep UV color-magnitude diagram of the population in the core of 47 Tuc. these clusters’ dynamical state: a post- ApJ, 422, 597 De Marchi, G., & Paresce, F. 1994b, The main sequence becomes sparser towards collapse phase is legitimate for all of fainter magnitude, as a result of mass A&A, 281, L13 them, wherein the core stellar segregation. The triangle marks the quiescent population is strongly and directly De Marchi, G., & Paresce, F. 1996, state of V2. ApJ, in the press modified by dynamical effects. King, I.R., Sosin, C., & Cool, A. 1995, But GC cores undergo also much ApJ, 452, L33 quieter and smoother population Paresce, F., et al. 1991, Nature, changes which are, nevertheless, 352, 297 fundamental in their dynamical life. Paresce, F., & De Marchi, G. 1994, Because of the relaxation process, ApJ, 427, L33 these systems evolve towards energy Paresce, F., De Marchi, G., equipartition through repeated stellar & Ferraro, F. 1992, Nature, 360, 46 encounters, in which more massive Paresce, F., De Marchi, G., & stars transfer kinetic energy to lighter Jedrzejewski, R. 1995, ApJ, 442, L57 objects (which then move outward Shara, M., Drissen, L., Bergeron, L., onto larger orbits) and sink into the & Paresce, F. 1995, ApJ, 441, 617 potential well at the cluster center. The net effect of this differential migration, called mass segregation, had long been predicted theoretically, yet had so far proved tremendously difficult to confirm observationally, particularly in dense cores. The first deep investiga- Figure 3. Solid line: LF of the core tions with the COSTAR-corrected population of M15 in the F346M band. Dashed line: LF of a region located FOC of the inner few arcseconds of 47 ~5' away from the center obtained with Tuc (Paresce, De Marchi & the WFPC2 in the F814W band, converted Jedrzejewski 1995, see Figure 2), to F346M and normalized to the other . NGC6397 (King, Sosin & Cool 1995), at the turn-off. At m346~22 (~ 0.65 Mo) and M15 (De Marchi & Paresce 1996) the number densities differ by a factor 10, in fair agreement with theoretical have revealed a dramatic drop in the expectations. luminosity function (LF) of main sequence stars that begins right from the turn-off and continues all the way down to the detection limit. Low mass stars are strongly depleted in the core 5 SpaceST ScI NewsletterTelescope Science • Science Institute News • Newsletter

Paris Meeting fields and to determine their properties Alan Dressler. The capabilities and by Mario Livio has facilitated amazing progress in the expected performance of the future study of globular clusters and in the HST instruments were also presented. The second conference on science understanding of stellar populations. Finally, an education session was using HST was held in Paris, Decem- In extragalactic astronomy, the HST held, in which, among other things, ber 4-8 1995. In spite of the difficulties resolution was again instrumental in innovative ways of using HST data introduced by the general transporta- revealing the properties of a variety of through the Internet were discussed. A tion strike in Paris, the meeting was Active Galactic Nuclei, the characteris- hands-on activity on object classifica- attended by more than 250 partici- tics of their host galaxies and the tion was demonstrated, utilizing many pants. detailed structure of the jets emanating of the concepts which the HST data The most striking thing about the from them. HST provided convincing can help elucidate. data presented at the meeting was the evidence for the presence of extent to which HST has impacted supermassive black holes in M87 and ALL of the areas of current astronomi- NGC 4261. Observations of the cal research. Observations of the solar H Key Project intergalactic medium, of QSO 0 system provided both spectacular To diseminate the results to absorption line systems and of galaxies images and abundance determinations a wider audience the H Key and clusters at redshifts ranging from 0 in objects ranging from Venus to Pluto. project has set up a WWW page zero to 3.4 begin to place very Observations of star-formation regions at: http://www.ipac.caltech.edu/ meaningful constraints on cosmologi- and of young stellar objects revealed H0kp/ cal models and on galaxy formation. proto-planetary disks, jets emanating HST is the key tool used for recent In that page you can currently from the centers of accretion disks and determinations of the Hubble Constant, find the abstracts of published unprecedented details in the structure and for the calibration of a variety of papers, postscript files of of jets and Herbig-Haro objects. The methods of distance scale determina- accepted papers, and addresses study of stars of all masses now tions. of authors to contact for preprint permits the construction of theoretical A special session was devoted to information. models for winds from massive stars, future HST science instrumentation. In for supernova explosions, and for the Eventually, an archive of this session, the servicing missions of shaping of planetary nebulae and H Key Project data will be 1997, 1999 and 2002 were discussed, 0 structure formation in supernova available. as well as the recommendations of the remnants. The ability of HST to “HST And Beyond” study chaired by resolve stars in extremely crowded

News HST & Beyond Committee Report by Goetz Oertel, AURA President The Oertel Report of the “HST & Beyond” Committee was released in January 1996. This report makes specific recommendations toward the scientific goals of: (1) direct study of the birth and evolution of galaxies like the Milky Way; and (2) the detection of Earth-like planets around other stars and the search for evidence of life on them. Draft copies of the Report were available at the Explore HST’s greatest hits at January 1996 AAS meeting in San Antonio. http://www.stsci.edu/public.html. The HST & Beyond Committee was established by AURA in the spring of 1994. The Committee is chaired by Alan Dressler (Carnegie Observatories) and comprised of members from a cross-section of the U.S. astronomy community and Richard Ellis for the ESA community. Thanks to the committee for its visionary and thoughtful report!

6 February 1996

Scientific performing FOS target acquisitions, was below the background rate, and Instruments Status the FOS has been particularly sensitive consequently the FLYLIM option was by Ron Gilliland to the new FGS behavior. When guide used. FLYLIM is an on-board software star lock is not established at the time algorithm to increase the S/N by All of the instruments on HST have the FOS prepares to begin an exposure, suppressing bursts of background operated smoothly and productively the FOS is shut down for the duration noise. The PI of this program (C. throughout the fall and early winter. of the observational sequence as a Hogan, U. of Washington) hopes to Even the long idle f/48 relay of the safety precaution. Five FOS observa- derive more stringent limits on the He Faint Object Camera is now returning tional sequences have been lost since 1 II Gunn-Peterson effect. NGC 1741 is excellent science observations. For all October ’95 due to the new FGS1 loss- a starburst galaxy whose optical HST Observatory of the instruments efforts continue to of-lock problem. Four of the occur- spectrum indicates the presence of maintain and extend the calibrations rences were during ACQ/PEAK target hundreds of Wolf-Rayet stars. A and definition of data characteristics. acquisition sequences and one during G140L spectrum was obtained, whose More information on the science an initial moving target tracking slew. quality rivals any other ultraviolet instruments may be obtained from the Such lost observations are automati- spectrum in existence for this class of World Wide Web which is a repository cally repeated, but of course result in object. The PI Of the program (P. for frequently asked questions, lowered observing efficiency overall. Conti, U. of Colorado) will use the calibration details, and late-breaking New operational procedures are in numerous stellar and interstellar lines instrument news. place and are resulting in a much lower in the GHRS spectrum to study the rate of lost observations. During this stellar population and the interstellar FOC quarter the FOS was used to obtain the medium of NGC 1741. The f/96 relay has continued to highest time-resolution data of the provide excellent science observations. post-COSTAR era with 0.25 second WFPC2 As detailed in recent Newsletter readout times for the November 1995 The WFPC2 continues to work articles the FOC f/48 relay has been stellar occultation by Saturn and its extremely well. As WFPC2 is the making a comeback from operational rings (A. Bosh, Lowell Observatory). youngest science instrument on HST, problems with the high-voltage system Also during November a near-record the level of data characterization issues first encountered in September 1992. volume of RAPID mode data were under investigation remains significant. Development of more robust opera- obtained during nearly 10 continuous The most troublesome issue to surface tional procedures, and extensive orbits (CVZ) of high time-resolution in recent months concerns a possible characterization of the instrument has observations (3- and 6-sec readouts) to photometric zeropoint difference for resulted in bringing the f/48 relay back facilitate tomographic analysis of the long versus short exposures. This to limited science observing status in cataclysmic variable HT Cas (J. Wood, effect was first reported by GOs order to allow use of its unique long- Keele University). performing careful calibrations in slit spectroscopic capability. The first support of the extragalactic distance science program using the f/48 GHRS scale key project. Further investigation spectrograph — Long-Slit Spectros- As with the FOS, the GHRS has shows that “long” vs. “short” is copy of the Center of M31, Dr. Ivan continued to provide a steady stream of probably a misnomer. The level of King executed successfully on 5 high quality science observations, background appears to be the main December 1995. The target acquisition although the GHRS also experienced a parameter rather than the exposure strategy appears to have worked few lost observation sets due to the time. The magnitude difference perfectly. Use of an 8-hour warmup FGS1 loss-of-lock problem. The measured between short and long period allowed the detector back- GHRS in combination with grating exposures is more pronounced for faint ground noise level to stabilize G140L on Side-1 is becoming more stars in large apertures, where it can somewhat, avoiding the high levels and more popular among observers of reach 0.05 mag, and is essentially that had been seen shortly after the faint (by GHRS standards) extragalac- absent for stars with more than 1000 high voltage switch-on in earlier f/48 tic targets. One of the reasons is the total counts. The dependence on tests. capability of the GHRS to make use of aperture and magnitude appears the FOS acquisitions of faint targets, consistent with a charge transfer FOS which has been made available in efficiency problem. The offset of faint The FOS has continued to operate Cycle 5. One of the faintest objects star magnitudes can be explained by a smoothly. During the past three months ever observed with the GHRS was the loss of 0.3 DN (2 e-) in each pixel used occasional sticking problems have QSO Q0302-003, which is famous as a in the aperture. We are actively developed with one of the three test case to study the He II Gunn- pursuing this problem with further (FGS1) Fine Guidance Sensors used Peterson effect. A series of successful testing and analysis and encourage for routine HST observations. Because spectra was obtained during several those who require accurate absolute of the spacecraft motions required for visits this fall. The object count rate photometry for their observations to 7 SpaceST ScI NewsletterTelescope Science • HST Observatory Institute • Newsletter

pay special attention to information optical bench. The MAMA detectors Hubble Data concerning this topic on the WWW or have been somewhat more problem- Archive News to discuss it with their Contact atic. Although high quality tubes have by Megan Donahue Scientist. been produced and excellent results have been obtained from the engineer- A new version of the Space NICMOS ing model units during the optical Telescope Data Archiving and by John MacKenty testing of the instrument, some Distribution System (DADS) was installed on December 1. One of the The construction of the NICMOS difficulties were encountered in major enhacements is the abibility to science instrument continues on producing completed flight detector retrieve data directly to the user’s local schedule at Ball Aerospace in Boulder, assemblies. Problems with the high disk. This option is to be used only for CO. At mid-December 1995, the voltage power supply and the tube small requests. For larger requests, for NICMOS Dewar was successfully potting scheme are now thought to be sites with slow data transfer or loaded with cryogenic nitrogen. PI understood and we expect to have unreliable internet connectivity, users Rodger Thompson has been heard flight detectors ready for integration in should still request FITS tapes. Using remarking that “the NICMOS design is February. A major landmark was this new facility, PIs can now retrieve now truly frozen.” The NICMOS reached in November when a large their own proprietary data. PIs can also Dewar is expected to remain cold until portion of the flight hardware and designate specific co-investigators that 2002. The NICMOS flight optics have software were first tested together. The can have access to the data from all been assembled and are presently test exercised the mode select specific proposals. Please note that all being aligned. NICMOS will be mechanism (MSM), slit wheel, mode investigators desiring to retrieve integrated and tested during the spring isolation shutter and echelle blocker proprietary data from the Hubble Data at Ball and is expected to arrive at mechanisms and the band 2 (near-UV) Archive must be registered archive Goddard Space Flight Center in MAMA system through the flight users. You can register directly on a August 1996. electronics, using the flight software and the STScI-developed commanding StarView screen or filling the form at STIS software. This end-to-end test was http://stdatu.stsci.edu/ by George Hartig highly successful, generating spectra in registration_form. Please contact the several science modes. Additional tests archive hotseat at [email protected] The STIS instrument is now nearing of this type, incorporating more of the after registering if you are going to completion of its hardware integration hardware and software are scheduled retrieve proprietary data. and flight software development stages for late December and January. Nearly This new version of DADS also at Ball Aerospace. Final optical every science mode of the instrument changed the name extension of the integration activities are now in has now been tested, from the far UV files retrieved from the Archive. It is progress. All of the science-mode to the visible, to assess the quality of now fits instead of fit. This will make gratings and mirrors are now installed the optical alignment. After some them more compatible with all FITS on the optical bench, with exception of adjustments were made to correct processing packages. In addition, all the spherical aberration corrector small focus offsets between several of GO tapes will now include the jitter group, which was successfully tested the gratings and mirrors on the MSM, files for every observation. An as a subsystem in September. The the optical performance of all modes automatic message will now be sent to calibration systems, comprising 6 lamp appears to readily meet the specifica- GOs and GTOs notifying them that a subsystems and about a dozen mirrors tions. Some 500 images and spectra tape was mailed. This last enhance- and beamsplitters, have been as- have been acquired, logged and ment will allow our operators to sembled and are due to be installed in archived to date as a result of this concentrate more on quality control. December. All seven of the mecha- testing. Meanwhile, the STScI is hard nisms have been assembled and all but StarView 4.2 at work to develop the commanding, the aberration corrector mechanism A new release of StarView is calibration and user-support software and calibration insert mechanism have available. Several new features were and documentation required to been tested and installed. The added to its capabilities: effectively use the STIS after its electronics are also nearing comple- installation in the HST. • a utility to overlay the apertures of tion, with the second of the two HST instruments on the images (redundant) main electronics boxes extracted from the Digitized Sky undergoing final assembly and Survey environmental testing in December. continued page 9 The flight CCD detector finished environmental testing in early December and is now installed on the

8 February 1996

RPS2 for Cycle 6 • Drop to Gyro If Necessary - For • Requires Ephemeris Correction Observations observations of the same target with indicates that a correction for by Ashim Bose, Glenn Miller different instruments (e.g. FOS and position errors due to moving-target and Karla Peterson WFPC2) it may not be possible to and/or HST ephemeris uncertainty use the same guide star pair for both may be needed to execute the A new version of RPS2 has been observations. If the WFPC2 is being exposure. This special requirement is released. It incorporates a number of used for a quick image, then Drop to only valid for exposures with moving enhancements suggested by users. Gyro will allow the WFPC2 targets. Cycle 6 observers should use this exposure to be taken under gyro • Multiple Guide Star visits - observa- version. pointing and avoid the expense of the tions requiring different guide stars Observers & Proposers Observers familiar with RPS2 from acquisition of a new guide star pair. can now be modeled within a single the last cycle will find that the “look • Low-Sky and Shadow - Low sky visit. and feel” of RPS2 is largely un- requests that the current exposure be changed. We just concentrated on taken when the total background An updated copy of the Cycle 6 adding new observing capabilities. light is no more than 30% greater Proposal Instructions will be mailed to Perhaps the most notable change is the than the yearly minimum value of the Cycle 6 observers, but an electronic new, prototype graphical Proposal zodiacal background for that target. version is available from the STEIS EDitor (PED). Instead of typing To minimize Earth shine, the Phase II Proposal Development page. information into a flat text file, PED, exposure will also be taken when the This new version of RPS2 can be with its point-and-click facilities, target is at least 40 degrees from the downloaded from the “Phase II allows you to enter data quickly and bright Earth. This limits visibility Proposal Development” page (under easily into graphical forms. It provides time to about 48 minutes per orbit. the Observer page). syntax checking and explanations on Efficiency and schedulability are We welcome your comments and legal and illegal options. reduced with this special require- suggestions on RPS2 and the new New observing capabilities with this ment, but to a much lesser degree Proposal Editor. Please send them to version of RPS2 include: than with SHADOW which requires your Program Coordinator. • Optional parameters which simplify the observation to be taken when the the specification of WFPC2 dithering HST is in the Earth’s shadow. • Schedulability special requirement • Save and Use Offset replace which allows you to increase the Interactive Acquisitions in many flexibility of tightly constrained situations and allow the offsets from observations by requiring smaller Onboard Acquisitions to be used in a target visibility intervals later visit.

Hubble Data Archive from page 8

• the tables summarizing query results http://stdatu.stsci.edu dist_starview. software. The survey is at http:// saved in StarView can be customized html for the following platforms: stdatu.stsci.edu/survey/. If you do not SunOs 4.1.3, Solaris 2.4, VAX VMS, have access to the WWW and would • columns to be saved to a file can be OpenVMS for DEC Alpha and DEC like to participate, please send a chosen and ordered UNIX (OSF/1) for the DEC Alpha. message to [email protected] and we • the width of the table columns in the will mail you a copy. StarView screen and in the saved file Hubble Data Archive User Survey can be modified interactively. We are conducting a survey of the HST user community through DADS New Features The Observatory Monitoring System February 1996. This is an opportunity • retrieval of files directly to your local disk screen has been added to StarView. for our users to give us input on future • PIs can retrieve their own proprietary data This will facilitate the retrieval of the directions and policies of the Archive. • jitter files included for all observations jitter files and also to search on new We would like to hear your sugges- • retrieved files extension is .fits fields such as the telescope roll angle tions and comments on recalibration, • automatic generation of tapes and the Earth-Sun limb angle, for data media, Archive services and • PIs notified automatically that tapes are mailed example. Distributed StarView is available at ftp://stdatu.stsci.edu/pub/starview or 9 SpaceST ScI NewsletterTelescope Science • Observers Institute & Proposers • Newsletter

GO and AR Statistics of PI by country Panel and TAC Members for Cycle 6

Country Submitted Approved Telescope Allocation Committee Members at Large Michael A’Hearn, Chair Alan P. Boss Australia 12 8 Philip A. Charles Austria(*) 1 0 Panel Chairs Mario Livio Belgium(*) 2 2 Peter Conti (Hot Stars) George Miley Brazil 2 1 Heidi Hammel (Solar System) Alexander Szalay Canada 26 13 Craig Foltz (Quasar Absorption Lines) Virginia Trimble Chile 2 1 Kenneth Freeman (Stellar Populations) Andrew Wilson Denmark(*) 2 0 John Meaburn (ISM) Finland(**) 2 1 Theodore Simon (Cool Stars) France(*) 33 16 Alan Stockton (AGN) Germany(*) 46 28 J. Anthony Tyson (Cosmology) India 2 0 Brian Warner (Binaries & Star Formation) Israel 3 1 Tim de Zeeuw (Galaxies and Clusters) Italy(*) 25 9 Japan 1 0 Mexico 4 3 PANELS Ray Sharples Netherlands(*) 13 6 Rogier Windhorst New Zealand 1 0 AGN Richard Barvainis Hot Stars Russia 1 0 Charles Bailyn South Africa 2 1 Chris Carilli Paolo Padovani Kris Davidson Spain(*) 10 2 James Ulvestad Urlich Heber Sweden(*) 4 2 William van Bruegel Nancy Morrison Switzerland(*) 5 1 Roeland van der Marel Regina Schulte-Ladbeck United Kingdom(*) 94 29 Sylvain Veilleux Edward Sion United States 732 372 Beverly Wills Donald Winget Total 1025 496 Binaries and Star Formation ISM Dana Backman Harriet Dinerstein Anne Cowley Robert Fesen (*) ESA member state Donald Garnett (**) ESA associate member state Ronald Kaitchuck Peter Leonard George Jacoby Tom Marsh Derck Massa Geraldine Peters John Mathis Bo Reipurth Patrick Roche Gary Schmidt Michael Shull Michael Simon Quasar Absorption Lines Cool Stars Jill Bechtold Kenneth Carpenter Peter Jakobsen Douglas Duncan Lenox Cowie Andrea Ghez David Meyer Donald Luttermoser Patrick Petitjean We would like to thank the Roberto Pallavicini David Turnshek John Webb members of the TAC & Panel Dieter Reimers Peter Stetson Solar System for their work. Cosmology James Bell Edmund Bertschinger Michael Brown Mark Dickinson Larry Esposito George Djorgovski Alan Fitzsimmons Alan Dressler Caitlin Griffith Puragra Guhathakurta David Jewitt Robert Kirshner Nicholas Schneider Michael Rowan-Robinson Stellar Populations Galaxies and Clusters Beatriz Barbury Kirk Borne Timothy Beers Jane Charlton Gerard Gilmore Harry Ferguson John Hillier Holland Ford Rosemary Mardling Robert Kennicutt Michael Rich Jeremy Mould Patrick Seitzer

10 February 1996

Cycle 6 — Summary Table

AGN BSF COS CS G&C HS ISM QAL SP SS Total

proposals received

GO 120 125 94 70 104 78 93 51 106 77 918

SNAP 712282322029

AR 143184122845878

orbits requested

1949 1400 2069 966 1281 789 1215 935 1783 1156 13543

accepted proposals

GO 34 56 46 36 53 46 46 22 49 47 435

SNAP 412262321023

AR 535472413438

accepted primary orbits

534 509 769 322 473 283 382 326 555 421 4574

accepted proposals

FOS (pure/mixed) 10/2 13/5 1/0 0/0 6/6 9/3 3/7 9/4 5/1 9/8 65/36

GHRS (pure/mixed) 3/0 16/5 1/1 18/0 4/2 4/4 17/2 6/4 1/0 6/8 86/26

FOC (pure/mixed) 3/1 2/1 4/2 4/0 1/2 3/2 1/0 2/0 0/0 0/1 20/9

WFP (pure/mixed) 19/3 17/1 39/3 8/0 39/8 16/4 21/7 3/0 43/1 20/10 206/37

FGS (pure/mixed) 0/0 3/0 0/0 8/0 0/0 0/0 0/0 0/0 0/0 0/0 11/0

accepted primary orbits

FOS (pure/mixed) 169/22 129/70 3/0 0/0 51/96 48/46 19/110 131/48 102/4 58/90 710/486

GHRS (pure/mixed) 130/0 147/70 10/11 157/0 70/14 75/55 129/14 93/48 19/0 49/87 779/299

FOC (pure/mixed) 33/16 5/20 50/55 20/0 7/12 13/9 1/0 0/0 0/0 0/8 129/120

WFP (pure/mixed) 264/38 126/20 655/66 77/0 228/112 83/48 23/110 54/0 430/4 185/113 2225/511

FGS (pure/mixed) 0/0 12/0 0/0 68/0 0/0 0/0 0/0 0/0 0/0 0/0 80/0 accepted ESA PIs 9 15 10 2 17 16 8 4 11 9 101

accepted ESA primary orbits

GO 102 116 68 22 121 87 50 36 96 71 769

SNAP 110 25 0 0 257 00000382 (17%)

11 STSpace ScI NewsletterTelescope Science • Observers Institute & Proposers • Newsletter

Approved Observing Programs for Cycle 6 Continued AntonucciAntonucciBaumBirettaBoyle University of California, Santa BarbaraCecil University of California, Santa BarbaraCimattiCohen Space Telescope Science InstituteDey Space Telescope Science InstituteDickinsonDunlop Royal Greenwich ObservatoryEvans University of North Carolina Lawrence Livermore National LaboratoryFerland University of California, San DiegoFosbury Confirming the Quasar in Cygnus A Space Telescope Science InstituteGoodrich The Spatially Extended Featureless Continuum Source of Cygnus A: Multicolor Imaging in Total Flux and Polarization Kitt Peak National ObservatoryGoodrich Institute for Astronomy, University of EdinburghGoodrich Harvard Smithsonian Center for AstrophysicsHeckman Black Holes and Gas Disks in a Complete Sample of Radio Loud UGC Ellipticals University of KentuckyHo Secular Changes in the Jet of M87 Space Telecope European Coordinating FacilityHutchings Space Telescope Science Institute UV Spectropolarimetry of Nearby Powerful Radio Galaxies Kay Space Telescope Science Institute High-resolution imaging of X-ray selected AGN Koratkar Space Telescope Science Institute A comparative HST imaging study of radio galaxies and the hosts radio-loud radio-quiet quasars. Johns Hopkins UniversityKriss Geometry and Generalizability of the Reflected Light Model for Seyfert 2 Galaxies The Helical Jet/ISM Interaction in NGC 4258 Lacy Dissecting 3C 324: Anatomy of an Aligned Radio Galaxy at z = 1.206 The Nuclear Ionization Field of NGC 1068 Dominion Astrophysical ObservatoryLehnert Studying the UV emission line spectrum of high z radio galaxies. Effects geometry and dust. Center for Astrophysics The Origin of the Alignment Effect: WFPC2 Imaging Polarimetry High Redshift Radio Galaxies LongairMacKenty Space Telescope Science Institute Barnard College, Columbia UniversityMaozMathur Johns Hopkins University A Hidden Power Source in the QSO PG 1630+377 Minniti Oxford University Dust in the Broad-Line Regions of Seyfert Galaxies Institute of Geophysics and Planetary PhysicsPogge Fe II Emission in AGN: the Confrontation between Theory and Observations Narrow-Line Seyfert 1s and the Iron Enigma in Active Galaxies Cavendish Laboratory, Cambridge University Space Telescope Science InstitutePuchnarewiczRawlings Imaging of QSO Host Galaxies at z>2 Sparks Tel-Aviv University Smithsonian Institution Astrophysical Observatory Ultraviolet Spectroscopy of Seyfert 2 Nuclei: Testing the Starburst-AGN Connection Stanford Mullard Space Science Laboratory Lawrence Livermore National LaboratoryStockton Multicolor Imaging Polarimetry of Obscured Seyfert 2 Nuclei Below the Lyman Edge: UV Polarimetry of Quasars The Evolution of Radio-Loud Quasars II Ohio State UniversityStocktonTadhunter WFPC2 Imaging of 2 Jy radio galaxies Astrophysics, Oxford University The Ultraviolet Properties of “Dwarf” Seyfert 1 Nuclei Urry Space Telescope Science Institute GHRS Observations of NGC5548 Welsh Insitute of Geophysics and Planetary PhysicsWhite A Snapshot of the UV Spectrum Mrk 335 Institute for Astronomy Bulge Morphology of Seyfert Galaxies Wills Institute for Astronomy, University of Hawaii University of SheffieldWilson Resolving Stars around the Nearest Known Seyfert 1 Nucleus HST imaging of the two most distant radio galaxies Investigating high-temperature big bumps in AGN Space Telescope Science Institute Keele University A SNAPSHOT Survey of ‘Radio-Loud’ IRAS Galaxies: Exploring the Genesis Post—Starburst AGN Space Telescope Science Institute High-Resolution Narrow-Band Imaging of LINERs, in Search Their Central Engines University of Texas at Austin Weak radiogalaxies at z > 2: imaging a unique sample University of Maryland The Optical Structure and Environments of z~1 3CR Quasars Blue Continuum Snapshots of 3CR Radio Galaxies The Interaction Between Active Galactic Nuclei and their Host Galaxy Environment Deep Imaging of Extended Optical Structure around the Quasars 4C37.43 and 3C351 The Environments and Host Galaxies of BL Lac Objects Resolving the Shocks in Powerful Radio Galaxies HST WFPC2 Observations of MilliJansky Radio Sources from the FIRST Survey Soft X-Rays and the UV Spectra of a Complete QSO Sample Ultra—Rapid UV Continuum Variability as a Probe of AGN Physics Testing Unified Models with a Complete Sample of Seyfert Galaxies

AGN

12 February 1996

Approved Observing Programs for Cycle 6 Continued BallyBaptistaBellBeuermannBeuermannBodenBohm-Vitense University of Colorado University of St AndrewsBond Universitaets-Sternwarte GoettingenBruhweiler Universitaets-Sternwarte Goettingen NRAL Jodrell Bank, University of ManchesterClampin University of WashingtonClampin Jet Propulsion LaboratoryCoolDevine Catholic University of AmericaEdmonds Space Telescope Science InstituteEisloeffel Space Telescope Science Institute Light Curve of an Eclipsing Millisecond Pulsar Companion Ferguson Space Telescope Science InstituteFranz The Accreting Magnetic White Dwarf in AM Her:,Heating, Chemical Composition and Mass Fridlund Supersoft sources in the LMC University of California, Berkeley University of Colorado Space Telescope Science InstituteFruchter Spectral Mapping of Accretion Disks in Cataclysmic Binaries: Bridging the CV Period Gap Gehrz Probing Proto-Planetary Disks in the Orion Nebula Laboratoire d’Astrophysique Ferguson EnterprisesGiesGies White dwarf companions of Barium and CH peculiar Stars Lowell ObservatoryGrindlay Astrophysics Division, European Space Agency Is the Central Star of K 648 in M15 a Close Binary? WFPC2 SV-PSF Characterization and Restoration in Morphological Photometric Analyses Guinan Determining the Physical Conditions in Gas Infall of Beta Pictoris Space Telescope Science Institute Polarimetric mapping of R Mon’s circumstellar environment Hartigan Dust properties in the Beta Pictoris disk: a case for imaging polarimetry University of MinnesotaHaswellHeber Georgia State UniversityHellier Optical Counterparts for Low-Luminosity X-ray Sources in Globular Clusters Harvard University Georgia State University Spectra of Faint Variables in 47 Tuc: CVs or LMXBs? Kaspi Velocity field and small scale structure in the L1551 IRS5 jet Villanova UniversityLandsman Rice UniversityLong Imaging Arcsecond Scale Jets from Young Stars Columbia University PC Imaging of HH29: The Nearest Interstellar Shock Margon Universitaet Erlangen-NuernbergMarsh High-Speed Photometry of the UV Counterpart to 4U 1820-30 Keele University Direct measurement of the BE Ursae Majoris sdO primary star mass-a critical test case for common envelope evolution Mason Hughes STXMauche IPAC/Caltech/JPLMauche Masses of Low-Luminosity Hyades Cluster Members O’Donoghue Space Telescope Science Institute University of WashingtonPadgett High Resolution Imaging of the Massive Overcontact Binary RY Scuti Southampton UniversityParesce The Masses of the O-type Binary 15 Monocerotis Mullard Space Science LaboratoryPatterson Lawrence Livermore National Laboratory Be + HELIUM STAR BINARIES Plavec University of Cape Town Lawrence Livermore National LaboratoryPolidan Spectroscopic Study of Origin and Nature CVs in Globular Clusters Resolving sdB binary systems Reipurth Eclipsing Binaries in the Magellanic Clouds: Fundamental Properties and Distances IPACRosen European Southern Observatory Outbursts in Black Hole X-Ray Transients Columbia University Shock Waves and Momentum Transfer in the Young Stellar Outflow Cepheus A SchmidtSchmutz Dwarf Novae in Quiescence University of CaliforniaSchultz NASA/Goddard Space Flight CenterSchultz Simultaneous Multiwavelength Observations of the Dwarf Nova Oscillations SS Cygni European Southern Observatory Spin-cycle variations of the UV emission lines intermediate polars The Eclipsing Binary Pulsar PSR B1718-19: A Clean RS CVn System? Schwope Dissecting the Wind and Disk of Nova-like Variable V347 Puppis Changing perspectives on accretion disk winds Time-Resolved Spectrophotometry of the Smallest Mass Function Binary Star University of LeicesterShara The post mass-transfer binary S1040 in M67 University of Arizona Institute of Astronomy The accretion disk and white dwarf in the nova Newdn Computer Sciences Corporation Fundamental properties of a DA—dM detached eclipsing binary with P_orb=3^h37^m Computer Sciences Corporation Astrophysical Institute Potsdam FOC Observation of the Evolution R Aqr Jet Space Telescope Science Institute Spectropolarimetry of Ultraviolet Continuum and Line Emissions in Binary Stars Proper Motions of Herbig-Haro Jets Ultraviolet Pulsations in WZ Sagittae Accretion in the Interacting Binary UX Monocerotis Evolution of Pre-Main Sequence Circumstellar Nebulosity Doppler mapping of chromospheric and transition region UV emission lines in BW Dra. Pyramid Imaging of Circumstellar Material About Nearby Stars Resolving the Unique Magnetic/Non-Magnetic Double-Degenerate Binary LB 11146 Decoding the Inner Disk about Beta-Pictoris Understanding the Simplest Symbiotic System(s), II. The 1996 eclipse of RW Hydrae Ultraviolet Mapping of the Unique Polar HU Aqr Where are the Dozens of Predicted Cataclysmic Variables in Globular Clusters?

Binaries and Star Formation

13 STSpace ScI NewsletterTelescope Science • Observers Institute & Proposers • Newsletter

Approved Observing Programs for Cycle 6 Continued SharaSionSoderblomStapelfeldtStockmanSzkody Space Telescope Science InstituteTavani Space Telescope Science InstituteVennes Department of Astronomy and Astrophysics Jet Propulsion LaboratoryWade Space Telescope Science InstituteWood University of Washington Columbia University UC Berkeley, Center for EUV Astrophysics The Pennsylvania State University GHRS Spectroscopy of the exposed white dwarf in High Accretion Dwarf Nova RX And Keele University UV and HAlpha-bright Stars in the Core of NGC 6752 HD 98800, An Extraordinary K Star: Completion of the Astrometry in Cycle 6 Accretion Streams in Magnetic Variables: FOS Eclipse Studies of 5 ROSAT/HEAO 1 Sources Imaging of the HH 30 Circumstellar Disk and Jets Fundamental Parameters of White Dwarfs in Close Binaries with Late-Type Stars The Identification and Cooling of the White Dwarf in WZ Sge-Like System AL Com UV Spectroscopy of face-on accretion disks High-resolution imagery of jets from superluminal X-ray transients Phase Resolved UV Spectroscopy of the Peculiar Binary V Sge ArmusBrowneBunkerConnollyCoteCowie California Institute of TechnologyDey Nuffield Radio Astronomy LaboratoriesDickinson University of Oxford, Department AstrophysicsDjorgovski Johns Hopkins UniversityDonahueDressler European Southern Observatory Institute for Astronomy, University of HawaiiEisenhardt Space Telescope Science InstituteElston Kitt Peak National Observatory California Institute of TechnologyFalco Are the damped Lyman-Alpha systems at z>3 really spiral galaxies? Ferguson Space Telescope Science Institute B2114+022: a gravitational lens system and/or an example of multiple active nuclei? Fort OCIW Jet Propulsion Laboratory Is IRAS 15307+3252 Gravitationally Lensed ? FrancisGiavalisco Imaging of z > 1 Massive Star Forming Galaxies Cerro Tololo Inter-American ObservatoryGilliland Space Telescope Science InstituteGriffiths Smithsonian Astrophysical ObservatoryGuhathakurta Evolution of Galaxies Through Multicolor Space Galaxy Rotation Curves at Large Radius using Ly-alpha Absorption Lines Impey HST Observations of a ‘Clusterless’ Giant Arc centered on 3C 220.1 Observatoire de Paris University of Melbourne OCIWJackson The Evolution of Elliptical Galaxies in Clusters The Reddest Objects in the Universe Jedrzejewski Space Telescope Science Institute Star Formation and Galaxy Morphologies in Distant, X-ray Luminous Clusters of Galaxies UCO/Lick ObservatoryKinney Johns Hopkins UniversityKoo The Nature of Very Red Field Galaxies Kron University of ArizonaLawrence Space Telescope Science Institute A Search For Multiple Images of QSOs Seen Through Damped Ly-alpha Absorbers Nuffield Radio Astronomy Laboratories, Jodrell Bank Lenses, Mirrors, and HST: IRAS FSC10214+4724 Under a Compound Microscope Lilly The Far-UV Evolution of Elliptical Galaxies Lowental Space Telescope Science InstituteMileyMould Lick Observatory Observations of a new sample gravitational lens candidates Jet Propulsion LaboratoryPierce The University of Chicago The Butcher-Oemler Effect A Search for Supernovae at High Z in the Hubble Deep Field Postman Imaging a Cluster of Galaxies at Redshift 2.38 Saglia LICK OBSERVATORY Weak Lensing in the Field of Luminous Quasars: Masses Groups Galaxies and Magnification Bias. University of TorontoSandageSchade Leiden Observatory Cosmology with the Deep Medium Survey Confirmation of a New Small-Separation Gravitational Lens Candidate Measuring Luminosity Evolution in z=0.3 Field Galaxies from Internal Kinematics Mt. Stromlo and Siding Springs ObservatoriesSchechter Indiana UniversitySmail Space Telescope Science Institute High-Redshift Galaxies and Their Contribution to the Ionizing Background Spectral Evolution of High Redshift Galaxies Institut für Astronomie und Astrophysik, Müenchen Imaging the Gravitational Lens System 1422+231 OCIW University of Toronto MIT Determination of the Extragalactic Distance Scale Emission-Line and Continuum Imaging of the Gravitational Lens System 21016+112 OCIW Dynamical Properties of Distant Field Galaxies The evolution of elliptical galaxies in distant clusters Spatial Structures, Kinematics, and Masses of Faint Field Galaxies Detailed Morphology of a Lyman-Alpha Galaxy at z=2.3 Morphology and Photometry of Galaxies in Optically Selected High Redshift Clusters Rest-frame ultraviolet imaging of normal galaxies at high redshifts Morphologies of high-redshift radio galaxies A Cepheid Search in the Virgo Cluster Galaxy NGC 4571 Quantitative measures of the evolution cluster galaxy population Calibration of Nearby Type Ia Supernovae as Standard Candles: NGC 3627 and SN 1989B What causes the astigmatism in gravitational lenses? An Ultra-Faint Galaxy Count and Redshift Survey Using Cluster Lenses

COSMOLOGY

14 February 1996

Approved Observing Programs for Cycle 6 Continued SparksSuntzeffSurdejSurdejSzalayThuan Space Telescope Science InstituteTonry Cerro Tololo Inter-American ObservatoryTyson Space Telescope Science Institutevan Breugel Space Telescope Science InstituteWarren The Johns Hopkins UniversityWindhorst University of VirginiaYee Massachusetts Institute of TechnologyZepf Lawrence Livermore National Laboratory AT&T Bell LaboratoriesZirbel Supernova Host Galaxies Imperial College of Science Technology and Medicine Arizona State University Geometric measurement of galaxy distances Mass Determination of QSOs Using Gravitational Lensing University of Toronto A New Gravitational Lens Candidate: QSO 0449-1645 A&B University of California, Berkeley Mapping an optical Einstein ring Haverford College Detailed Studies of two z>3.5 Radio Galaxies The Cosmic Velocity of the Great Attractor Modelling Cluster Mass Distributions from Gravitationally Lensed Arcs Nearby young dwarf galaxies and their Lyman Alpha emission The Enigma Lens Q2345+007: Early Assembly of Dark Matter? WFPC2 Ly-alpha imaging of galaxy clusters at z=2.4: formation from compact sub-galactic clumps? Using a Cepheid based Distance to Test the Large Peculiar Motions Inferred in Centaurus Region Imaging of a Protogalaxy at z=2.7 Discovered by its Young Stellar Population The Evolution of Galaxies in Groups AyresAyresBaadeBenedictBenedictBoehm-Vitense University of ColoradoBrown University of ColoradoBrown Hamburger SternwarteBrown McDonald University of WashingtonCarpenter McDonald ObservatoryCookCowan University of ColoradoCuntz Space Telescope Science InstituteDuncan LASP University of ColoradoDupreeDupreeGhez Naval Research Laboratory University of OklahomaGuinan University of Colorado/JILAHarrison University of Chicago Fishing in the Coronal Graveyard Henry Smithsonian Astrophysical Observatory Sleuthing the Dynamo: The Final Frontier Kastner Cepheid Masses Probing the extended envelope of Zeta Aur type binary 32 Cyg Smithsonian Astrophysical ObservatoryKirkpatrick Continuation of An Astrometric Search for Planetary Companions to Proxima Centauri Linsky University of California Los Angeles A Search for Superplanets Around Weak T-Tauri Stars Villanova UniversityLuttermoser New Mexico State UniversityMacConnell Detection and Mass Determination of Low-mass Companions to Nearby M Dwarfs - Continuation Unravelling the Complex Wind from Zeta Aurigae: Cycle 6 Portion Space Telescope Science InstituteMagnier Massachussetts Institute of Technology JPL/IPACMassa Activity on the Edge of Convection: The Atmosphere Canopus (F0 Ib-II) Mathieu Applied Research Corporation Spectroscopic diagnostic for late-type stellar atmospheres Direct Imaging of Betelgeuse University of Colorado / JILAParsons Computer Sciences Corporation Capella: Separating the Giants Peterson Abundances of Very Heavy Elements in the Early Galaxy. III. A detailed analysis of GHRS spectra Alpha Ori (M2 Iab) using stochastic wave radiation-hydro models Reid University of IllinoisRosenthal Locating Disks, Accretion Flows, and Outflows in Close Binary T Tauri Stars Probing the Chromospheric Structure of Alpha Tau Be-deficient Halo Stars: Implications for Galactic Chemical Evolution and Cosmology Applied Research CorporationSaar University of Wisconsin - MadisonSakai Computer Sciences Corporation FOC Imaging of the Dusty Envelopes Mass-Losing Supergiants Simon Astrophysical Advances The Distances to Dwarf Novae, and the Calibration of Technique Infrared Spectroscopic Parallax Calibrating the Mass-Luminosity Relation at End of Main Sequence Center for Astrophysics Probing the Dynamo for Stars with Shallow Convection Zones: The Young F0V Star 47 Cas California Institute of Technology Density Diagnosti for the Dynamic Atmospheres of LPV Stars Smithsonian Astrophysical Observatory PC Astrometry of the Brown Dwarf Candidate PPL 15 Systematic Analysis of Mass Loss from Evolved Stars Jet Propulsion Laboratory University of Hawaii Determining the Binary Frequency for Ultra-cool, Nearby M Dwarfs Dynamical Masses for the Stars in Pre-Main- Sequence Spectroscopic Binary 045251+3016 Determination of the Distances and Masses 2 Galactic Cepheids The Mass of the Bright Giant HD 173764 The disk and jet structure of Holoea Low-mass binaries in the Hyades - completing survey Rapid UV Variability: The Contribution of Flare Heating in the Atmospheres Active, Evolved Stars Calibrating Boron Abundances with RR Lyrae A Search for Brown Dwarfs and Luminous Young Planets in the Hyades Color Calibration of the Tip Red Giant Branch Luminosity A Hyades Enigma: 71 Tauri

COOL STARS

15 STSpace ScI NewsletterTelescope Science • Observers Institute & Proposers • Newsletter

Approved Observing Programs for Cycle 6 Continued SimonSimonSmithSmithStaufferTaff University of HawaiiVilhu State University of New York UCO/Lick Observatory University of Texas Center for Astrophysics The Johns Hopkins Universit University of Helsinki Observatory Orbits of Pre-Main Sequence Binaries The High Chromospheres of the Late A Stars, Altair and Alpha Cephei A Search for Outflows and Mass Loss from Population II Red Giants A New Tool for Probing Magnetic Activity with CIV Line Profiles The Mass Function and Binary Star Fraction of the Trapezium Cluster Continued Observations for Orbit and Individual Mass Determinations the Low-Mass Binary L722-22 The Origins of Boron AllenBattinelliBertolaBorneBowenBregmanBregman Space Telescope Science Institute Osservatorio Astronomico di RomaButa University of PadovaCalzetti Hughes STXCarollo Royal Observatory EdinburghCecil University of MichiganCharles University of MichiganCharltonCiardullo University of Alabama Space Telescope Science InstituteColina Sterrewacht LeidenConti The nature of the density cusp in core Ursa Minor The Opacity of Spiral Galaxy Disks Currie University of North Carolina, Chapel Hill Oxford UniversityDanly Pennsylvania State Universityde Zeeuw The Pennsylvania State UniversityDettmar Space Telescope Science InstituteDopita The interstellar medium of nearby galaxies using supernovae as probes Unveiling the Nature of Ultraviolet Spike at Center Sa Galaxy NGC 2681 Elmegreen JILA University of MarylandFaber Sterrewacht Leiden WFPC2 Mapping of Dust Obscuration and Stellar Populations in Starburst Galaxies. Cooled Gas in X-Ray Emitting Elliptical Galaxies Space Telescope Science InstituteFerguson The Cool Interstellar Medium in Hot Clusters of Galaxies Filippenko Fine Structure in the Nuclear Superbubble of NGC 3079 Snapshot Survey of the Ultraluminous IRAS Galaxy Sample Ruhr-Universitaet BochumForbes Vassar College Mt. Stromlo and Siding Spring ObservatoriesFord Nuclear Rings: Probing the Hearts of Barred Galaxies Franx Exploring PN Production as a Probe of Elliptical Galaxy Stellar Populations Formation of Stellar Systems in Mergers a Compact Group Galaxies Space Telescope Science Institute University of California, Santa CruzGarcia-Vargas Cusps or cores in barred bulges? University of California, BerkeleyGiavalisco UV Imaging of Circumnuclear Starburst Rings Goudfrooij High resolution UV imaging of M33-X8, the nuclear X-ray source in M33 UCO/Lick ObservatoryHodge VILSPA, IUE Observatory. ESAHodge Johns Hopkins University A Study of the Gaseous Halo Andromeda Galaxy A Definitive Test for the Excitation Mechanism of LINERs Kapteyn Astronomical InstituteHunter OCIWJaffe FOS Spectroscopy of NGC 1316 (Fornax A) European Southern ObservatoryKeelKenney High Resolution Imaging of Ionized Gas in the Disk-Halo Interface Spiral Galaxies Black holes in kinematically decoupled cores: a study of IC 1459 University of WashingtonKobulnicky Black Holes and Cores of Early-Type Galaxies Intergalactic Stars in the Virgo Cluster University of WashingtonKurt Super Star Clusters and H II Regions in Nuclear Rings Lowell Observatory Hot Stars and Young Super Star Clusters in the Wolf-Rayet Starburst Galaxy He 2-10 LaydenLeitherer Sterrewacht Leiden HST Observations of Galaxies in a Close, Nonmerging Encounter Lequeux University of Alabama Yale University University of Minnesota Unveiling the massive star content in prototypical nuclear starburst NGC7714 Resolving the Radio Hotspots in Nearby Starburst Galaxies Fundamental Plane, Morphology-Density Relation, and Lensing in the z=0.58 Arc Cluster CL2053 Kinematics of Ionized Gas in the Dusty Nuclear Disk NGC 6251; An Excellent Candidate for a Massive Black Hole Rice University McMaster University Ionized Gas with Broad Emission Lines in the Nuclei of Ellipticals Space Telescope Science Institute Observatoire de Paris The Spiral Arms of NGC 4321 The Optical Thickness of the Magellanic Clouds A UV Atlas of Nearby Galaxies Intermediate Mass Stars and Unusual Stellar Limits in a Starburst Galaxy The Nuclear Morphology of Elliptical Galaxies C and N Production Pollution Mechanisms in Low-Metallicity Extragalactic HII Regions Dust Structure in Backlit Galaxies NGC1569 as a Local Probe of Galaxy Evolution at High Redshift — Part 2: Spectroscopy The Collisional Debris of NGC 4438 The Nucleus and Stellar Populations of the dEn Galaxy NGC 5206 Abundances in the neutral medium of blue compact galaxy IZw 18 WFPC2 Imagery of the Dusty H ii Region SMC N88A

GALAXIES AND CLUSTERS

16 February 1996

Approved Observing Programs for Cycle 6 Continued LuMacchettoMalkanMalkanMcHardyMeurer Space Telescope Science InstituteO’Dea CaltechOdewahn University of CaliforniaOliver University of CaliforniaRix Physics Department, University of SouthamptonRose The Johns Hopkins UniversityRowan-Robinson Space Telescope Science Institute Arizona State UniversitySakaiSchreier Blackett Laboratory, Imperial College Imperial College of Science Technology and MedicineShopbell The Origin of the X-Ray Background: What are faintest Galaxies? Silk Dynamics of the Circumnuclear Disk in M87 Steward ObservatorySkillman Department of Physics & AstronomySmith Hyper-luminous IRAS Galaxies: Star formation, AGN or Lenses? Soifer Jet Propulsion Laboratory Space Telescope Science InstituteStiavelli California Institute of Technologyvan der Marel Subarcsecond Structures in Nearby Normal Galaxies — Do They Differ From Those Active Galaxies? Windhorst UV Spectroscopy of the Luminous Cooling Flow Nebula in A2597 University of Minnesota Ionized Gas Disks In Nearby Early Type Galaxies: A Key to Measuring Supermassive Black Holes Star Clusters And The Duration Of Starbursts University of California, BerkeleyZabludoff Snapshot Survey of Ultraluminous Infrared Galaxies University of ArizonaZaritsky A New Abundance Reference at the Present Epoch Institute for Advanced Study California Institute of Technology Neural network classification of deep WFPC2 images: Archival studies field galaxy evolution Space Telescope Science Institute The Butcher-Oemler Effect in Nearby Clusters of Galaxies Arizona State University Carnegie Observatories Optical Morphology of NGC 5128: X-ray Ridges and the Geometry Dust Lane UCO/Lick Observatory The spatial distribution of dust extinction through spiral disks The Galactic Wind in M82: Structure and Excitation of the Optical Filaments The Unknown Stellar Populations in Amorphous Galaxies: NGC 3077 and M82 Globular Cluster Formation in Galaxy Mergers: What, Where, When, Why, and How I Zw 18: Building a Model High Resolution Imaging of the Luminous Infrared Source IRAS 09104+4109 Core properties of the bulges spiral galaxies Nuclear structure & merger—starburst relation in the ultraluminous IRAS galaxy NGC 6240 Ultraviolet Imaging Polarimetry of the Low-Redshift BALQSO Mrk 231 The WFPC2 B-Band parallel survey: a systematic and synoptic study of galaxy formation evolution The Detailed Morphology of Post-Merger Galaxies Lopsided Galaxy Disks and the Accretion Rate BailynBarstowBianchiBignamiBobrowskyBolte Yale UniversityBurleigh University of LeicesterCaraveo Space Telescope Science InstituteDe Marchi Istituto di Fisica Cosmica del CNR CTA INCORPORATEDDreizlerFosterHeap University of California, Santa Cruz XRA Astronomy GroupHeydari-Malayeri Istituto di Fisica Cosmica del CNR Space Telescope Science InstituteHolbergHumphreys Universität Erlanger-Nüernberg Observatoire de ParisJeffery Naval Research LaboratoryJordan Winds of massive stars in nearby galaxies: NGC6822 Kepler NASA Goddard Space Flight Center The B/UV Colors of Geminga Suggest Spectral Feature on Hot Continuum. Kingsburgh University of Arizona University of MinnesotaKoester The Wind And Photosphere of the Unique DO White Dwarf RE J0503-289 Lallement Blue Straggler Stars, Stellar Collisions and the Fate of Globular Clusters A Detailed Study of the Blue Stragglers in Core M3 University of St. AndrewsLeitherer Snapshot Survey of Proto-planetary Nebulae and AGB stars Inst. fuer Astron. und Astrophysik der Universitaet Kiel Distance, Proper Motion and Colors of the Vela Pulsar. Lennon The Blue Stragglers in the Core of NGC 6397 Universidad Nacional Autonoma de Mexico Universidade Federal do Rio Grande SulLundgren Determining the Morphology of Intense Magnetic Field in Hot DA White Dwarf RE J0317-853 Institut fuer Astronomie und Astrophysik The origin of the peculiar hybrid PG 1159 stars Service d’Aeronomie du CNRS UV-Spectroscopy of a Peculiar Highly Magnetic White Dwarf How Did Stars Evolve in the Early Universe? , The Role of Metallicity Space Telescope Science Institute White Dwarf Companions to Binary Neutron Stars: Astrometric Frame Ties Universitaets-Sternwarte Muenchen Tight clusters of newly born massive stars in compact \h2 regions the Magellanic Clouds Naval Research Laboratory UV and Optical Spectroscopy of DR 1, the WO3 Star in IC 1613 its Surrounding Nebula, S3 First Ultraviolet Asteroseismology of a Pulsating DB White Dwarf High Resolution Imaging of Unstable Massive Stars at the Top HR Diagram Testing the Theory of Radiative Levitation in DA White Dwarfs Hydrogen and metal abundances in the cool helium-rich white dwarf Ross640 A bolometric light curve for pulsating helium star LSS3184 Lyman-Alpha Line Center Continuum as a Diagnostic of the Winds Bright A Stars Ultra-High Precision Monitoring of Photospheres and Winds Hot Stars The wind momentum-luminosity relationship for LMC A- and B-supergiants Evolution of Binary Neutron Stars and Their White Dwarf Companions: Part 2

HOT STARS

17 STSpace ScI NewsletterTelescope Science • Observers Institute & Proposers • Newsletter

Approved Observing Programs for Cycle 6 Continued MassaMcCarthyMeixnerMignaniMoffatNapiwotzki Applied Research Corporation California Institute of TechnologyNotaPavlov University of Illinois, Urbana-ChampaignPena Istituto di Fisica Cosmica del CNRPeters Universitaet Erlangen-Nuernberg Universite de MontrealProffittProvencalProvencal Space Telescope Science Institute Pennsylvania State UniversityRothschildSchulte-Ladbeck Instituto de Astronomia University of Southern CaliforniaShara Imaging Reflection Nebulosity in Three Post-AGB Objects WLR Distances from Accurate Multi-Color WFPC2 Photometry of A & B Supergiants in M31 and M33 Computer Sciences Corporation University of Delawarevan Kerkwijk The Winds of Main Sequence B Stars in NGC 6231: Evidence for Shocks Weak Winds. University of Delaware University of PittsburghVidal-Madjar University of California, San Diego Search for the Optical Counterpart of PSR1055-52. WalbornWalter The photospheric iron abundance of UV bright stars in globular clusters Werner California Institute of Technology Space Telescope Science InstituteWerner Institut d’Astrophysique de Paris Circumstellar Nebulae as Fossil Records of the Mass Loss History in Luminous Blue Variables Wesemael Fine Structure in Ejection Nebulae Around Population I and II Wolf-Rayet Stars White Space Telescope Science Institute UV-Optical Spectra of Middle-Aged Pulsars: Thermal vs. Nonthermal Winget Heavy Element Abundances in AV 304, a B0.5 Main Sequence Star the Small Magellanic Cloud State University of New YorkWinkler Universitaet Potsdam Boron Isotope Ratios in Early B Stars from III Universitaet Potsdam Universite de Montreal Spectrophotometry of the WR Central Star LMC-PN N66 A Counterpart Search for SGR 0526-66 Carbon and Convective Mixing in Hot Helium Rich White Dwarf Stars Space Telescope Science Institute Imaging Circumstellar Nebulae around Luminous Blue Variables in the Magellanic Clouds Hydrogen, Interstellar Accretion, and Hot Helium Rich White Dwarfs University of Texas Fundamental properties of the pulsar/white-dwarf binary PSR B1855+09 A Snapshot Survey for Companions and Clusters around Wolf-Rayet Stars Middlebury College Far UV emission spectrum and stellar wind of Sirius A Spatially Resolved Spectroscopy of New Compact Multiple Systems in the LMC Parallax, Proper Motion, and Spectral Energy Distribution of an Isolated Old Neutron Star The P Cygni Nebula UV spectroscopy of a DAO white dwarf showing signatures an extremely hot wind Ultraviolet Spectroscopy of Hot DB White Dwarfs Metal diffusion and radiative levitation in hot helium-rich white dwarfs A Unique Test of Asteroseismology: the DBV GD358 An Optical Counterpart to the X-Ray Point Source in Puppis A Supernova Remnant? AllerBalickBennettBladesBorkowskiBujarrabalCardelli University of California, Los Angeles University of WashingtonCardelli University of ColoradoChu Space Telescope Science Institute North Carolina State UniversityChu Centro Astronomico de YebesDavidsonDopita Villanova UniversityDrilling Villanova UniversityFesenFilippenko University of Illinois University of MinnesotaFilippenko Spectroscopic diagnostics for gaseous nebulae and symbiotic stars University of IllinoisFitzpatrick Mt. Stromlo and Siding Spring ObservatoriesGarnett Louisiana State UniversityGry Physical conditions near high galactic latitude molecular clouds University of California, Berkeley Dartmouth College Evolution and excitation of bipolar nebulae Hamilton A Search for Jets in Planetary Nebulae University of California, BerkeleyHester A NLTE Analysis of the UV Spectrum HD 44179 Shocks in protoplanetary nebulae Princeton University ObservatoryHesterJacoby University of Minnesota Post Asymptotic Giant Branch Evolution in the Magellanic Clouds JILA Laboratoire d’Astronomie Spatiale Interstellar Cadmium: Probing Galactic Chemical Evolution Arizona State University Interstellar Carbon Abundance in Low Density Gas Arizona State University Probing the equatorial ejecta of Eta Carinae National Optical Astronomy Observatories High Resolution Imaging of Bubble and Superbubbles in HII Regions An Archival Study of the Environments Supernovae The Luminous Giant HII Regions in M101 A study of circumstellar material formed in a hydrogen-deficient environment Interaction of Supernovae with Circumstellar Material Observations of Interstellar Clouds in the Galactic Halo A WFPC2 Search for Surviving Binary Companions in SN Ia Remnants Physics of diffuse clouds in the Local Bubble , Part I : CMa tunnel Spectroscopy and Imaging of a New Globular Cluster Planetary Nebula HST Imaging and Spectroscopy of the Peculiar LMC H II Region N44C Continuation of Temporal Monitoring the Crab Synchrotron Nebula Ionization Structure, Photoevaporation, and Star Formation in M17 UV Imaging of S Andromedae (SN 1885) in M31

ISM

18 February 1996

Approved Observing Programs for Cycle 6 Continued JenkinsKirshnerKulkarniKwokLinskyLopez Princeton University ObservatoryLundqvist Harvard College ObservatoryMacAlpine California Institute of TechnologyMeyerMeyer Department of Physics and Astronomy JILA/University of ColoradoNeufeld Universidad Nacional Autonoma de Mexico Stockholm ObservatoryO’Brien University of MichiganRocheRubin Northwestern UniversitySahai Northwestern UniversitySahai Thermal Pressures of the Local Interstellar Medium Johns Hopkins UniversitySavage Liverpool John Moores UniversitySchmidt SINS: Supernova Intensive Study - Cycle 6 The Enigmatic Soft Gamma-Ray Repeaters Imaging of Proto-Planetary Nebulae University of Oxford High-resolution imagery of the Bipolar, Rotating, Episodic Jet in Planetary Nebula PK 112-00 1 Sembach NASA Ames Research CenterSembach Jet Propulsion Laboratory/ CaltechShara Jet Propulsion Laboratory/ CaltechSmith The ISM Toward Nearby High-Velocity Stars: Accurate H Columns, D/H, and Walls University of Wisconsin-MadisonSofia Mount Stromlo and Siding Spring Observatories Massachusetts Institute of TechnologyTrammell The Missing Mass of the Crab Nebula Massachusetts Institute of TechnologyTrammell A Test For Products of Oxygen Burning in the Crab Nebula Vidal-Madjar Space Telescope Science InstituteWakker Small-Scale ISM Structure: The Remarkable Sightline Toward Mu Cru Resolving the nature of nova shells NASA Goddard Space Flight CenterWalsh The Abundance of Interstellar Nitrogen Search for Interstellar Water in Translucent Molecular Clouds University of ChicagoWalsh SN 1991T: Reflections of Past Glory National Research Council University of ChicagoYang Institut d’Astrophysique de Paris The Small Scale Structure and Symmetries in Proto-Planetary Young Planetary Nebulae Planetary Nebulae With Supporting Infrared Data A SNAPshot Emission-line Imaging Survey of Very Low Excitation Planetary Nebulae High Resolution Imaging of Young Stellar Objects in Serpens Ionization of C IV High Velocity Clouds in the Galactic Halo HST and ORFEUS-II Observations of Highly Ionized Galactic Halo Gas Towards ESO 141-55 University of Wisconsin High Velocity Thermal Shock Instabilities in the Vela Supernova Remnant Space Telescope European Coordinating Facility Space Telescope European Coordinating Facility University of Illinois High-resolution imagery of the next bright Galactic nova Search for Interstellar CH_2 in the Spectrum of HD 154368 High spatial resolution polarization mapping of the nebula around Eta Carinae Deuterium in the local interstellar medium towards hot stars Parallel high resolution imaging of diffuse objects in the Magellanic Clouds On the Nature of Dust Mineralogy The Origin of Shock Emission in Proto-Planetary Nebulae The Early Onset of Asymmetric Outflow During the Planetary Nebula Formation Process The metallicity of high-velocity cloud complex C The Structuring of the ISM by Massive Stars in NGC 604 AravBechtoldBowenFoltzGreenHamannKhersonsky University of Arizona CaltechLanzetta Royal Observatory EdinburghLanzettaLanzetta Multiple Mirror Observatory Smithsonian Astrophysical ObservatoryLu University of California, San Diego Dept. of Physics & AstronomyMathurPetitjean State University of New York at Stony BrookRao State University of New York at Stony BrookRauch State University of New York at Stony BrookReimersReimers Smithsonian Astrophysical Observatory CaltechReimers Institut d’Astrophysique de Paris PG 1416-129: The Only X-ray Bright BAL QSO, or the Missing Link? Steidel M33: An archetypal QSO absorption line galaxy? A Group or Cluster of Ly-alpha-Absorbing Galaxies at z ~ 0.26 The Connection between the Ly-Alpha Forest at z=0.5 and Large Scale Structures in Galaxy Distribution University of Pittsburgh Associated (\zaz ) Absorption Lines in QSOs Carnegie Observatories Damped Lyman-alpha Absorption Lines from Moderate-Redshift Galaxies Hamburger Sternwarte The Distribution and Evolution of Lyman-Alpha Forest Cloud Sizes High-Resolution Images of QSO Lyman-alpha Absorbing Galaxies The Statistical Properties of the LyAlpha Forest in Redshift Interval z=0 - 4 Hamburger Sternwarte Hamburger Sternwarte FOC Spectroscopy of BALQSOs California Institute of Technology Absorbing Outflows in Quasars and AGN FOS Observations of QSO Pairs An Expanded Survey for Study of the LyAlpha Line in QSO MgII Absorption Systems Low Redshift Lyman Alpha Forest Clouds: Their Kinematics and Relation to Galaxies Ly-alpha forest clouds at intermediate redshifts z=0.8 to 1.4 in the new double QSO HS 1216+5032 WFPC2 Imaging of Intermediate Redshift Absorption-Selected Galaxies The Relationship Between Lyman-Alpha Clouds and Galaxies at z<0.3 Ne absorption lines in the spectrum of QSO HS 1700+6416 Spectroscopy of two further UV bright high-redshift quasars

QSO Abs Lines

19 STSpace ScI NewsletterTelescope Science • Observers Institute & Proposers • Newsletter

Approved Observing Programs for Cycle 6 Continued StockeStockeTurnshekTurnshekTytlerWebb University of Colorado, Boulder University of Colorado, Boulder University of Pittsburgh University of Pittsburgh University of California, San Diego University of New South Wales A Metal Absorption Line System in the Local Supercluster ? Origin and Physical Conditions in the Local Ly-Alpha Forest Ssnpshot search for High Redshift QSOs with Far-UV Flux The BAL Region Covering Factor in a Sample of IRAS-Selected QSOs The Origin of the Polarization in Gravitationally Lensed “Cloverleaf” BAL QSO H1413+1143 The Gaseous Extent of Galaxies: How Far is Too Far? BaggettBennettBessellBomansBragagliaBrodie Space Telescope Science InstituteBuonanno Lawrence Livermore National LaboratoryBurstein Mt. Stromlo and Siding Spring ObservatoriesChaboyer University of Illinois, Astronomy Department Osservatorio Astronomico BolognaCoteDa Costa Observatory of Rome Lick Observatory, University of CaliforniaDeliyannisDrissen Arizona State University Canadian Institute for Theoretical AstrophysicsFergusonFerguson Measuring Proper Motions of Galactic Microlenses UV-Visible Observations of Hot Stars in Young Magellanic Cloud Star Clusters NGC 3664 - a case study of shock-induced propagation star formation Mt Stromlo and Siding Spring ObservatoriesFerraro The Star Formation History of the Magellanic Clouds Dominion Astrophysical Observatory Yale UniversityFulltonFusi Pecci Universite Laval Johns Hopkins UniversityGebhardt White Dwarf Distance and Precision Age for Globular Clusters Extragalactic Globular Cluster Systems The Formation of the Inner Galactic Halo and Thick Disk Space Telescope Science InstituteGeislerGeisler Osservatorio AstronomicoGregg Osservatorio Astronomico Space Telescope Science Institute The Horizontal Branches of the M31 Dwarf Spheroidal Companions And II and III Hesser University of MichiganHibbard The second-parameter effect and the formation history of Milky Way Galaxy Hodge A Search for Intermediate-Age Globular Clusters in the Nearby Giant Elliptical Galaxy NGC 5128 UV Spectra of Representative Stellar Populations Age > 2 GYr Kitt Peak National ObservatoryHuizinga Kitt Peak National ObservatoryHunter Lawrence Livermore National LaboratoryIbata Dominion Astrophysical ObservatoryJablonka Dwarf Elliptical Galaxy Snapshot Survey University of HawaiiJablonka University of Washington Revealing the Stellar Population(s) of Andromeda IV King European Southern Observatory Boron in Halo Giants : A Solution to the D+3He Crisis Big Bang Nucleosynthesis? MacKenty Ages of Extreme-metallicity Inner Galaxy Globular Clusters Lowell Observatory Deep Imagery of NGC 3603: Low-Mass Star Formation in the Closest Starburst Region Massey The Origin and Nature of UV Bright stars in Globular Clusters II Meylan Observatoire de Paris, Section Meudon Department of Astronomy Large Population Studies of Globular Clusters Mighell Observatoire de Paris, Section Meudon The Stellar Population of M32: A Dual Approach The Globular Cluster Systems of the Dwarf Elliptical Galaxies NGC 185 and 205 Mighell Photometry for M28 and NGC 5286 Space Telescope Science Institute The Globular Cluster Systems of Distant Giant Ellipticals Miller University of California The Formation of the Galaxy: Completing Age Profile Outer Halo Globular Clusters Morrison National Optical Astronomy ObservatoriesOestlin European Southern ObservatoryOlszewski Columbia UniversityParesce Globular Cluster Systems along the Hubble Sequence The UV-upturn of super-metal-rich globular clusters Columbia UniversityPeterson The Color-Magnitude Diagram of the Super-Metal-Rich Globular Cluster G198 in M31 The Oldest Star Clusters of Local Group Irregular Galaxies Imaging of Two Dwarf Galaxies in Tidal Tails Space Telescope Science Institute Case Western Reserve University Astronomiska Observatoriet Steward Observatory Star Formation in the Prototype Super Cluster R136 Photometry of the globular cluster system Sagittarius dwarf galaxy The Physics of Nearby Blue Irregular Starbursts European Southern Observatory Structure in the Superstar Clusters NGC 1569 Astrophysical Advances Precise Astrometry in the Core of Globular Cluster 47 Tuc: A Complete Census High-Velocity Stars The Very-Low-Mass Star Content of the Globular Cluster NGC 6397 The Stellar Populations in the Pheonix and LGS 3 Dwarf Galaxies Halos of Nearby Edge-on Spirals The Star Formation History of the Sagittarius Dwarf Spheroidal Galaxy A Stellar Population Survey of the Nuclear Region M33 Multiwavelength Imaging of two Luminous Blue Compact Galaxies Searching for Low Mass Stars: the Function at H Burning Limit The Gaseous Environment of the Ursa Minor Dwarf Spheroidal Galaxy Ultraviolet Spectral Templates from the Metal-Rich Open Cluster NGC 6791

Stellar Populations

20 February 1996

Approved Observing Programs for Cycle 6 Continued RenziniRichSchombertSchulte-LadbeckSmithSmith European Southern Observatory University of PittsburghStecher NASA Headquartersvon Hippel Columbia UniversityWalkerWalterbos UCO/Lick ObservatoryWorthey UCO/Lick Observatory NASA Goddard Space Flight Center University of Wisconsin Cerro Tololo Inter-American Observatory New Mexico State University University of Michigan A Very Deep Luminosity Function for the Galactic Bulge Comparing the Stellar Populations of Isolated Dwarf Irregular Galaxies — UGC 6456 and Beyond WFPC2 Imaging of Dwarf Spirals The Pattern of Massive Star Formation in Nearby Irregular and Amorphous Galaxies Deep V,I Photometry for 20 M31 Globular Clusters Photometry of the Oldest Field Populations in Magellanic Clouds The Main Sequence Luminosity Functions of NGC 5466 and Palomar 5 The Early Evolution of Local Group Dwarf Irregular Galaxies Calibration of Stellar Evolutionary Ages and Variations in the IMF The Stellar Populations Inside Expanding HI Shells in Galaxies Stellar Ages in M 32: Exposing the Conspiracy A’HearnA’HearnBallesterBeebeBeebeBen Jaffel University of MarylandBertaux University of MarylandBosh University of MichiganBrown New Mexico State UniversityClarke New Mexico State University Institut d’Astrophysique de ParisCochranCombi Service d’Aeronomie du CNRSDenkFeldman Lowell Observatory CaltechFitzsimmons University of MichiganFrench The University of Texas at AustinGerard University of MichiganGerardGladstone Queen’s University of Belfast The Origin of C_2 in Comets Deutsche Forschungsanstalt fuer Luft- und Raumfahrt The Johns Hopkins UniversityGoguen 55P/Tempel-Tuttle and the Leonid Meteors Global and Temporal Coverage of Atmospheric Regions Selected for Intense Galileo Observations The abundance and distribution of deuterium on Mars, Jupiter, Saturn HST observations of Io’s atmosphere coordinated with GALILEO Hall Wellesley College Rapid Response to Anomalous Activity in Jupiter’s Atmosphere Hall Universite de Liege Deuterium Abundances in the Upper Atmosphere of Venus Hammel Disk-resolved Spectrophotometry of the Dark Side Iapetus Universite de Liege Southwest Research InstituteJamesKrasnopolsky Jet Propulsion Laboratory A Search of the HST Archive for Intermediate-Sized Comets: Linking Ground-Based and Observations LamyLamy The Johns Hopkins University Does Pluto Have a Haze Layer? Levison Massachusetts Institute of Technology The Johns Hopkins University HST Far-UV Imaging and Spectra of Jupiter’s Aurora Coordinated with GALILEO National Research Council/Goddard Space Flight CenterMcGrath University of Toledo A Campaign to Determine the CO and \cotwo\ Abundances in Cometary Nuclei A search for outgassing from Kuiper Belt Objects Meech A Comprehensive Study of the H Ly—Alpha Line Profile and Water Photochemistry in a TOO Comet Na Determining the Crustal Composition of Io through Atmospheric Spectroscopy Noll Laboratoire d’Astronomie Spatiale The second measurement of D/H in Mars’ upper atmosphere Noll Laboratoire d’Astronomie Spatiale Southwest Research InstitutePrange Space Telescope Science Institute Archival Studies of Auroral Haze on Jupiter Rages Saturn’s Rings Institute for AstronomyRoush The link between the UV Saturnian aurora and polar stratospheric haze The Atmosphere of Uranus: Vertical Aerosol Structure and Horizontal Inhomogeneity Seidelmann Global Mapping of the Opposition Surge on Galilean Satellites Observation of short timescale variability the Jovian UV aurora University of Colorado Transit Observations of Io’s Atmosphere Space Telescope Science Institute Far-UV Airglow and Albedo Observations of Europa Ganymede Space Telescope Science Institute Institut d’Astrophysique Spatiale Space Physics Research Institute United States Naval Observatory The nucleus of comet 22P/Kopff and its dust gas emissions San Francisco State University The nucleus of comet 46P/Wirtanen Synoptic Monitoring of Seasonal Phenomena on Mars Io’s SO2 Atmosphere: Patchy or Not? An Ultra-Deep Study of Comets in the Kuiper Belt Ultraviolet Spectra of Saturn’s Satellites: Ion Modification Surface Ice Distant Comet Nucleus Sizes The Ultraviolet Spectrum of Callisto Correlated study of the outer magnetosphere with FOC, GHRS and Galileo Jovian Global Photometry During the Galileo Epoch Multispectral observation of Venus atmosphere: Composition, Circulation and Variability Recovery of Inner Satellites Neptune Ultraviolet Spectra of Uranian Satellites

Solar System

21 SpaceST ScI NewsletterTelescope Science • Observers Institute & Proposers • Newsletter

Approved Observing Programs for Cycle 6 Continued 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 involve- ment in the Space Telescope Project. Robert Fosbury (Editor) Space Telescope — European Coordinating Facility Karl Schwarzschild Str. 2 D-85748 Garching bei München Federal Republic of Germany E-Mail: [email protected]

Live from HST March 14 April 23

NASA Select TV PBS See details on the next page ShemanskySmithSofiaSpencerSromovsky University of Southern CaliforniaSromovskyStern Lunar and Planetary LaboratoryStorrsWeaver National Research Council Lowell Observatory University of Wisconsin-MadisonWeaver University of Wisconsin-MadisonYoungZellnerZellner Southwest Research Institute Space Telescope Science InstituteZellner Applied Research Corporation Morphology of OH in the Saturn Magnetsophere Applied Research Corporation NASA Ames Research Center Georgia Southern University WFPC2 Support for the Mars Pathfinder Mission Georgia Southern University Archive Research on Neptune’s Atmospheric Dynamics Georgia Southern University Atmospheric Dynamics and Cloud Structure on Neptune Ozone Abundance in Mars Atmosphere Temporal Variability of Io’s Surface and Plumes An Imaging Study of Asteroids A Targeted HST Search for New Species in the Lunar Atmosphere Systematic Investigation of C/1995 O1 (Hale-Bopp) HST Investigation of a Bright, New Comet Spatially-resolved mapping of Titan’s atmosphere at several interesting altitudes Vesta at Perihelion Spectrophotometry of Inner Satellites Uranus Spectrophotometry of Inner Jovian Satellites

22 February 1996

Office of Public Outreach educational activities and public for scientists to share the excitement of by Carol Christian information programs. Please send space astronomy research with them to [email protected]. students and the public. Today, the The Office of Public Outreach program is administered by the Space (OPO) has had an interesting year with Telescope Science Institute on behalf a number of changes in personnel, of NASA. The IDEA program various upheavals in NASA structure Initiative to Develop encourages research astronomers to and management, and hurdles in Education through use their talents and enthusiasm to securing our budget. Nevertheless Astronomy (IDEA) undertake projects that promote greater OPO was able to provide to the public mathematical, technological, and glimpses of some remarkable research On December 18th the Office of Institute News scientific literacy. It emphasizes results and spectacular Public Outreach hosted a proposal n and O collaboration between partners in the io ut data. In the latter review for the Initiative to Develop at re c a professional education community, as u c part of the year, Education through Astronomy (IDEA) d h well as links to active learning and E in between the grants program. Review participants • education reform. Funding is available • release of included astronomers, educators,

G up to $20,000. Funds may be used, for

n e results such as science supervisors from local school t o example, to support salary, travel, t i i t the brown districts, planetaria/science museum n a materials and stipends. Funding for g c u dwarf, compan- staff, NASA education personnel and In d equipment is discouraged but allow- v E ion of Gliese 229, representatives from STScI. o e able in exceptional circumstances. lve nc showcasing the Eagle In total, 66 IDEA proposals were d in Scie To receive the IDEA announcement Nebula (M16) data and reviewed requesting $716,000. Among or for more information on how to scientific research and preparing for the many excellent projects that were apply for a grant next year, please send the Hubble Deep Field observation, selected, we can mention: email to [email protected] or call OPO has taken some time for a • A program for middle school students Carole Rest at (410) 338-4590. pragmatic look at our activities and near Yerkes Observatory to experi- A copy of the 1995 announcement is resources. We have worked on ence telescope building, astrophotog- also available at URL: http:// documenting a mission statement for raphy, and developing original www.stsci.edu/EPA/education.html. the Office and a set of albeit ambitious research using the 10-inch and 24- goals. We believe we have formulated inch reflecting telescopes at Yerkes; a sensible (but exciting!) core program to better serve the public, but also to • The continuation of a Washington Live from HST support the astrophysics community in DC-based pilot program developing Remember your curiosity as a child articulating the value and process of video-based curriculum in As- of the sky and all the wonders it holds? our scientific research. tronomy and Space Science to be Now you can share in the same To define the OPO Core Program, used as a supplement to general curiosity of children from around the we have examined strategies for science courses at the junior high world through the “Live From HST” improving the delivery of materials level; project. and services and applying our talents • An interactive, WWW-based “Live From HST” is a PASSPORT and resources to broker the expertise of astronomy supplement for high to KNOWLEDGE integrated multime- the astrophysics community and HST school physics curricula in the Iowa dia educational project aimed primarily Program to the public. The changes we City area; at the middle school grades. The have formulated include enhancement project involves live and videotaped to the OPO Web resources coordinated • A teacher workshop for schools with images, printed materials suggesting with overall improvements in Space high hispanic enrollment in the Las hands-on in-class activities, and on- Telescope Electronic Information Cruces, NM, Independent School line computer activities. Systems (STEIS). As our changes take District; By using the Internet, students form, they will be documented at • The development of a system-wide participated in an electronic “Great http://www.stsci.edu/. Soon you will approach for teaching hands-on/ Planet Debate” with Planet Advocates be invited to open our electronic “file minds-on astronomy concepts to over Reta Beebe (New Mexico State cabinet” to access images, background 15,000 K-6 students in the Prince University) for Jupiter, Carolyn Porco information, scientists’ fact sheets and George’s County, MD, Public (University of Arizona) for Uranus, educational materials. OPO welcomes Schools; Heidi Hammel (MIT) for Neptune, and your creative commentary on our plans Marc Buie (Lowell Observatory) for and our resources, and invites the The IDEA program was developed Pluto. The debate resulted in the astrophysics community to keep us in 1991 by the NASA Astrophysics decision that the student Co-Investiga- informed of your new research results, Division to create more opportunities tors will use two of their HST orbits to 23 SpaceST ScI NewsletterTelescope Science • Institute Institute News • Newsletter

study Neptune and one to study Pluto. Christian (STScI) presented innovative Epoch Southern (SES) Survey (Lasker Reta Beebe "loaned" one of her GO uses of the World Wide Web for public and Cannon 1990), to provide a orbits so Jupiter could also be and educational outreach. comparable modern epoch survey in included. Students will be able to The session finale was a hands-on the southern hemisphere. Major follow the progress of their upcoming demonstration presented by Kim features of this program are digitiza- observations via the Internet. Zeidler called “Planet Picking.” Kim, a tion based on scans of the original STScI astronomers and staff are K-6 science coordinator now interning plates, supplemented by copy plates of supporting the on-line component of for a year in the STScI Outreach the PPARC/SERC Equatorial Red “Live From HST” by providing group, conducted the activity devel- survey, processing of all fields in all biographies and journals describing oped by the Pacific Science Center passbands (3576 plates total), the use what it’s like to work on the Earth’s which is designed to allow students to of a 1” sampling interval, and most powerful astronomical tool. They use their own deductive ability in distribution of the full-plate pixel data will also participate in an electronic sorting postcards featuring planets and to the community. question and answer session with planetary features to help them learn In support of this, the microdensito- students curious to learn more about how a scientist works. Extra materials meters used for the original scanning their work and careers. were distributed to session participants for the Guide Star Catalog (Lasker et “Live From HST: Making YOUR for use in their own classroom visits. al. 1990) were rebuilt as laser- Observations” will air on PBS and Kim also prepared a practical guide illuminated 5-channel systems capable NASA Select TV live from STScI, for scientists visiting a classroom. It of scanning rates well in excess of Goddard Space Flight Center and ST- includes facts about students by grade, 1000 plates per year. The metrology is ECF in Garching (Germany) on March information on the constructivist stable to 0.5m, and the densitometry 14, 1996. education model that predominates extends three density units above the “Live From HST: Announcing today’s classrooms, and simple sky (note that typical sky values on the YOUR Results” will air live from guidelines to help a scientist prepare original plates are in the range 1.5- STScI on April 23, 1996, 3 days after for a visit and make the most of the 2.5). The scans are of dimension National Astronomy Day and during time spent with students. If you are 23040x23040 which corresponds to NSF’s National Science and Technol- interested in receiving a copy, contact 1.1 Gbyte per plate (for a 2.8 Tbyte ogy Week. [email protected]. survey total). For more information, access the At the ST ScI, the raw scans are project’s Home Page at: http:// archived on 6 Gbyte WORMs (six quest.arc.nasa.gov/livefrom/hst.html The Digitized Sky scans per disc). However, with existing technology, this data set is too large for Survey II - simple community distribution; and Preliminary Data Education Session some data compression is essential. A Availability very similar problem with earlier ST at HST Paris Meeting by Barry Lasker and Brian McLean ScI scans of the POSS-I (E) and the SERC J surveys led to the development More than thirty meeting attendees The Catalogs and Surveys Branch is of the Digitized Sky Survey - I, based braved uncertain homeward transporta- pleased to announce that a preliminary on 10X compression with loss, using tion to remain in Paris for a special version of the second epoch Digitized the H-transform (White, et al., 1992), Saturday session on education. Sky Survey based on scans of the SES and occupying 102 printed CD ROMs. “It was the best session of the meeting and POSS-II surveys is now available The same approach and the same for me,” quipped Mike Disney from on the ST ScI WWW server. compression factor were adopted for the University of Wales, College of As part of our ongoing program to the DSS-II. A basic difference, Cardiff. support HST operations and to provide however, is that the POSS-II and SES The classroom-sized group made it the underlying material for a future surveys are still in progress. Thus the easy for Doug Duncan (Adler second generation Guide Star Catalog data must be regarded as preliminary Planetarium), to pass out diffraction (GSC-II), CASB is in the process of in that certain plates may be retaken or gratings as an example of a hands-on scanning the latest sky survey Schmidt rescanned as resources permit near the activity he uses to help visitors plates in both the northern and end of the project. This alone pre- appreciate spectroscopy. He gave many southern hemispheres. Accordingly, in cludes the initial investment required illustrations of what astronomers can 1991 Caltech and the ST ScI com- for a massive printing on CD ROMs. do to collaborate with planetaria. pleted a Memorandum of Understand- However, the general community Barrie Jones of the United ing which defined The Palomar - ST interest in the data makes it appropriate Kingdom’s Open University brought ScI Digitized Sky Survey. Similarly, that we create a preliminary distribu- video clips to show how he teaches the Anglo-Australian Observatory and tion mechanism for immediate use, “Astronomer at a Distance.” Carol the ST ScI are obtaining a new Second 24 even while still maintaining our February 1996

during the academic year commencing Table 1 - DSS-II Data Summary Status information as of November 1995 in September 1996 will be given to applications received by February 2, North POSS-II South SES+ER 1996. Sabbatical visitors for the academic year 1995-95 include Band BJ RIR Plate Emulsion IIIa-J IIIa-F IV-N IIIa-F Massimo Della Valle (University of Telescope Filter GG385 RG610 RG9 RG610 Padua), Henny Lamers (University of Mean Wavelength 4800 6500 8500 6500 Utrecht), Ronald Webbink (University Limiting Mag. 22.5 20.8 19.5 20.8 of Illinois) and Tom Wilson (Max- Plate Status 82% 83% 55% >90% Scan Status 43% 43% 15% 36% Planck_Institute für Radioastronomie). CD ROM Status — 15% — 15% ESA Fellowships at STScI committment to make a printed CD REFERENCES ROM version after the completion of Lasker, B.M., et al., 1990, AJ, 1019. Astronomers of ESA member Lasker, B.M. & Cannon, R. 1990 the observing and scanning. countries are reminded of the possibil- Digital Sky Surveys, eds. C.Jaschek The technology adopted for the ity of coming to do research at STScI preliminary distribution is write-once and H.T.MacGillivray. Bull.Centre de Donnees Stellaires No.37,p.13 as an ESA Fellow. Prospective CD ROMs. With 10X compression, six fellowship candidates should aim to Reid, I.N., et al. 1991, PASP, 103, 661. plates fit on a single volume (but fewer work with a particular member or where severely crowded fields make White, R.L., Postman, M., & Lattanzi, members of the staff at STScI, and for 10X too large a compression factor). M.G. 1992 Digitised Optical Sky this reason, applications must be As a preliminary distribution of the Surveys, eds. H.T. MacGillivray and accompanied by a supporting letter E.B. Thompson (Dordrecht: Kluwer), DSS-II data, such discs are now being from STScI. p. 167. prepared and mounted in a jukebox Details of the interests of staff accessible at the ST ScI WWW server. members at STScI can be obtained The new scans may be accessed at from Dr. N. Panagia. Details of the URL http://stdata.stsci.edu/dss/ Sabbatical Visitors fellowships and applications proce- dss_form.html at STScI dures can be obtained from the Because of the limited throughput of In order to promote exchange of EDUCATION OFFICE,ESA,8-10 rue write-once technology, only a few ideas and collaborations in HST- Mario Nikis, 75738 PARIS 15, copies of each volume are being made. related science, STScI expects to FRANCE. One is located at ESO while the provide limited funds to support Completed application forms must disposition of the others remain to be visiting scientists who wish to spend be submitted through the appropriate negotiated in consideration for help in extended periods of time (typically national authority, and should reach relieving resource-based risks to the three to six months) doing research at ESA no later than 31 March for project. STScI. Typically the visitor is on consideration in May, and no later than The highest priority for the sabbatical leave from his or her home 30 September for consideration in continued development of this institution. In general, these visitors November. community data server is to complete will have the status of STScI employ- A copy of the completed application coverage in the R-band; then, as ees and have access to the facilities should be sent to the Chairman of the resources permit, the POSS-II J and available to staff members, including Postdoc Selection Committee, Dr. M. IV-N plates will be added. As of this access to NCSA facilities. Fall, at STScI, 3700 San Martin Drive, writing, sky coverage is about 15% and Established scientists who might be Baltimore, MD 21218, USA. increasing by about 5% per month. interested in such a visit should send a Selected Fellows must negotiate the letter specifying the suggested period commencement dates of their ESA ACKNOWLEDGEMENTS Fellowships at STScI with the In addition to the strong institutional for the visit and any other relevant Research Programs Office (c/o Ron support provided for the POSS—II by details to the Visiting Scientist Caltech and its benefactors (cf., Reid Program, c/o Nino Panagia (e-mail Allen) at least 2 months before their 1991 for a full list) we are grateful to [email protected]) at STScI. prospective starting times. the Anglo Australian Observatory Applicants should also include a The interests and activities of staff which operates the UK Schmidt, the statement of research plans and a copy members at STScI can best be National Aeronautics and Space of their curriculum vitae. Applications assessed by reading the annual report Administration and to the European of the Institute which is to be found in Southern Observatory for support of can be submitted at any time of the the Bulletin of the American Astro- the digital aspects of the program. year, but full consideration for visits planned during the summer of 1996 or nomical Society (1995) Vol. 27, p. 586. 25 SpaceST ScI NewsletterTelescope Science • Institute Institute News • Newsletter

Currently there are two ESA Fellows in residence at STScI: Salvatore Scuderi, whose interests are stellar winds and supernovae, and Nicola Caon, who is studying elliptical galaxies.

Colloquia, Symposia, and Workshops by Mario Livio “The Extragalactic Distance Scale,” this year’s STScI May Symposium will take place on May 7-10. A variety of methods, as well as the most recent results on the determination of the Hubble Constant will be presented and discussed. The deadline for registration is April 1, 1996. People interested in participating should contact Cheryl Schmidt at STScI by mail, e-mail ([email protected]) or phone (410- 338-4404). The registration fee is $140. More information can be obtained at http://www.stsci.edu/ftp/ meetings/meetings.html. A number of workshops are being planned:(i) Evolution of Low Lumi- fractions of the entire sky. Parallel X- as a definition of the technical and nosity Galaxies, March 25-27; (ii) ray and radio surveys over the same schedule requirements for future Multi-Wavelength Digital Sky areas will produce astronomical image surveys. The meeting will review the Surveys, August 26-30, and (iii)The and spectroscopic databases of multitude of surveys by spectral Astrophysics that Can be Learned from unprecedented size and quality. region, and then will address the Planet Searches, at a date still to be Together, these surveys make it opportunities for innovative research determined. possible to pursue scientific programs resulting from the combination of that could not be supported by any surveys. Scientific issues and opportu- single one. The combined data sets nities that are common to most surveys IAU Symposium No.179 will provide significant new constraints will be considered, as well as problems New Horizons from Multi- on star formation, stellar dynamics, related to data processing and Galactic structure, the evolution of archiving. The Symposium will occupy Wavelength Sky Surveys galaxies, and large scale structure, as a five-day interval, with 4.5 days of by Barry Lasker and Brian McLean well as new opportunities to identify formal discussions and one half-day The Space Telescope Science rare Galactic and cosmological objects. reserved for informal discussions and a Institute and The Johns Hopkins The focus of this meeting will be social-cultural event. The meeting University are pleased to announce that how surveys at different wavelengths format will consist primarily of invited they will be co-sponsoring IAU can be coordinated with each other, as reviews, but posters and a small Symposium 179 during the week of well as how strategies adopted for one number of selected contributed talks August 26-30th 1996. survey may be used to enhance the are welcome. Generous intervals will Large area sky surveys are now a scientific output of another. By be scheduled for discussions and for reality in the Radio, IR, Optical, UV, bringing together the experts represent- the poster papers. Additional informa- X-ray and Gamma-ray passbands. In ing the various surveys, spectral tion may be obtained by sending e- the next five years, new surveys using regions, and astrophysical disciplines, mail to the local organizing committee optical, UV, and IR mosaic cameras new opportunities will be identified at [email protected] or via the with high throughput digital detectors and explored. The result will be in a WWW at URL http://www- will expand the dynamic range and better understanding of the possibilities gsss.stsci.edu/iau_symp_179/ accuracy of photometry and astrometry for coordinating present surveys and announcement.html 9 26 for > 10 objects covering significant for combining data from them, as well February 1996

Recent ST ScI Preprints

967. “The Sub-Arcsecond Radio Structure in NGC 1068: I. 982. “Radiative Transfer in a Clumpy Universe: II. The Observations and Results,” J.F. Gallimore, S.A. Baum, C.P. Ultraviolet Extragalactic Background,” F. Haardt, P. Madau. O’Dea, A. Pedlar.

983. The H2O Megamasers in NGC 2639—Evidence for an 968. “Nuclear Rings in Active Galaxies,” T. Storchi-Bergmann, Accretion Disk in a Liner Nucleus,” A.S. Wilson, J.A. Braatz, A.S. Wilson, J.A. Baldwin. C. Henkel.

969. “Hubble Space Telescope Observations of Globular 984. “A ROSAT Search for Clusters around Three Powerful > > Clusters in M87 and an Estimate of H0,” B.C. Whitmore, W.B. Radio Galaxies at Redshifts 0.1 ~ z ~ 0.25,” C.P. O’Dea, D.M. Sparks, R.A. Lucas, F.D. Macchetto, J.A. Biretta. Worrall, S.A. Baum, C. Stanghellini.

970. “A Search for Far-UV Emission Lines from Diffuse Hot 985. “Bar Dissolution and Bulge Formation: An Example of Gas in the Halo of NGC 4631,” H.C. Ferguson, W. Van Dyke Secular Dynamical Evolution in Galaxies,” C.A. Norman, J.A. Dixon, A.F. Davidsen, R.-J. Dettmar. Sellwood, H. Hasan.

971. “The Origin of Cosmic Rays Above 1018.5 eV,” C.A. 986. “Intermediate Velocity Gas in the North Galactic Norman, D.B. Melrose, A. Achterberg. Hemishere: HI Studies,” K.D. Kuntz, L. Danly.

972. “The Unusual X-Ray Collision Morphology of NGC 4782/ 987. “The Hot Gaseous Halo of the Spiral Galaxy NHC 3628 in 4783 (3C 278),” L. Colina, K.D. Borne. the Leo Triplet,” M. Dahlem, T.M. Heckman, G. Fabbiano, M.D. Lehnert, D. Gilmore. 973. “An Emission-Line Imaging Survey of Early-Type Seyfert Galaxies—I. The Observations, J.S. Mulchaey, A.S. Wilson, Z. 988. “The Subarcsecond Radio Structure in NGC 1068: II. Tsvetanov. Implications for the Central Engine and Unifying Schemes, J.F. Gallimore, S.A. Baum, C.P. O’Dea. 974. “Common Envelope Evolution in Binary Systems,” M. Livio. 989. “The Interpretation of Color-Magnitude Diagrams through Numerical Simulation and Beyesian Inference,” E. Tolstoy, A. 975. “On the Erosion of the Helium Layer in White Dwarf Saha. Nova Progenitors,” D. Prialnik, M. Livio. 990. “The Resolved Stellar Population of Leo A, E. Tolstoy. 976. “The Broad-band Energy Distribution of the Misaligned Gamma-Ray Blazar PKS 0521—365,” E. Pian, R. Falomo, G. 991. “The Highest Energy Cosmic Acts,” C.A. Norman. Ghisellini, L. Maraschi, R.M. Sambruna, R. Scarpa, A. Treves. 992. “On the Nature of Radio Galaxies,” A.S. Wilson. 977. “A Reconnaissance of the 900—1200 AA Spectra of Early O Stars in the Magellanic Clouds,” N.R. Walborn, K.S. Long, 993. “Are Microlensing Events Contaminated by Dwarf Nova D.J. Lennon, R.-P. Kudritzki. Eruptions?” M. Della Valle, M. Livio.

978. “The Age-Related Properties of the HD 98800 System, 994. “Spectroscopy of Suspected Variable Stars,” R.A. Downes, D.R. Soderblom, T.J. Henry, M.D. Shetrone, B.F. Jones, S.H. D. Wallace. Saar. 995. “Circumnuclear Disks in Radio-Quiet Active Galaxies,” 979. “HST Imaging and Polarimetry of NGC 5128 (= Centau- A.S. Wilson. rus A), E.J. Schreier, A. Capetti, F. Macchetto, W.B. Sparks, 996. “Magnetic Reconnection and Star Formation in Molecular H.J. Ford. Clouds,” S.H. Lubow, J.E. Pringle. 980. “A Survey of Ca II H and K Chromospheric Emission in 997. “Young Binary Star/Disk Interactions,” S.H. Lubow, P. Southern Solar-Type Stars, T.J. Henry, D.R. Soderblom, R.A. Artymowicz. Donahue, S.L. Baliunas.

981. “H and OH Masers As Probes of the Obscuring Torus in 2 Preprints can be requested at [email protected]. NGC 1068,” J.F. Gallimore, S.A. Baum, C.P. O’Dea, E. Brinks, A. Pedlar.

27 Contents How to contact ST ScI All services and most of the documentation provided by STScI can be New HST Key Projects for Cycles 7-9 ...... 1 found at: http://www.stsci.edu Science News Director’s Perspective...... 2 by sending mail to [email protected] The Hubble Deep Field Project ...... 3 or calling +1-410-338-1082 Probing Globular Clusters’ Cores with the FOC ...... 3 Additionally, documentation and support can be requested at: Paris Meeting ...... 6 Phase I [email protected] H0 Key Project ...... 6 HST Data Archive [email protected] AURA News Instrument Information: http://www.stsci.edu/instruments.html HST & Beyond Committee Report ...... 6 STSDAS http://ra.stsci.edu/STSDAS.html

HST Observatory Any questions about the scheduling of your observations should be Scientific Instruments Status ...... 7 addressed to your Program Coordinator. After program execution, you can always contact your Contact Scientist. PRESTO’s Mosaic page Hubble Data Archive News ...... 8 (http://presto.stsci.edu/public/propinfo.html) contains that informa- Observers and Proposers tion, if you do not know who these persons are. RPS2 for Cycle 6 Observations ...... 9 GO and AR Statistics of PI by country...... 10 Panel and TAC Members for Cycle 6 ...... 10 Cycle 6 Summary Table ...... 11 Newsletter Notes Approved Observing Programs for Cycle 6 ...... 12 Comments, suggestions and mailing list corrections can be addressed to the Editors, Daniel Golombek (+1-410-338-4974, Institute News [email protected]) or David R. Soderblom (+1-410-338-4543, Office of Public Outreach ...... 23 [email protected]). Initiative to Develop Education through Astronomy...... 23 Design and Layout: John Godfrey Live from HST ...... 23 The STScI Newsletter is issued by the Space Telescope Science Education Session at HST Paris Meeting ...... 24 Institute, which is operated by the Association of Universities for The Digitized Sky Survey II - Preliminary Data ...... 24 Research in Astronomy, Inc., for the National Aeronautics and Space Administration. Sabbatical Visitors at STScI ...... 25 ESA Fellowships at STScI ...... 25 Colloquia, Symposia, and Workshops ...... 26 NON PROFIT IAU Symposium No.179 New Horizons SPACE U.S. POSTAGE from Multi-Wavelength Sky Surveys ...... 26 TELESCOPE PAID Recent STScI Preprints...... 27 SCIENCE PERMIT NO. 8928 INSTITUTE BALTIMORE MD How to contact ST ScI ...... 28 Newsletter Notes...... 28

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