October 1995 • Volume 12, number 2

SPACE TELESCOPE SCIENCE INSTITUTE Highlights of this issue: • Dr Michael Hauser arrives as STScI Deputy Director. • Dr Carol Christian arrives as head, Office of Public Outreach. • Director’s Perspective Newsletter on page 2.

atomic and molecular species. As a basic premise is to use precisely 6 NGC 891 Atomic Physics with the Radio 4 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 consequence of the high signal-to- determined experimental f-values for 3000 x III x Goddard High Resolution III x x V

75 x V x I 2 V II 000 x x I V x x x 50 V I I x

Flux Density [MJy/sr] V x 1000 x III I O3O4 O5 x O6 O7O8 I I 25 O9B0B Spectral Type 1

0 4 2 0 -2 -4 Spectrograph noise ratios attained (typically 200 to multiplets containing a weak interstel- Relative Distance Along Major Axis [ '] by Steven Federman, 1000), many lines of interstellar lar line to ensure the linearity between University of Toledo species were detected for the first time. amount of absorption and abundance. and Jason Cardelli, First detections include weak This abundance then is used to derive a Villanova University intercombination lines where the suite of self-consistent oscillator Most interstellar species have a large excited electron changes spin. strengths for the other lines. In other fraction of their electronic transitions Our high quality spectra showed words, the relative f-values derived at far ultraviolet wavelengths. Many of many lines of neutral sulfur (SI) and astronomically are placed on an Science News these transitions are accessible in the singly-ionized iron (Fe II). These data absolute scale with the experimental wavelength range covered by gratings are of very high precision and are results. The final step involves comparing the astronomically-derived oscillator strengths with other laboratory measurements and with results from large-scale computations like the Opacity Project. Two methods of analysis were applied to the GHRS data: for S I a curve-of-growth analysis was performed (Federman & Cardelli 1995, ApJ, in press), while for Fe II the observed variation of apparent optical depth with velocity (the τ - v method) was studied (Cardelli & Savage 1995, ApJ, in press). Neutral sulfur is a minor constituent because its ioniza- tion potential is less than hydrogen’s, and as a result S I absorption mainly arises from denser, cold gas along the sight line to a star. Therefore, in a Fig. 1 — Curve of growth for S I. The position where the optical depth at direction with a single principal line center equals 0.5 is indicated. For larger optical depths, saturation affects component of dense gas, a curve of the analysis. growth can be used to extract the abundance of S I from a weak line of a of the Goddard High Resolution indicating the limitations in the multiplet and the Doppler width (or b- Spectrograph (GHRS). We are available atomic data used for value) for the absorbing material from involved in a variety of programs that interpretation. Of particular interest to a strong line of the multiplet. Fe II, on probe the interstellar medium through our research are comparisons of the other hand, is the predominant absorption lines seen against the astronomical results with available form of iron in interstellar space and continuum of an early-type back- laboratory and theoretical data on absorption is seen in many compo- ground star. Our observations reveal atomic transition probabilities and nents. Curves of growth are usually not spectra rich in absorption lines from oscillator strengths ( f-values). Our reliable under such circumstances and continued page 3 SpaceST ScI NewsletterTelescope Science • Science Institute News • Newsletter

Director's Perspective the Goddard High Resolution and Astronomy and Solar Physics, and by Bob Williams Faint Object Spectrographs. The Time previously the Infrared Astrophysics and F.D. Macchetto Allocation Committee and its Branch, Mike has considerable component panels will review all the experience in the management of large Life at Space Telescope Science proposals during the next month, and projects. He has been a part of several Institute and with HST is now reaching meet in November 1995 to carry out important scientific investigations, a steady state, but like the Universe it the peer review process. including IRAS and COBE, and serves is an evolving equilibrium. It is not an In addition to supporting the work on a number of prominent national exaggeration to say that HST is an associated with the different observing committees as well. He has specialized outstanding scientific success and is cycles, ST ScI is preparing to operate in infrared astronomy and instrumenta- making fundamental contributions to and use the two new instruments, tion, and therefore has a good technical all areas of astronomy, both by NICMOS and STIS, which will be knowledge of space hardware which confirming and expanding our deployed in the 1997 Servicing will be valuable to the HST commu- understanding of a variety of physical Mission. The development of these nity. It is a pleasure to welcome Mike phenomena and by providing observa- instruments is proceeding extremely to ST ScI as the new Deputy Director. tions and data that challenge current well, thanks to the commitment of the Dr. Carol Christian, formerly with wisdom. The Institute is working very many individuals involved in these the Center for Extreme Ultraviolet hard to schedule the HST with the projects and to the excellent communi- Astronomy at Berkeley, joined the highest possible observing efficiency, cations established with the Investiga- Institute on September 18th as Head of and efficiencies higher than 50% are tion Definition Teams. the Office of Public Outreach. Carol is now being attained. HST users are The long term future of the HST is familiar to the Institute, having served working equally hard to analyze their currently projected to be in very good on our Visiting Committee and as chair data and produce a steady stream of shape, with the Advanced Camera for of the STSDAS Users’ Committee. In scientific results at the forefront Surveys (ACS) being built for the 1999 addition to her experience in both of astrophysics, which appear in Servicing Mission and the current ground-based and space astronomy, the scientific journals and in the activities within ESA to define an Carol is very interested in the popular press. instrument for the 2002 mission. These applications of technology to data This spring HST users joined activities are concurrent with negotia- transfer and outreach. She created and together with ST ScI staff in a tions between NASA and ESA to successfully secured funding for a workshop entitled “Calibrating HST: extend the Memorandum of Under- national education program, the Post-Servicing Mission.” Roughly 75 standing between the two agencies Science Information Infrastructure, and HST investigators and a comparable beyond the current expiration date of she has good familiarity with current number of Institute staff attended this 2001. An important element in this efforts in astronomy education and forum for detailed presentations and extension would be ESA’s provision of computer technology. Carol will be a discussions concerning the calibration a new instrument. (See the September valuable asset to the Institute not just and analysis of post-servicing mission ECF Newsletter for details on the in leading our development of the data. The meeting was useful both for instruments under study) We are very outreach program but also in advocat- the HST users, who were able to ask optimistic that the continued success of ing HST programs. questions to Institute staff about their HST will be assured by the combina- On the negative side of the scale, we data, and for the Institute, which tion of excellent scientific output and a regret to announce the departures from benefited from some novel approaches solid program to deploy state-of-the-art STScI of two stalwarts of the Institute, to data analysis being made by the instruments in each of the forthcoming Bob Milkey and Mark Johnston, two HST community. The proceedings of maintenance missions. people who have made important the workshop were mailed to Cycles 4 A number of key personnel changes contributions to the Institute and the and 5 GOs. have taken place at ST ScI. Following HST program over the years. For more We have recently completed Cycle 4 the resignation of Peter Stockman as than ten years Bob was the Associate observations and are well into Cycle 5 Deputy Director a search committee Director for Program Management and at the time of this writing. The Institute was established by the Space Tele- he performed an outstanding role in the has just received over 1000 proposals scope Institute Council to work with organizational life of the Institute. He for the Cycle 6 Phase 1 submission, for the Director in finding a replacement. has left ST ScI for the American consideration by the TAC, surpassing The search culminated in the appoint- Astronomical Society where he has the record of 863 proposals received ment of Dr. Michael Hauser as the next become the Executive Officer. We wish last year. This overwhelming interest Deputy Director. Mike, who begins his him well and we look forward to the far exceeds any previous response for a new duties as Deputy on October 2, many opportunities that we will have NASA project and is a measure of the has been on the staff of Goddard Space to continue to interact with Bob in the value with which the community holds Flight Center for more than 20 years. future. Mark Johnston has held a HST. Cycle 6, of course, represents the As Chief of the Laboratory of number of positions during his 13 2 last opportunity for observations with October 1995 years at the Institute. His most recent October 1, when he will join a private compounded by further cuts to the GO assignment has been as the Head of company in California involved in funding that resulted directly from the PRESTO, and thanks in large part to scientific software. Congressional rescission of funds his efforts the efficiency of HST Finally, we continue to be concerned previously appropriated late last year. observations has risen steadily to the about the overall poor funding We are working hard with NASA and current high values. Mark has made situation for science and its effect on the community to protect this area as many other significant contributions the HST budget. Congressional budget much as possible in the future because to HST operations, e.g., the RPS decisions have resulted in significant the scientific productivity of HST proposal entry system and the SPIKE reductions in the HST budget recently, would be seriously impacted. scheduling system. His great creativity which have affected the funds available will be missed after his departure on to GOs and GTOs. This effect has been

Atomic Physics from page 1 another method is needed to analyze flat portion of the curve of growth analyzed. Figure 2 shows a composite the data. The τ - v method allows one represents an uncertainty in the b-value apparent column density profile for to express the apparent column density of only 0.1 - 0.2 km s-1. Fe II toward β1 Sco, constructed by at each data point in velocity. Compari- The astronomically derived S I combining portions of different son between weak (small f-value) and f-values can be compared with other profiles where there is no unresolved strong (large f-value) lines can be used determinations. Of particular interest saturated structure. The apparent to check for unresolved saturated to spectroscopists is a comparison with column density profile is remarkable in structure in the cores of the stronger the results from the Opacity Project. that it shows Fe II column densities lines. In the limit where no unresolved Our results for transitions involving the spanning a range of 10,000. The saturation is present, the apparent ground state of S I (3p4 3P) and excited amount of Fe II in a variety of column density profiles for weak and 3S° states agree with the theoretical interstellar environments is more strong lines match each other. results from the Opacity Project at the clearly defined than was possible in Toward ζ Oph, we detected 27 lines 5 - 10% level! The results for the 3D° the past. of S I arising from 14 multiplets. The states are not always as consistent, but These astronomical results for Fe II absorption comes from the velocity where significant disagreement arises are timely. They provide a benchmark component associated with dense gas (~ 50% level), the differences can be for comparison with the ongoing work -1 (vhelio = -15 km s ). Although ultra- traced to additional mixing among of the Iron Project. For transitions that high-resolution (~ 0.3 - 0.5 km s-1) levels beyond what was considered in do not involve a spin change, the observations indicate the presence of 2 the calculations. available results from the Iron Project subcomponents, the data for K I As noted above, Fe II probes many for strong lines agree nicely with our suggest the subcomponents have kinds of interstellar environments and, results, but the correspondence is not nearly equal strength, and therefore, therefore, is a guide to metal enrich- very good for the weakest lines. The the b-value derived from the curve ment/depletion. The determination of differences for the weak lines may be of growth may represent the separation f-values utilized two relatively weak attributed to the fact that the theoretical in velocity of the subcomponents transitions of Fe II for which new calculations could be providing a (~ 1.1 km s-1). accurate laboratory f-values are poorer representation for some of the The curve of growth for S I based on available to place the analysis on an highly excited states. Furthermore, precise experimental f-values appears absolute basis. Through use of the our results are useful in placing in Figure 1. The filled circles indicate apparent column density method, analyses of QSO absorption systems, the multiplet with the precise oscillator comparisons between these transitions including those at high redshift studied strengths, while the data with open and others (both weaker and stronger with the Keck Telescope, on a firmer circles have refined oscillator strengths ones) allowed us to determine foundation. that provide a consistent curve of corrections to the existing f-values With these two examples, we growth. The position where the optical since by definition, all transitions showed that GHRS spectra are an depth at line center equals 0.5 is should yield the same apparent column essential component in improving indicated because previous analyses of density in the limit of no unresolved atomic oscillator strengths. Laboratory interstellar spectra rarely included saturated structure. results for a select number of transi- weaker lines, but these are essential for In all, f-values for 9 transitions of tions place the astronomical data on an an accurate curve of growth. It is also Fe II, spanning a range in absorption absolute scale for comparison with worth noting that the dispersion in the strength of over a factor 4000, were large-scale computations. These 3 SpaceST ScI NewsletterTelescope Science • Science Institute News • Newsletter

comparisons show that the theoretical gaseous components of the Galactic science aperture, was not degraded by work is quite accurate in most interstellar medium (ISM). the spherical aberration of HST’s instances and the astronomical data Our first results (Roth & Blades primary mirror. In the figure we 1995) focus on the heavy metal present spectra for two of these stars absorption lines of singly ionized zinc with the Zn II, Cr II, and Mg I line and chromium. These ions reside in positions indicated. The pipeline- regions of mostly neutral material, and reduced spectra and calibration the typically weak line strengths are wavelength files were retrieved from easily interpreted in terms of physical the archive through DADS, and final column densities without the need to data reductions made use of the IRAF invoke large saturation corrections. and STSDAS software packages. However, the primary motivation We derived column densities by behind our emphasis on the abun- fitting simultaneous multi-component dances of these two trace metals in the Voigt profiles to the detected absorp- ISM is the crucial role they have tion features. We find, not surprisingly, played in characterizing the physical that the observed large variations in state of neutral gas in damped Lyman- Cr/Zn line-strength ratios apparent in α absorption systems toward high- the figure are reflected in the corre- redshift QSOs (e.g. Pettini et al. 1994). sponding Cr/Zn column density ratios. Our sample consists of Zn II and We interpret this phenomenon as Cr II GHRS ECH-B spectra obtained evidence for changing depletion levels prior to September 1993 toward 20 due to dust in different lines of sight bright (m through the Galactic disk and halo. Fig. 2 — Composite apparent column density profile for V < 9) Milky Way disk and Fe II toward β1 Sco. halo stars. The observations were not Zn II and Cr II represent the affected by the failure of Side 1, and dominant ionization stages of Zn and the spectral quality of these data, all Cr in neutral gas, and when combined

suggest where further improvements obtained through the 0.25" small with H I and H2 measurements toward can be made. In closing we note that this approach was also used to improve our understanding of ultraviolet transitions in the molecules CO (Lambert et al. 1994; Federman et al.

1994) and C2 (Lambert et al. 1995) References Lambert, D.L., Sheffer, Y., Gilliland, R.L. and Federman, S.R. 1994, ApJ, 420, 756 Federman, S.R., Cardelli, J.A., Sheffer, Y.; Lambert, D.L. and Morton, D.C. . 1994, ApJ, 432, L139 Lambert, D.L., Sheffer, Y. and Federman, S.R. 1995, ApJ,438, 740

GHRS Archival Spectra of Interstellar Zinc and Chromium by Katherine Roth The HST Archive contains a wealth of images and spectra that are made available to the astronomical commu- Two representative Zn II and Cr II spectra extracted from the GHRS archive. nity within one year from the date the The dotted lines represent our adopted stellar continuum levels across the observations are executed. Chris interstellar absorption features. HD 23630 (η Tau; l= 167°, b=-23°.5) is one of Blades and I are engaged in an effort, the nearest stars in our sample at a distance of only 125 pc, while HD 149881 using the spectral database, to model (l =31°, b =36°.2) is over 2 kpc away. These lines of sight illustrate the wide the disk and halo distribution, range of profile complexity and relative absorption strengths present in the Zn II 4 dynamics, and physical state of various and Cr II archival database. October 1995 these same stars (Diplas & Savage accurate fiducial has been established, Keck, and KPNO observatories, 1994; Savage et al. 1977), our more meaningful interpretations of although the desirability of selecting a measured column densities lead damped Lyman-α QSO absorption second field in the southern CVZ is directly to Zn and Cr gas-phase systems will be possible. acknowledged should this be possible abundances. Since Zn is generally in the future. The field is more than believed to not deplete onto dust References two degrees away from any bright star grains, Zn abundances are taken as Diplas, A. & Savage, B. D. 1994, (< 2 mag), and devoid of nearby bright metallicity indicators in the ISM as ApJS, 93, 211 sources, known nearby clusters, and well as in QSO absorption systems. In Pettini, M., Smith, L. J., Hunstead, R. W., & King, D. L. 1994, ApJ, 426, 79 contrast, Cr is highly refractory, and Roth, K. C. & Blades, J. C. 1995, ApJ, previous studies have shown that Table 1 445, L95 toward nearby disk stars nearly all Limit of magnitude for 75 2100 second exposures Savage, B. D., Bohlin, R. C., Drake, J. (≥ 99%) of the Cr is missing from the F., & Budich, W. 1977, ApJ, 216, 291 Filter Effective AB mag gas phase and presumably has been Name Wavelength limit depleted onto grains. F300W 2963 27.65 We find a large range of values for F450W 4527 28.11 the gas metallicities and Cr/Zn The Hubble Deep Field project F606W 5940 28.73 abundance ratios in the archival data. by H.C. Ferguson F814W 7878 28.08 Our Zn abundances are not consistent Among the most striking images with the solar valve, with between 25 obtained with the refurbished HST are and 75% of the Zn II apparently Table 2 those of high-redshift galaxies. missing from the gas phase. The Ground-based 10 sigma Limits Impressed by the cycle-4 images, correlation between this amount of STScI director Bob Williams decided Band Limit Reference “missing” Zn and the fractional to devote a significant fraction of his Un 26.2 (Steidel, Pettini & Hamilton 1995) abundance of molecular hydrogen AB HST Cycle-5 discretionary time to the B 26.2 (Metcalfe et al. 1995) (f(H )) argues that dust depletion AB 2 study of the formation and evolution of V 25.8 (Smail et al. 1995) processes are indeed affecting the AB galaxies. This project is being carried R 25.8 (Smail et al. 1995) measured Zn abundances, and AB out as a community service. The data I 25.1 (Smail et al. 1995) therefore Zn is not always a reliable AB are non-proprietary and will be made metallicity indicator. If we consider available soon after they are obtained. only the low f(H ) lines of sight where 2 On March 31, a special Advisory fewer than 0.1% of the total hydrogen bright radio sources. The extinction is Committee met to discuss how to best is in molecular form, we find 35±6% A = 0 to within the accuracy of use this time to make an impact on V of the Zn has been processed onto current measurements; 21cm observa- studies of the formation and evolution grains, assuming the intrinsic tions give N = 1.72 x 1020 cm-2 along of galaxies. It's recommended that the H metallicity of the ISM is solar. Since the line of sight. time be devoted to deep images of one there are no known high f(H ) QSO 2 field, making use of the Continuous absorption systems, this suggests that Filter Selection Viewing Zone (CVZ) to increase the existing metallicity estimates in high- The selection is governed by total exposure time. The project has redshift absorbers based on Zn/H balancing the desire for depth and become known as the “Hubble Deep abundance ratios are low by about color information as well as by Field” (HDF). 0.2 dex. practical considerations involving The companion article by Hans The Cr/Zn abundance ratio in the scattered Earth light. The current plan Martin Adorf in the September issue archive sample ranges from 2 — 17% involves roughly equal observing times of the ST ECF Newsletter describes solar. This approaches the observed in the F300W, F450W, F606W, and the issues such as field selection, filter high-redshift values of 20 — 80% F814W filters. choice, observing strategy, and options solar, and perhaps it is not necessary to This filter combination provides a for parallel observations. invoke different dust formation and reasonable compromise between depth Up to date information can be found destruction mechanisms in these and spectral coverage, while at the on the HDF web page under the presumably evolving galaxy precur- same time making nearly optimal use Observer heading. sors. Future observations with HST of of the “bright time” in the continuous more distant stars and extragalactic Field Selection viewing zone. Because the CVZ objects which probe the full extent of observations graze the limb of the The HDF field is at 12h 36m 49.42s the Milky Way disk and halo will Earth, there are significant periods of +62 13' 46.3" (J2000). The northern provide for a better understanding of time when the WFPC2 background is hemisphere was chosen to allow for abundance and depletion processes dominated by scattered light from the follow-up observations from the VLA, within the Galactic ISM. Once an Earth. The F300W observations, which 5 SpaceST ScI NewsletterTelescope Science • Science Institute News • Newsletter

assumed that the 50 % incompleteness limit corresponds to 3 sigma. Hubble Deep Field With the four-filter strategy the HDF 0h 12 hm 36 49.4s (2000.0) will thus reach depths at least three +62° 13' 46" magnitudes fainter than the deepest ground based images in the red bands, 2 magnitudes deeper in the B band, and 1 magnitude deeper in the U band. The 80% completeness limit of current

deep spectroscopic surveys is BAB ~ 24,

and IAB ~ 22.5. For at least the next few years, information on the redshift distribution of such very faint galaxies will have to come from statistical analysis of the color distribution, or from gravitational lensing studies (e.g. Smail et al 1994).

Data Distribution NCP It is our goal at STScI to provide the data as quickly and to as many 80° CVZ researchers as possible, while at the same time making sure that the quality 70° 1 Week of the finished product is not compro- mised by taking too many shortcuts in 60° 8h 16h the data reduction. We anticipate that different people 50° will want different products of the

40° observations, ranging from all the raw 15 h Ursa Major h Cluster 9 data and calibration files, to final catalogues of detected objects and their h 14 10 h photometric parameters. The current h h 13h 12 11 plan is to release the data on January 15, 1996, roughly two weeks after the observations are complete. This brief delay in the release will provide time The position of the Hubble Deep Field on the sky. The wavy lines at the top of the image represents for STScI to construct cosmic-ray the galactic plane. The large circles show the region of the sky swept out every 55 by HST Continuous cleaned, summed images and a viewing zone, and the smaller circle shows the portion swept out in one week. The X marks the preliminary source catalog, and position of the deep field. will avoid placing an impossible load on the archive from too many people trying to access the individual are always dominated by read noise, Existing HST observations indicate data frames. make efficient use of this time. that most galaxies fainter than I ~ 23 The data will be summarized in Table 1 shows the observing time have half-light radii smaller than 0.2", an AAS poster and a paper detailing and estimated 10σ limiting magnitudes with sizes decreasing to fainter the observational strategy and data of our preliminary 150 orbit schedule. magnitudes, so the aperture size is reduction, with a minimum of These numbers may change slightly reasonably conservative for objects at interpretation. for the final version. They are the HDF limits. After January 15, it will be “open calculated using nominal handbook For comparison, Table 2 shows the season” on the HDF data and publica- values for the bandpass throughputs, limits reached by the deepest ground tions therefrom. At that time we hope readout noise and dark current, but based observations. These are 10 to have the calibrated, summed images using predictions of a detailed sigma limits on the AB (Oke 1974) available in the HST archive, along zodiacal+scattered light model system, converted from the author’s 3 with all the individual frames, and (SEAM) for the sky background. The sigma limits, where provided. Where 3 possibly some intermediate cosmic-ray object aperture size used is 20pix sigma limits are not provided, we have cleaned images at different offset 6 (approximately 0.5" diameter). positions. The summed images are October 1995 small enough that they may be therefore be lost. Many of these nmo95.html. The proceedings will be reasonably extracted over the network. pointings are relatively short (less than published by the ASP. However, the full set of individual 2 orbits) and may not be CR-SPLIT. The workshop was designed to images is large enough that it is best As this program is conducted as a allow staff from Gemini, Subaru, sent on tape. If you are sure now that public service, the data are placed Keck, HET and ESO’s VLT to learn you would like all the individual data immediately in the public archive. frames, you may request a tape in At the request of the STScI Director, advance from [email protected]. we have formed an internal team to define an observing program and to HDF Clearinghouse collect these data. Its members are While there is likely to be lively John MacKenty, Sylvia Baggett, John competition in interpreting the HDF Biretta, Daniela Calzetti, Stefano images and carrying out follow up Casertano, Harry Ferguson, Andrew observations, it is our hope that there Fruchter, Marc Postman, Alex Storrs, will not be much needless duplication and David Taylor. After consideration of effort. To this end, we invite anyone of the existing programs and the contemplating follow-up observations contents of the HST archive, we have or detailed analysis to share informa- chosen to explore a less visited region tion through the HDF web page. We of phase space with the intention of re- will provide pointers to other web visiting this decision after a few locations that describe research on the months of data are obtained. HDF. The aim is to establish a forum The observing strategy is to use the for publicizing the status of follow-up WFPC2 filter which provides wave- work in order to avoid too much lengths slightly shorter than those duplication, and to provide points of available from the ground but still has contact for cooperation or collabora- the maximum available sensitivity. tion between various investigators. If Ground based observations (initially you are interested in participating, the digitized sky survey plates) at please contact [email protected]. longer wavelengths will be used to estimate the colors of objects and (for Anonymous spiral galaxy serendipitously observed with References the single exposure instances) to WFPC2 in the F300W filter on the WF4 detector. The Smail, I., et al. 1995, ApJ, 449, L105 discriminate between sources and galaxy spans approximately 12 arcseconds and has at least Smail I., Ellis, R. S., & Fitchett, M. J., cosmic rays. Please contact us if you 5 bright knots in its inner regions. 1994, MNRAS, 270, 245 have questions or comments. Steidel, C. C., Pettini, M. & Hamilton, D., 1995, preprint from each other and from existing Metcalfe, N., Shanks, T., Fong, R., & Roche, N., 1995, MNRAS, 273, 257 New Methods of Observing facilities in terms of planning for new for the 21st Century and optimal observing strategies and operating modes. Given the cost of by Glenn Miller, Mark Johnston these new telescopes, and their ability and Ethan Schreier WFPC2 UV Parallel Survey to exploit superb seeing conditions, the by John Mackenty An international workshop to large question examined at the In July, we have initiated a new consider innovative observing and workshop was whether traditional parallel program known as the scheduling strategies for the 21st ground-based scheduling methods “WFPC2 Ultraviolet Parallel Survey” century was held at the University of were effective in realizing the scientific (DD 6253). The primary goal of this Hawaii in Hilo in July 1995. The potential of these new facilities. The survey is to discover sources with workshop considered a variety of consensus was that new scheduling excess ultraviolet flux. The secondary topics including queue scheduling, techniques such as queue (or inter- goal is to determine the UV morphol- service and remote observing, leaved) and flexible scheduling, were ogy for a randomly selected sample of scheduling in response to changing not only required but have already field galaxies. This program is observing conditions, and data been successfully used at several designed to utilize those WFPC2 reduction and archiving. Speakers from observatories. The experience of space parallel observing opportunities which a variety of observatories gave talks on observatories such as HST was would otherwise not be used by the their experience with new and classical particularly relevant, since we already Cycle 5 parallel programs and would modes of observing. The abstracts can do many of these things. be found at http:/www.jach.hawaii.edu/ 7 SpaceST ScI NewsletterTelescope Science • Science Institute News • Newsletter

The need for quantitative under- out that many projects are already It became quite clear at the standing of observatory operations and using versions of the HST planning workshop that the experience of STScI observing efficiency was emphasized tool. The viewgraphs from this talk are with HST will be of increasing and several speakers presented such available from http://presto.stsci.edu/ relevance to the next generation of quantitative analyses. Tod Boroson of spike/ ground-based facilities. HST has been the U.S. Gemini Program Office/ In order to foster better communica- operated in a “service observing” NOAO presented a simulation of tions between observatory schedulers, mode since the telescope first went operations for a traditional model and software developers and users, into operations in 1990. for interleaved/flexible operations. In Johnston proposed three recommenda- We plan to help with this process by the case of ground-based telescopes, tions for the future: participating in future workshops of weather is unpredictable. In addition, this type, and we encourage the • Data Interchange: Develop a multi- times of excellent seeing are not only establishment of new dialogs between Observatory interchange format for rare (10-25%) but not very predictable. the STScI and other facilities. In scheduling data. This will facilitate This means that with traditional particular, the Institute and Gemini are coordinated campaigns and allow scheduling, top-rated programs are not planning to discuss possible coordina- comparison of scheduling methods completed at a high rate and that tion in planning and scheduling work, between facilities. programs don’t often get the seeing within the context of a more general they require. The analysis showed the • Benchmark Problems: Publish effort by AURA to foster technical potential gain in both quality and benchmark problem sets and coordination efforts among its centers. quantity of science if interleaved and solutions for realistic observing flexible scheduling are used. scenarios Mark Johnston’s talk “Scheduling • Better dissemination of information: Tools for Astronomical Observations” Provide more information to other discussed the need for automated sites about methodology, approaches, planning and scheduling tools, outlined tools, results, and problems. different approaches for solving the Suggested venues include: WWW problems and presented examples of pages, listserv mailing lists and systems in use today. He also pointed future conferences.

WFPC2 image of HH 47

An example of the images obtained with HST that are available for downloading. You can find all the press releases’ photographs and texts, plus animations at http://www.stsci.edu/ public.html. To download the image directly, click the “Load to local disk” button in the Options menu at the top of the Mosaic window. If you use Netscape, you can save the image selecting “Save As” from the “File” menu. (Photo courtesy of J. Morse)

8 October 1995

Scientific Instruments Status dark current has continued to show which is continuously variable from by Ron Gilliland improved behavior, although a format 371 to 976.2 nm. Several programs dependence was recognized in the last have now utilized the ramp filters and Since the last Newsletter, all of the test — this will be further character- everything appears to be working well. instruments on HST have continued to ized before the f/48 is released for perform quite well and stably. In routine science observations. addition, results of ongoing tests to calibrate and characterize the f/48 side Hubble Data Faint Object Spectrograph Archive News of the Faint Object Camera have been The FOS Red and Blue sides have encouraging and we are optimistic that both continued to perform well with no by Marc Postman it will be made available for spectros- HST Observatory substantial anomalies arising. Further As post-COSTAR HST data copy in Cycle 6. characterization of polarimetric accumulates in the Hubble Data The mid-point of observations capabilities has suggested substantial Archive (HDA), usage has increased. between the first and (planned) second problems (perhaps as a result of small Over the last 4 months, the average servicing missions has now been y-base instabilities) with gratings G190 retrieval rate has been 15 Gbytes per passed. The proceedings of the Second and G270 on the Red side. Existing week, comparable to the present data HST Calibration Workshop held at ST GO/GTOs using these have been ingest rate. The total data volume of ScI 15-17 May 1995, (edited by A. contacted and advised to move their the HDA is now approximately 1.7 Koratkar) were distributed. A full observations to the Blue side. Tbytes. The Data Archive and revision of the HST Data Handbook Distribution Service (DADS) has will be available next month. Goddard High Resolution Spectrograph managed this load well. Between June If you would like more information, Both Sides 1 and 2 of the GHRS and August DADS was up and running please be reminded that the World have continued to return excellent 91 percent of the time. Improving the Wide Web is a repository for late observations with no substantial performance and reliability of DADS, breaking instrument news, frequently anomalies to report. The first use of none the less, remain top priorities asked questions, details of calibrations, FLYLIM for a science program was in (indeed, we would like to see the duty etc. Instrument pages may be easily June 1995 and resulted in a substantial cycle approach 100 percent!). accessed under the ST ScI homepage: reduction of background noise for One of the more significant http://www.stsci.edu. this observation. This is a procedure reliability improvements will be the that limits background level by Faint Object Camera replacement of the Aptec array throwing away 0.2 second time slices processor which handles the FITS Science and calibration observations with excess counts likely to have arisen conversion of HST datasets prior to with the f/96 relay have continued to from noise bursts. optical disk archiving. The Aptec also provide excellent results. controls a large staging disk which is The FOC f/48 relay has not been Wide Field and Planetary Camera 2 used for both data archiving and used for routine science observations Stable operations for the WFPC2 retrieval. Aptec problems accounted since the initial high-voltage turn-on have also continued with no substantial for 25 percent of DADS downtime failure in September 1992. Subsequent problems arising. Characterization of during the last quarter. engineering observations showed that the instrument performance has turned Testing of a major new tool that the detector background was higher up an infrequent, but important type of automates the generation of tapes for than nominal, time-varying and with anomaly that observers will want to external distribution has begun. Other spatial structure present. The cause of guard against. A bright star just off the near term service improvements will these problems is not thoroughly corner of the PC can result in multiple include mass tape production and/or understood, but may be related to diffuse arcs imaged onto it. A bright continuous on-line access to large, breakdown in insulation or potting star near the outer corner of the PC popular datasets such as the upcoming around high-voltage components. pyramid facet (region where outer WFPC2 observations of the Hubble Modifications to the turn-on procedure corner of WF chip would be) can Deep Field (see related article in this have enabled more robust operations, result in sharp arcs on the PC. Both issue) and direct electronic access to and more recent testing has shown types of ghosts are probably the result proprietary data by PIs. The latter improvements in the background noise of incomplete/inadequate baffling of augmentation will be coupled with level and greater stability. Testing of the PC relay optics. Further details direct delivery of data to your host the f/48 relay, which currently provides may be found by browsing the WFPC2 computer and will eliminate the need the only long-slit spectrographic WWW page. to FTP data from staging areas at capability on HST, passed a major The linear ramp filters are now fully STScI. In the meantime, it should be milestone on July 10th with a operational, with the first science noted that the STDATU staging areas successful calibration of the slit images being taken on 23 June. These do occasionally become full. Users are position to an accuracy of ~0.1-0.2". λ ∆λ filters provide a bandpass / ~80 requested to FTP their archive The troublesome excess background 9 SpaceST ScI NewsletterTelescope Science • HST Observatory Institute • Newsletter

retrievals shortly after they are Now that the HDA is operating on a configuration) tube is now being built downloaded. The staging disk is routine basis, the STScI has begun to up as flight prime detector and should purged of data more than 2 days old. consider options and strategies for the soon undergo environmental tests. The We will significantly increase the long-term enhancement of the archive. hope is that the STF6 tube, now in staging disk space capacity early this We can anticipate the availability of electron scrub, will meet specification fall. As a reminder, DADS status faster and higher density archival and supplant the less desirable chevron information can be obtained by typing: media, especially important after the tube in a few months. The FUV finger [email protected]. 1997 servicing mission when data (Band 1) MAMA flight detector is StarView, the primary user interface ingest rates will more than triple. We being tested. to the HDA, continues to be improved. are now able to incorporate non-HST The flight CCD noise problems The latest added features include: data (e.g., new data from the VLA were largely surmounted in the past direct access to the STScI Digitized FIRST survey) into the HDA on a cost- few weeks and three of the four Sky Survey (DSS), display of world recovery basis. Database searches channels now show about 3.5 e- RMS coordinates when previewing HST and based upon more extensive astrophysi- read noise. The fourth channel is DSS images, improved cross correla- cal criteria such as color, redshift, and still a bit noisy (6 e-). The metal tion features, and ports to Sun Solaris, classification will be added to the vacuum seal of the flight spare detector DEC OSF/1 (on Alpha machines) and growing capabilities of StarView. By has been problematic, most likely due VMS 6.1. these actions we hope to keep the HDA to marginal finish quality of the Access to the DSS (which can also a vital and dynamic astronomical seal surfaces. be accomplished through the WWW; resource. As always, user comments Optical verification testing is has proved particularly popular — and suggestions are welcome. proceeding apace: slit-to-detector since the installation of remote DSS images show that the optical system is access in mid-May, we have received working as expected, with specifica- over 16,000 DSS retrieval requests. A STIS Hardware Status tions easily being met. Verification of new StarView modification, which the aberrated OTA simulator are well by George Hartig should be available by this fall, is a underway. Images obtained with BIA utility to overlay HST instrument STIS optical alignment and testing CCD camera system compare well apertures on DSS images. The overlay is proceeding satisfactorily at Ball with the optical models and the location and orientation can be Aerospace. An alignment problem, Goddard Independent Verification specified either by the user directly or discovered during the band 2 echelle Team is now at Ball using their by using the parameters from any alignments, was traced to distortion of wavefront sensor (ABA) to determine existing HST dataset that can be the Mode Selection Mechanism the image and pupil locations and displayed with the preview utility. We (MSM) optics ring caused primarily by aberration content of the RAS. anticipate this utility will be very an overly long screw. This has been The corrector system breadboard is helpful in phase II planning of cycle 6 corrected, the ring mounting pads on scheduled to be assembled and aligned HST observations and in determining the MSM were dressed to be more during the last week of August and which archival data are best suited for coplanar, and the ring has been will be placed in the RAS to verify a given research program. Other reinstalled on the mechanism. Testing the capability of the corrector mirrors StarView improvements which should is now in progress to assure proper to cancel the OTA aberration in be available this fall include column alignment of the ring optics. Mean- early September. reordering on the table format screen, while, alignment of the mode 1.4 export of query results with proper echelle is proceeding. The original column size and order based upon mode 1.3 echelle will not be installed; NICMOS Status parameters set in the table format we will wait for the replacement screen, and a port to OpenVMS Alpha by John MacKenty, David Axon, echelle, which is on order. and Chris Skinner (now in beta test). A problem was also discovered with Requests for modifications of the the order sorter mounts — a shiny ring The construction of the NICMOS proprietary period for HST data can was left unmasked at the edge of clear science instrument proceeds on now be done through STEIS. Select the aperture. The filters are being schedule at Ball Aerospace. A major “Requesting Proprietary Rights dismounted and the mounts reworked milestone was successfully passed with Modifications” option on the Archive to remove this potential straylight the testing of the flight detectors home page. All requests should be problem. The filters will likely be installed in the cooled dewar. All three received at least 2 weeks before the installed on the MSM after its detectors performed as expected and current proprietary period expires and reinstallation in the truss. are not expected to be removed from must be approved by the Director’s The NUV (Band 2) MAMA flight NICMOS until after its flight in HST. office before being enacted. detector developed glow discharge on NICMOS will undergo thermal 10 the tube exterior so the STF2 (chevron vacuum testing next spring at Ball and October 1995 is expected to arrive at Goddard Space change-out. One unique aspect of the compared to 5 years of the existing Flight Center in August 1996. NICMOS change-out is the addition of onboard Gyros. Priority #3 has been The NICMOS IDT (Rodger another kind of interface: the cryo- reserved for the Spare Rate Sensing Thompson, PI) and the STScI are genic venting system. Beside the Unit (RSU) to replace RSU #2. Finally, working together to prepare for mechanical, electrical, and software Priority #4 has been assigned to the NICMOS operations. The Proposal interface the cryogenic interface Spare Solar Array Drive Electronics Instructions are essentially complete provides an exhaust path for the (SADE) to replace SADE 2. Prior to and the commanding software is on gaseous nitrogen from the solid the First Servicing Mission SADE #1 schedule and approaching the half way cryogen dewar. Next in the list is failed due to thermally over stressed mark. The data reduction pipeline has assigned to the Spare Data Interface transistors. The SADE 1 unit has been proceeded through the Preliminary Unit (DIU) that will replace DIU #2 refurbished including the addition of Design phase and several elements whose A-side electronic has failed due transistor heat sinks. (including enhancements to IRAF/ to a short circuit in the Power Control The Critical Design Review did not STSDAS and the basic image Unit (PCU) during the Fist Servicing reveal any serious “show stopper” for calibration parts) passed their Final Mission. This spare will restore critical the upcoming Servicing Mission, Design reviews and are being coded. redundancy for commands and which as of now is scheduled for The SMOV requirements have been telemetry. A reboost test will be February 13, 1997, which - by the way defined and an initial draft of the performed next. A reboost of HST to a - is NOT a Friday. activities to be performed has been higher altitude is mandatory for the written. A NICMOS mini-Handbook Third Servicing Mission in November was distributed with the Cycle 6 Call 1999 especially in the light of the Filter choice for the Advanced for Proposals and a complete NICMOS expected maximum of the solar cycle Camera for Surveys Instrument Handbook and Proposal during that time. The objectives of the Instructions are being prepared for Reboost Test is to demonstrate the by Mark Clampin Cycle 7. ability to reboost HST without The Advanced Camera for Surveys retracting the solar arrays. To improve (ACS) is a 3rd generation instrument mechanical stiffness a support post will for HST. It is scheduled for installation Manifest for the Servicing be installed on the Flight Support during the 1999 Servicing Mission. Mission 1997 System. Finally, the Spare Engineering ACS consists of three cameras, a Wide Science Tape Recorder (ESTR) will Field Channel (WFC), a High by Manfred Miebach replace the faulty Tape Recorder #2. Resolution Channel (HRC), and a During the Critical Design Review Solar Blind Channel (SBC). The WFC (CDR) of the Second Servicing Secondary Priority Items features a 204" × 211" field of view, Mission the “1997 Manifest” was Priority #1 within the Secondary with a plate scale of 0.05"/pixel, and is presented specifying the priorities in Priority category is assigned to the optimized for sky-limited V and I-band hardware to be exchanged and replacement of ESTR #1 with new imaging. The HRC provides spectral activities including its priorities for the Solid State Recorder (SSR). The new coverage from 200-1000 nm with a upcoming Servicing Mission presently SSR provides 10 times the capacity (12 26" × 27" field of view and an effective scheduled for February 1997. GBIT versus 1.2 GBIT) of the existing plate scale of 0.026"/pixel. The SBC mechanical recorders. Furthermore, the covers the spectral range 115-170 nm Primary Priority Items new unit will allow simultaneous with a 30" × 33" field of view and a The primary priorities has been recording and dumping of science data. plate scale of 0.03"/pixel. assigned to the replacement of the Priority #2 within the secondary The Camera has two filter wheels GHRS with the second-generation category is assigned to the Hemi- shared by the WFC and HRC, and a Space Telescope Imaging Spectrograph spherical Resonator Gyros (HRG) to third filter wheel for the SBC. A total (STIS), the replacement of the FOS replace Remote Sensing Unit # 3 of 29 filters will be mounted in the with the Near-Infrared Camera and (RSU-3) and Electronic Control Unit WFC+HRC filter wheels. The filter Multi-Object Spectrometer #3 (ECU-3). All of the Gyros onboard wheel closest to the detector will (NICMOS), and the replacement of are of concern because of the generic contain a clear slot allowing the FGS-2. corrosion of the flex leads and in the WFC+HRC cameras to be used in A special aspect of the Instrument long term because mechanical gyros parallel with the broadband filters. change-out is the fact that STIS is are a technological dead end. The new The preliminary filter complement extremely sensitive to particulate HRG has no wear-out mechanism and for the WFC+HRC channels is shown contamination. This results in stringent is based on a solid state gyroscope in Table 1. The science team has requirement for the sun-avoidance with a silica hemispherical shell as the chosen to adopt the Sloane Digital Sky volume in the cargo bay of the orbiter inertially sensitive element. Its Survey (SDSS, AJ submitted) filter set and STIS aperture pointing during the expected lifetime is more than 15 years (Fukugita et al 1995) as one of the 11 SpaceST ScI NewsletterTelescope Science • HST Observatory Institute • Newsletter

Slot Wheel #1 Camera primary broadband filter systems, High efficient, low dispersion along with the standard U, B, and V spectroscopy is provided by a grism 1 Clear WFC filters for WFC programs. For deep for the WFC and a UV prism in the 2 i (SDSS) WFC imaging with WFC, two broad HRC channel. 3 z (SDSS) WFC bandpass filters are provided, a V filter The SBC filters are selected for 4 r (SDSS) WFC similar to the WFPC2’s F606W imaging programs in the FUV and are 5 g (SDSS) WFC (employed for the Medium Deep shown in Table 2. A narrow-band 6 Johnson B WFC Survey), and an I band filter similar to Lyman-α filter will isolate this line for 7 Johnson V WFC the WFPC2 filter F814W. For high observations such as auroral emission 8 Broad V (F606W) WFC efficiency near-UV imaging in the on Jupiter. A narrow band CIV filter is 9 Broad I (F814W) WFC HRC channel, two broadband filters provided for imaging of the nuclei of 10 F658N - Hα (∆λ = 1%) WFC are provided, one centered at 220 nm AGN. Longpass filters, designed for 11 F502N - [OIII] (∆λ = 1%) WFC and one at 250 nm. use in pairs are provided to isolate a 12 UV Polarizer (0°) HRC For wide-field, narrow-band specific bandpass, and will provide 13 UV Polarizer (60°) HRC imaging there are Hα and [OIII] filters, coverage of the spectral region from 14 UV Polarizer (120°) HRC each with a bandpass of 1%. To 120-160 nm where the SBC has good complement them there is a medium- sensitivity. A LiF prism provides a band continuum centered at 547 nm high transmission, high efficiently and Slot Wheel #2 Camera with a bandpass of ~11%. The majority relatively constant dispersion from 120 of narrow-band imaging will be nm to 180 nm. A CaF prism performs a 1 Clear WFC undertaken using ramp filters similar to similar function, but with a cutoff 2 220 nm (180 - 250 nm) HRC those in WFPC2, but with a signifi- wavelength which blocks Lyman-α 3 220 nm (200 - 300 nm) HRC cantly larger monochromatic field of emission. 4 u (SDSS) (300 - 400 nm) WFC view (70" × 30") at any given 5 F550M - 547 nm cont WFC wavelength. Four ramp filters will 6 Grism WFC cover the wavelength region 365-985 Space Telescope 7 [OII] Ramp WFC nm, with a bandpass of 2% at any Analysis News 8 [OIII] Ramp WFC given wavelength. Each ramp filter will 9 Ha Ramp WFC have three strips which are arranged The Space Telescope Analysis 10 IR Ramp WFC parallel to the rotation direction of the News are 3 monthly electronic 11 Redshift quad WFC filter wheel. This will permit the publications with news and 12 Uis Polarizer (0°) HRC central strip in each filter wheel to information on the FOS, GHRS 13 Uis Polarizer (60°) HRC image onto the HRC as well as the and WFPC2. 14 Uis Polarizer (120°) HRC WFC. Two additional 2% bandpass If you are not in our mailing lists 15 clear HRC narrow-band filters are included to and would like to receive them, 16 UV prism HRC provide HRC imaging in the NeV line, please send a message to 17 u' (300-380 nm) HRC for imaging of AGN nuclei, and the [email protected] 18 F344N - Ne V (∆λ = 2%) HRC methane band (892 nm) for imaging of λ ∆λ solar system objects. Finally, a 19 CH4 ( c=892, =2%) HRC quadrant filter is included to provide four 100" × 100" field of view medium Slot Wheel #1 SBC bandpass filters. The ACS filter complement has two 1 Blank sets of polarizers optimized for UV

2 Longpass MgF2 (>1150 Å) and visible band polarimetry with the

3 Longpass CaF2 (>1250 Å) HRC. The UV polarizers will be 4 Blank optimized for the 200-400 nm region

5 Longpass BaF2 (>1400 Å) and are located in filter Wheel 1 to 6 Crystalline quartz (>1500 Å) permit them to be crossed with the UV 7 Blank filters in Wheel 2. The visible band

8 CaF2 Prism (R~100) polarizers are located in filter Wheel 2 9 LiF Prism (R~100) and are designed to be crossed with 10 Blank broad and narrow band filters in Wheel 11 CIV 1450-1650 Å 1. Each set of polarizers comprises 12 Lα three separate elements which give Explore HST’s greatest hits at relative polarizer angles of 0˚, 60˚ and http://www.stsci.edu/public.html. 12 120˚, respectively. October 1995

Cycle 6 Proposal week of December 18. The paper “Visit Status Information” will give Selection Schedule letters will follow shortly thereafter. the status of each visit in the program. by Ron Downes and Mike Shara Plan Window information for unex- ecuted visits is now included in As mentioned in the previous this page. Newsletter, the deadline for Cycle 6 General Observer/Archival Researcher Funding Observations are assigned “Plan proposals was September 15, 1995. Windows” which are a subset of the Upon careful review of the proposal by Ray Beaser observing opportunities dictated by the selection process, we have made two Phase I budgets for U.S. astronomers scientific and spacecraft constraints.

major changes which will allow for a Observers & Proposers are required only for Cycle 6 Archival For most observations, Plan Windows more thoughtful selection by the Researcher Proposals. Budgets for are between 2 and 8 weeks in duration, Telescope Allocation Committee U.S. General Observers (GO) will be but they can be shorter or longer (TAC), and for more rapid notification requested after the selection of Cycle 6 depending on the visit’s constraints. of the results to the proposers. observing Programs. The GO budgets Barring unforeseen circumstances, In the past, the TAC meeting will be submitted for the Phase II your visit will be executed within its occurred immediately after the panel deadline early next year after the Plan Window. meetings, which did not allow the TAC selection of the program. It is easier to implement changes members to study the results of the Funding notification letters for received at least 6 weeks before the panel meeting. We have now included Cycle 5 General Observer Programs published Plan Window opens. a 1.5 week delay between the two were mailed on July 12 and August 1, Changes received beyond this time meetings, so the TAC members can 1995. The deadline for the receipt of may delay execution of the visit. have the time to assure a properly revised Cycle 5 budgets was extended For the observer, the long-range plan balanced science program, both until September 30, 1995. provides the obvious benefit of between panels and within a given Due to NASA budgets constraints, it indicating when the observation will be panel. With this extra time, we will has become necessary to change the executed, to monitor the progress of also be asking the TAC to look more method of funding GO/AR programs. the project and plan for the data carefully at the large (with more than Preparatory funding will be reduced to reduction and analysis. Long-range 60 orbits) science programs. a maximum of 10% of the approved planning also has several benefits to The notification letters have all been funding for a program and should be the entire observatory. The plan allows mailed to the proposers on the same requested only when essential to the Program Coordinators and other day. However, their arrival seem to prepare for the receipt of HST data. observatory staff to order their spread over a two week period. In The balance of funding will be proposal preparation work. The plan order to assure that all proposers conditionally awarded upon the receipt allows the STScI to monitor the receive their results at the same time, of observational data. Expenditures on progress in executing the Cycle’s and to make it as short as possible, we a project will be limited to a funding observations including the detection of will be sending electronic as well as profile which will initially release 50% inter-proposal conflicts. The long- paper notification letters. of the available funding, with the range plan is also a tool for increasing The post-deadline schedule for balance available eight months later. observing efficiency by exploiting Cycle 6 is as follows: Around the end opportunities of good target visibility of September, the referees will begin (e.g. continuous viewing zone or their scientific evaluation of the avoidance of South Atlantic Anomaly proposals, and the Panel Coordinators HST Long-Range Observing Plan impacts). Another important use of the (STScI scientists) will perform a Now Available via the World long-range plan is in re-planning technical evaluation. These evalua- Wide Web observations which miss a scheduling tions, along with preliminary grades, by Glenn Miller, Peg Stanley, opportunity. will be loaded into our TAC database and Wayne Kinzel If you have any questions about the in preparation for the scientific panel The HST long-range observing plan assigned plan windows or status of the meetings. There are 10 scientific is now available via the Presto visits you can contact your Program panels, which will meet in two groups Program Information page. From the Coordinator (who is listed on the from October 30 - November 1 and STScI Homepage you should select program status page). There is also November 2 - 4. The TAC meeting is “Observer” and then “Program Status detailed help which explains the scheduled for November 17-19. After and Visit/Scheduling Unit level proposal and visit status values. Just verification of the database, the STScI information”. click on the appropriate item to see a Director’s review will occur the week After entering your proposal id more detailed explanation. of December 11. The electronic number, a summary of the proposal notification letters should be sent the status will be displayed. Selecting 13 SpaceST ScI NewsletterTelescope Science • Observers Institute & Proposers • Newsletter

The detailed scheduling of HST observations is performed on a weekly basis and begins 4 weeks prior to the week of execution. Approximately 3 News weeks before the week of execution the preliminary timeline of observa- Welcome New Members tions has been established. At this by Goetz Oertel, AURA President point, the scheduled start and end time We are pleased to announce that the University of Minnesota and the of a visit will be displayed on the University of North Carolina - Chapel Hill have joined AURA as its newest WWW page. This information is also members. Bruce Carney from Chapel Hill and Len Kuhi from Minnesota have e-mailed to the Principal Investigator joined our Board. We cordially welcome them. Len had served on the Board or program Contact Co-Investigator previously, from 1978 to 1989, when he was at the University of California — and posted to STEIS. In most cases, we are glad to have him back! Bruce has worked closely with us in several the observations will be executed at capacities. We are glad to see him in this new role. this time, but it is possible that the timeline can be disrupted by instru- ment or spacecraft problems or target of opportunity observations. Key AURA Committees We welcome your comments and by Diana Whitman, AURA Corporate Office suggestions on this new service. Annual elections at the AURA Board meetings change the membership of key commit- tees of the Board. As a result of this year’s elections, the members of the Executive Committee and the Space Telescope Institute Council (STIC) are: Science with the Hubble Executive Committee: Space Telescope — II Bruce Margon, Chair University of Washington A Scientific Conference Richard Zdanis, Vice Chair Case Western Reserve University co-organized by ST ScI and ST-ECF Donald Baldwin University of Washington December 4-8, 1995 Jay Frogel The Ohio State University John Huchra Harvard/Smithsonian Center for Astrophysics UNESCO Buildings — Paris Morton Lowengrub Indiana University The aim of this Conference is Richard Margison University of Illinois to present and discuss the results Goetz Oertel AURA of the last two years of Vera Rubin Carnegie Institution of Washington operations with the fully Lee Anne Willson Iowa State University restored HST. The program will also include reviews of future Space Telescope Institute Council (STIC): HST Instruments, plans for Malcolm Longair, Chair University of Cambridge future maintenance missions, Donald Baldwin, Vice Chair University of Washington and a Special Session on Neta Bahcall Princeton University “Education and HST.” Jacqueline Bergeron European Southern Observatory The Scientific Organizing Richard Ellis University of Cambridge Committee consists of Elizabeth Hoffman Iowa State University P. Benvenuti, J. Bergeron, Jonathan Grindlay Harvard College Observatory R. Ellis, R. Fosbury, Robert Millis Lowell Observatory H. Hammel, R. Kirshner, Goetz Oertel AURA R. Kudritzki, D. Macchetto, Douglas Richstone The University of Michigan G. Miley, V. Rubin, Lyman Spitzer, Emeritus Princeton University Observatory and E. Schreier Robert Szczarba Yale University Juri Toomre University of Colorado For further Information contact: Edwin Turner Princeton University Observatory Britt Sjöberg at ST-ECF ([email protected]) Cheryl Schmidt at ST ScI ([email protected])

14 October 1995

Office of Public Outreach being done with HST. The Education Time for a Good IDEA by Ethan Schreier group, led by Anne Kinney, has The call for proposals for IDEA embarked on a variety of programs, During the Institute’s strategic grants (Initiative to Develop Education continuing and extending the pioneer- planning process in 1993-1994, through Astronomy) went out on ing work done by Laura Danly, the education was identified as one of the August 17th via e-mail and the original lone “Education Project four “pillars” of our long range plan. following week by regular mail. Scientist” at the Institute. Finally, the Subsequently, with NASA’s encour- IDEA grants provide funding for Products and Services group, led by agement and support, and with the professional astronomers to develop Trish Pengra, provided the infrastruc- endorsement of the Space Telescope and carry out innovative educational ture to produce graphics, photos, Institute Council, we set out to greatly and outreach programs with an Institute News animations, posters, TV production, expand our public outreach and emphasis on collaborating with internet, and other technical and teachers or education specialists. n and O education activities. io ut programmatic support for our at re Proposals can be submitted in a wide c a Over the past u c education and public information d h year, we have range of topics, including teacher and E projects. We have been or are engaged • set up student workshops, curriculum or • in a number of projects — local product development, internet usage, G a new Office

n classroom activities, planetarium e multi-cultural programs, public t o of Public t i shows, museum exhibits, teacher i t outreach, student outreach, students n a Outreach, g c workshops, etc. — which will be u research opportunities, and teacher In d recruited staff, v E discussed in future issues of this resources. The IDEA proposals can be o e solicited outside lve nc newsletter. In separate articles of this d in Scie advice, started made in either of two categories: small issue, we discuss the IDEA grants familiarizing ourselves with the world projects, not to exceed $6,000, and program and a workshop recently held of science education, developed a large projects, not to exceed $20,000. at the Institute. preliminary science education plan, The deadline for submission of Meanwhile, we want to thank and embarked on a variety of projects. proposals is October 31, 1995. everyone who has helped develop our A key element was to convene an Proposals will be evaluated by a panel expanded outreach program, especially external advisory committee — the of astronomers, teachers, and educa- mentioning: Laura Danly and Bob STScI Advisory Council on Education tion specialists. Inquiries about the Brown, who as “voices in the wilder- (STACE). This group of 12 experts proposal process, and requests for a ness” worked both locally and from the science education community call for proposals can be made to nationally to advocate STScI activities — astronomers, teachers, and [email protected]. in astronomy education; Mimi educators, from museums, universities, Bredeson, who helped with the and schools, met for the first time last transition to the new organization fall. They provided general guidance structure; Ray Villard, who kept the Keeping the Public Tuned-in and specific advice on how to news releases flowing; Anne Kinney, to Hubble’s Discoveries construct a balanced program spanning who moved into a new domain and by Ray Villard both formal and informal education started formalizing our education activities. Following their strong Every month, dozens of popular program; and Trish Pengra, who while recommendation that we build on articles describe Hubble Space new to the Institute, was key to our existing programs, we also embarked Telescope’s contributions to modern success in starting new programs while on a series of visits and contacts with astronomy, while students and adults keeping essential existing activities and other science education programs, around the world download the interfaces with NASA going. providing us with further valuable telescope’s latest images across the Finally, during the last year, we insights into the world of science Internet. The STScI Public Information engaged in a national recruitment for a education. Office helps to disseminate this head of OPO. By the time this The STScI Office of Public newsworthy science to tens of millions newsletter is printed, Dr. Carol Outreach consists of three groups. The of interested individuals. Christian, formerly at the Center for News and Information group encom- Continual, positive news coverage Extreme Ultraviolet Astrophysics at passes our previous Education and for Hubble has several benefits. Space Berkeley, will have taken over to lead Public Affairs Office, headed by Ray Telescope’s discoveries consistently OPO. We enthusiastically look forward Villard. Ray, with Cheryl Gundy and fire the public’s imagination and have to Carol’s work with us. others, continues to work with HST’s intrinsic cultural, educational and users and with NASA to support press intellectual value. Furthermore, releases and otherwise keep the media because the HST project is federally informed about the outstanding science funded, taxpayers have a right to learn what they are getting for their 15 SpaceST ScI NewsletterTelescope Science • Institute Institute News • Newsletter

investment, as well as to have an are being announced at AAS or other galaxy, smallest identified star). opportunity to share in the wonder of science conferences, we will prepare 6. Deal with unpredicted, transient exploration and discovery. Finally, the and provide all news materials needed events (nearby comets, a nova, resurgence of astrology, UFO sightings by reporters attending the conference. changing weather on a planet). and other occult “sciences” betrays an We can serve as the contact point for 7. Provide new insights into: cosmol- alarming lack of public understanding filtering and coordinating media ogy, extrasolar planets, black holes, about science. Hubble’s accomplish- request for interviews, so that you are dark matter, solar system objects, ments demonstrate that true scientific not swamped with queries. distant galaxies, Earth’s evolution, research is exciting, revealing, and extraterrestrial life. challenging. News Distribution 8. Are scientifically interesting but also Press releases reach several hundred If you have scientific results that invite curiosity or novelty (i.e. O2 on you believe have popular interest, we news reporters and science journalists the moon Europa) are here to help you communicate your internationally, through direct mail, 9. Yield images that are visually findings to an information-hungry Internet, and FAX transmissions. striking and have aesthetic appeal, public. Because most people are NASA and ESA co-release much even though there is no new science unfamiliar with astronomical terms of this material to their respective (i.e. interior of the Orion nebula) and concepts, science reporting mailing lists. Results are also posted requires a great deal of explanation on SpaceLink, NASA’s computer and simplification. We provide a full bulletin board. Pathway to issuing a News Release range of services intended to generate Video news releases are mailed If you have results that you feel might clear, accurate and timely news directly to all major networks to be be of interest to the public: coverage of Hubble’s latest findings. edited into televised reports. 1. Call Ray Villard (Public Information Our Internet home page allows Manager) at (410) 338-4514 or send e- What we can do for you millions of people to directly access mail to [email protected] to discuss the Science Communication Hubble images, spectra, animation and results and the data. We translate scientific findings into news information independently from 2. Following a telephone interview, we concise, accurate and understandable traditional news sources. will e-mail to you a draft news release, press releases and background A variety of outside educational photo caption, and sample image for informational material for the news products incorporate our information final review and approval. We will media and public. and images including slide sets, work with you to develop graphics to posters, color newsletters, educational further clarify and explain your results. Image Processing video and CD-ROMs. This material is 3. We will coordinate with you and We format and layout HST images for available to educators, planetariums your home university public informa- reproduction as photographic prints, and science museums. tion office to set a date for release. slides, and electronic files. Typically, one month is required to prepare a press kit, so it’s important Science Visualization Some General Guidelines that we be contacted well in advance of We create science illustration of results Your research has genuine news value a publication or conference deadline. and prepare simplified diagrams. We if your results: The press release date will usually use state-of-art computer animation for 1. Represent a major discovery of a coincide with acceptance of your showing astronomical concepts that new phenomena or class of object (i.e. research for publication in a science involve temporal changes, spatial brown dwarfs), or are so significant journal. You might also be asked to relationships or three-dimensional they decisively clarify a mystery or participate in a televised press structure. controversy in astronomy. conference broadcast from NASA 2. Present a new mystery or unex- Headquarters in Washington, D.C. Video Production pected new complexity to a known 4. Following the release we can We produce video news releases phenomena (i.e. observations of provide you with a bibliography of including animation, diagrams and “naked” quasars). newspapers that carried the story. interviews with the principal investiga- 3. Are a significant step forward in a tor. This product provides all the specific research area (i.e. refined Special Circumstances elements a TV news station needs to value for the Hubble constant). If your results warrant announcement prepare a report for broadcast. 4. Are an incremental but important in an IAU telegram, please contact us step forward in knowledge in a given before issuing a telegram. Under News Coordination area (i.e. new structure in the Beta special circumstances we can prepare We work with your home university Pictoris disk). and distribute a press release within 24 press office to simultaneously release 5. Set a new astronomical record or hours of notification. In the absence of news of your research. If your results benchmark (i.e. the farthest known a press release only a few reporters 16 October 1995 will pick up on the IAU circular, and way, inadvertently, science is taught. concept, which was to be introduced in this will diminish chances for broad The scientists’ version is “Science is a future class. news coverage. Also it is more likely a the continuing search for underlying The workshop was attended by reporter will get the facts wrong commonalities in apparently disparate STScI staff, including Director Bob without a release that provides a full phenomena. Science is an intense Williams, and by NASA Headquarters explanation and background. engagement with things that arouse staff as well as staff from Goddard curiosity in us.” The student version is Space Flight Center. Another one-day News Exclusives “There is something called Science, in workshop is planned for the late fall. Researchers sometimes are contacted which I am told what to see, what to To request more information, contact by reporters from individual magazines know, and what to think. This Science [email protected]. who request data for immediate is rather unrelated to my world, so I publication. In the spirit of fair play, give up using and trusting my senses.” please defer such requests by telling Dr. Worth and Dr. Lopez presented a the reporter that they will have to wait picture of education as a dialogue, Hubble Postdoctoral for a formal news release. Giving such where the students learn by experienc- Fellowship Program exclusives diminishes chances that ing the concepts. In the workshop’s by Howard Bond your results will be picked up by the hands-on exercise, Investigating The Space Telescope Science mainstream news media. Floating and Sinking, the underlying, Institute announces the continuation of complex concept that was being the Hubble Postdoctoral Fellowship introduced — that of density — was Program, in cooperation with astro- ST ScI Education not mentioned. The exercise was nomical institutions throughout the Awareness Workshop designed to give the students the United States. The main objective of experience necessary to understand the The saying, “Tell me, I may listen. Show me, I may understand. Involve me, I will learn” aptly captures the changes taking place in science education. There are new curriculum standards. New teaching methods. More schools have computer labs and some are even on-line. There may not be much about a schoolroom we would recognize from our own experiences, but some things don’t change. Students still need exposure to the excitement of scientific discovery and role models. It is important for astronomers to get involved in science education, so it is important to understand today’s classroom and how we can best contribute. STScI held the first in a series of one day workshops aimed at educating astronomers about the process of education. The workshop was moderated by Ramon Lopez, the Director of Education and Outreach at the American Physical Society, and Karen Worth, a Senior Associate at the Workshop attendees (seated left to right) Marie Wicks, Baltimore City Materials Manager, Educational Development Center in Ethan Schreier, Associate Director, STScI, Julian Parks, Teacher, Baltimore City College High Boston. Attendance was limited to School, FUSE Science Outreach, Karen Worth, Workshop Co-moderator, Science Associate, classroom size to encourage dialogue, Educational Development Center, John Wood, Astronomer, GSFC, Anuradha Koratkar, Astrono- and the agenda included a demonstra- mer, STScI, (standing) Ramon Lopez, Workshop Co-moderator, Director of Outreach, American tion hands-on activity. Physical Society Dr. Worth introduced two definitions of science — one is the way scientists perform science, and the other is the 17 SpaceST ScI NewsletterTelescope Science • Institute Institute News • Newsletter

the Program is to provide opportunities September 1996 should send a letter SEBASTIANO LIGORI joined the for postdoctoral research on problems specifying the suggested period for the Institute on April 3, 1995 as a Graduate that are broadly related to the scientific visit and any other relevant details to Student. mission of the Hubble Space Tele- the Visiting Scientist Program, c/o scope, and compatible with the Nino Panagia ([email protected]) at BRIAN McLEAN was promoted to interests of the host institutions. The STScI. Applicants should also include Scientist on June 1995. program is open to applicants of any a statement of research plans and a KEITH NOLL transferred to the nationality, who have earned (or will copy of their curriculum vitae. WFPC2 group as Instrument Scientist/ have earned) their doctoral degrees on Applications received by November 1, Assistant Astronomer, effective June 1, or after January 1, 1993, in astronomy, 1995, will receive full consideration 1995. physics, or related disciplines. for visits planned in the academic year The duration of the Fellowships is 1996-97. ROCÍO PATIÑO KATSANIS joined for a total of three years, which Confirmed sabbatical visitors for the the General Support Pool in SSD as a includes an initial appointment of two academic year 1995-96 include Henny Data Analyst on September 5, 1995. years and an extension to a third year, Lamers (University of Utrecht), Tom contingent on a positive mid-term Wilson (Max-Planck-Institute für SAMANTHA OSMER transferred to review. Subject to availability of Radioastronomie, Bonn) and Ronald the General Support Pool in SSD as a funding from NASA, up to 8-10 new Webbink (University of Illinois). Data Analyst on September 11, 1995. Hubble Fellows will be appointed this KAILASH SAHU joined the Institute year, through grants to United States on August 10, 1995 as STIS Instru- institutions. Recent Staff Changes ment Scientist/Assistant Astronomer. The Announcement of Opportunity, including the detailed application ROBIN AUER transferred to the RITA SAMBRUNA, left the Institute instructions and forms, may be Servicing Mission Office as Adminis- on May 31, 1995 for a position in the obtained by writing to the Hubble trative Secretary, on June 26, 1995. Laboratory of High Energy Physics at Fellowship Program Office at STScI at GSFC. [email protected]. Information is RAYMUNDO BAPTISTA, left the also available at http://www.stsci.edu/ Institute on June 30, 1995 for a MASSIMO STIAVELLI joined the Hubble_fellow.html position at St. Andrews University. Institute on September 5, 1995 as a The application deadline is WFPC2 Instrument Scientist/Assistant KIRK BORNE, former Associate November 15, 1995. The new Hubble Astronomer. Scientist in the Archive Branch, left the Fellow appointments are expected to Institute on July 28, 1995 for a position begin on September 1, 1996. Women PETER STOCKMAN assumed the at NSSDC. and members of minority groups are role of Astronomer in SESD/Division Office as of June 1, 1995. strongly encouraged to apply. GARY BOWER, a former Postdoctoral Fellow, left the Institute on June 30, MEG URRY was granted tenure on 1995. He is now at the Johns Hopkins July 1995. Sabbatical Visitors at ST ScI University. DEBRA WALLACE transferred to the In order to promote exchange of GUIDO DeMARCHI, left on July 31, General Support Pool in SSD as a Data ideas and collaborations in HST- 1995 for a postdoctoral position at Analyst on September 11, 1995. related science, STScI expects to ESO. provide limited funds to support YIPING WANG, former Research visiting scientists who wish to spend MEGAN DONAHUE joined the Support Scientist in RPO, left the extended periods of time (typically Archive Branch as Archive Scientist/ Institute on April 21, 1995. three to six months) doing research at Assistant Astronomer on October 1, STScI. Typically the visitor is on 1995. HAL WEAVER, former Associate sabbatical leave from his or her home Astronomer in RPO, left the Institute HARRY FERGUSON joined WFPC2 institution. In general, these visitors on June 30, 1995. He is now a Senior group as Instrument Scientist/Assistant will have the status of STScI employ- Scientist at Applied Research Corp. Astronomer on September 1, 1995. ees and have access to the same ERIC WYCKOFF joined the Institute facilities available to staff members, GINA JONES, former Research on June 13, 1995 as a Data Analyst in including those at NCSA facilities. Assistant, left the Institute on July 28, the General Support Pool/SSD. Established scientists who might be 1995. interested in such a visit during the CHENG-YUE ZHANG, a former summer of 1996 or during the Postdoctoral Fellow, left the Institute academic year commencing in 18 on June 30, 1995. October 1995

Recent ST ScI Preprints

927. “HST Imaging of the Planetary Nebula K648 in M15” L. 942. “Nova Outbursts on Magnetic White Dwarfs” M. Livio. Bianchi, H. Ford, R. Bohlin, F. Paresce, G. De Marchi. 943. “White Dwarf Standard Stars: G191-B2b, GD 71, GD 153, 928. “Quasar Lyman Edge Regions in Polarized Light” A. HZ 43” R.C. Bohlin, L. Colina, D.S. Finley. Koratkar, R.R.J. Antonucci, R.W. Goodrich, H. Bushouse, A.L. Kinney. 944. “Unified Schemes for Radio-Loud Active Galactic Nuclei” C.M. Urry, P. Padovani. 929. “Towards Understanding the Fanaroff-Riley Dichotomy in Radio Source Morphology and Power” S.A. Baum, E.L. Zirbel, 945. “Implications of Non-Thermal Motions for Statistics of C.P. O’Dea. Lyman-Alpha Forest Clouds” V.P. Kulkarni, S.M. Fall.

930. “A Model for the Galactic Population of Symbiotic Stars 946. “Accreting, Isolated Neutron Stars: III. Preheating of with White Dwarf Accretors” L. Yungelson, M. Livio, A. Infalling Gas and Cometary H II Regions” O. Blaes, O. Warren, Tutukov, S.J. Kenyon. P. Madau.

931. “Low Mass Stars in Globular Clusters. II. The Mass 947. “Radio and Emission-Line Jets in the Type 2 Seyfert Function of M15” G. De Marchi, F. Paresce. Galaxy MKN 1066 (UGC 2456)” G. Bower, A. Wilson, J.A. Morse, R. Gelderman, M. Whittle, J. Mulchaey. 932. “Low Mass Stars in Globular Clusters. III. The Mass Function of 47 Tucane” G. De Marchi, F. Paresce. 948. “Software for the Analysis of Emission Line Nebulae” R.A. Shaw, R.J. Dufour. 933. “Compton Heating and Superthermal Electrons in Gamma-Loud Agns” A.M. Beloborodov, A.F. Illarionov. 949. “On the Origin of the FIR-Radio Relation in Active Galaxies” L. Colina, D. E. Perez-Olea. 934. “High Resolution Coronographic Imaging and Spectropolarimetry of the HR Carinae Nebula” M. Clampin, 950. “Evolutionary Models of the Radio Emission in Compact R.E. Schulte-Ladbeck, A. Nota, M. Robberto, F. Paresce, G.C. Starbursts” D. E. Perez-Olea, L. Colina. Clayton. 951. “Variable Stars in the Irregular Galaxy NGC 2366 (DDO 935. “High Resolution Far-Infrared Mapping of the Star- 42)” E. Tolstoy, A. Saha, J. G. Hoessel, K. McQuade. Forming Region RCW 122C” C.Y. Zhang, P.M. Harvey, B.J. 952. “Constraints on the Extragalactic Background Light from Smith, C. Colome, J. DiFrancesco. Gamma-Ray Observations of High Redshift Quasars” P. 936. “The Calibration of Novae as Distance Indicators” M. Madau, E.S. Phinney. Della Valle, M. Livio 953. “Spectroscopy of Poorly-Studied Cataclysmic Variables” 937. “Consequences of Dust in Damped Lyman-Alpha R. Downes, D.W. Hoard, P. Szkody, S. Wachter. Systems” S.M. Fall, Y.C. Pei. 954. “Environmental Properties of BL LAC Objects” J.E. 938. “Core Properties of Elliptical Galaxies: A Northern Pesce, R. Falomo, A. Treves. Hemisphere Sample at High Resolution” P. Møller, M. Stiavelli, 955. “Evidence for an Obscured Quasar in the Giant Radio W.W. Zeilinger. Galaxy PKS 0634-205” C. Simpson, M.J. Ward, A.S. Wilson. 939. “Scattering Properties of the Dust in the Reflection Nebula 956. “Nuclear Disks of Gas and Dust in Fanaroff-Riley Type I IC 435” D. Calzetti, R.C. Bohlin, K.D. Gordon, A.N. Witt, L. Radio Host Galaxies: 3C 402N and NGC 7052” L. de Juan, L. Bianchi. Colina, D. Golombek. 940. “The Evolution of Lithium Abundances of Solar-Type 957. “Discovery of an Optical Synchrotron Jet in 3C 78” W.B. Stars. V. K Dwarfs in the Hyades” D.R. Soderblom, B.F. Jones, Sparks, D. Golombek, S.A. Baum, J. Biretta, S. de Koff, F. J.R. Stauffer, B. Chaboyer. Machetto, P. McCarthy, G.K. Miley. 941. “The Intercomparison of Star Catalogs III: Comparing the 958. “The Lyman Continuum in Starburst Galaxies Observed AGK3, the AGK3U, the ACRS (part 1), and the PPM to the with the Hopkins Ultraviolet Telescope” C. Leitherer, H.C. GC” D. Daou, J.E. Morrison, L.G. Taff. Ferguson, T.M. Heckman, J.D. Lowenthal.

19 ST ScI Newsletter • Institute News

Recent ST ScI Preprints Continued HST Related Publications

959. “O Stars in Transition. I. Optical Spectroscopy of the The following is a list of papers based on HST observations that OFPE/WN9 and Related Stars” A. Nota, A. Pasquali, L. have appeared in refereed journals since the last Newsletter. Drissen, C. Leitherer, C. Robert, A.F.J. Moffat, W. Scmutz. This list is maintained by the ST ScI Library ([email protected]) to which corrections and additions should 960. “Cosmic Metal Production and the Contribution of QSO be sent. Please remember that supplying the ST ScI Librarian Absorption Systems to the Ionizing Background” P. Madau, with preprints or reprints is a requirement for GO/AR grant J.M. Shull. recipients and strongly encouraged for everyone else as well.

961. “Dynamo Driven Accretion Discs and Dwarf Nova Atreya, S.K.; Edgington, S.G.; Trafton, L.M.; Caldwell, J.J.; Eruptions” P.J. Armitage, M. Livio, J.E. Pringle. Noll, K.S.; Weaver, H.A. “Abundances of ammonia and carbon disulfide in the Jovian stratosphere following the impact of 962. “Cataclysmic Variables in Globular Clusters” M. Livio. comet Shoemaker-Levy 9” Geophys. Res. Lett. 22: 1625-1628, 963. “Dust Obscuration in Starburst Galaxies from Near- 1995 Infrared Spectroscopy” D. Calzetti, A.L. Kinney, T. Storchi- Bahcall, J.N.; Kirhakos, S.; Schneider, D.P. “PKS 2349-014: a Bergmann. luminous quasar with thin wisps, a large off-center nebulosity, 18 and a close companion galaxy” ApJ 447: L1-L4, 1995 964. “Detection of H2 O in Jupiter” K.S. Noll, R.R. Gerballe, R.F. Knacke. Baptista, R.; Horne, K.; Hilditch, R.W.; Mason, K.O.; Drew, 965. “Accreting White Dwarfs and Type Ia Supernovae” M. J.E. “Hubble Space Telescope and R-band eclipse maps of the Livio, D. Branch, L.R. Yungelson, F. Boffi, E. Baron. UX Ursa Majoris accretion disk” ApJ 448: 395-415, 1995

Barcons, X.; Lanzetta, K.M.; Webb, J.K. “Extensive dark- matter haloes in low-luminosity galaxies revealed by quasar absorption lines” Nature 376: 321-323, 1995

Ben Jaffel, L.; Leers, V.; Sandel, B.R. “Dark auroral oval on Saturn discovered in Hubble Space Telescope images” Science 269: 951-953, 1995

Bernacca, P.L.; Lattanzi, M.G.; Porro, I.; Neuhauser, R.; Bucciarelli, B. “Hubble Space Telescope astrometric observa- tions of pre-main sequence stars from the Hipparcos Program. ST-ECF II” A&A 299: 933-939, 1995

Bobrowsky, M.; Zijlstra, A.A.; Grebel, E.K.; Tinney, C.G.; Te Newsletter Lintel Hekkert, P.; Van De Steene, G.C.; Likkel, L.; Bedding, T.R. “He 3-1475 and its jets” ApJ 446: L89-L92, 1995 The Space Telescope — European Coordinating Facility publishes a quarterly Borkowski, K.J.; Harrington, J.P.; Tsvetanov, Z. “Interaction of newsletter which, although aimed principally at a stellar wind with clumpy stellar ejecta in A30” ApJ 449: European Space Telescope users, contains articles of L143-L147, 1995 general interest to the HST community. If you wish to be included in the mailing list, please contact the Bowen, D.V.; Blades, J.C.; Pettini, M. “The distribution of editor and state your affiliation and specific involve- metal-absorbing high velocity clouds in the galaxy” ApJ 448: ment in the Space Telescope Project. 662-666, 1995 Robert Fosbury (Editor) Space Telescope — European Coordinating Facility Bowen, D.V.; Blades, J.C.; Pettini, M. “Interstellar Mg II absorption lines from low-redshift galaxies” ApJ 448: 634-661, Karl Schwarzschild Str. 2 1995 D-85748 Garching bei München Federal Republic of Germany Bower, G.A.; Wilson, A.S. “Hubble Space Telescope images of E-Mail: [email protected] the nuclear star forming region in the interacting galaxy NGC 5930” ApJS 99: 543-549, 1995

20 October 1995

HST Related Publications Continued

Boyd, P.T.; Van Citters, G.W.; Dolan, J.F.; Wolinski, K.G.; Elson, R.A.W.; Gilmore, G.F.; Santiago, B.X.; Casertano, S. Percival, J.W.; Bless, R.C.; Elliot, J.L.; Nelson, M.J.; Taylor, “HST observations of the stellar population of the globular M.J. “High-Speed Photometer observations of the LMC pulsar cluster omega Cen” AJ 110: 682-692, 1995 B0540-69” ApJ 448: 365-368, 1995 Federman, S.R.; Cardelli, J.A.; Van Dishoeck, E.F.; Lambert, Brandt, J.C.; Heap, S.R.; Beaver, E.A.; Boggess, A.; Carpenter, D.L.; Black, J.H. “Vibrationally excited H2, HCl, and NO+ in K.G.; Ebbets, D.C.; Hutchings, J.B.; Jura, M.; Leckrone, D.S.; the diffuse clouds towards Zeta Ophiuchi” ApJ 445: 325-329, Linsky, J.L.; Maran, S.P.; Savage, B.D.; Smith, A.M.; Trafton, 1995 L.M.; Walter, F.M.; Weymann, R.J.; Snow, M.; Randall, C.E.; Ake, T.B.; Robinson, R.D.; Wahlgren, G. “An atlas of Alpha Ferlet, R.; Lecavelier Des Etangs, A.; Vidal-Madjar, A.; Bertin, Orionis obtained with the Goddard High Resolution Spec- P.; Deleuil, M.; Lagrange-Henri, A.-M.; Lallement, R. “HST- trograph on the Hubble Space Telescope” AJ 109: 2706-2735, GHRS observations of alpha Piscis Austrini” A&A 297: L5-L8, 1995 1995

Capetti, A.; Axon, D.J.; Macchetto, F.; Sparks, W.B.; Forbes, D.A.; Franx, M.; Illingworth, G.D. “Ellipticals with Boksenberg, A. “HST imaging polarimetry of NGC 1068” ApJ kinematically-distinct cores: WFPC1 imaging of nearby 446: 155-166, 1995 ellipticals” AJ 109: 1988-2002, 2278-2279, 1995

Capetti, A.; Macchetto, F.; Axon, D.J.; Sparks, W.B.; Fullton, L.K.; Carney, B.W.; Olszewski, E.W.; Zinn, R.; Boksenberg, A. “The morphology of the narrow line region of Demarque, P.; Janes, K.A.; Da Costa, F.S.; Seitzer, P. “A VI(c) Markarian 3” ApJ 448: 600-610, 1995 color-magnitude diagram of the globular cluster NGC 6352 from Hubble Space Telescope planetary camera observations” Carpenter, K.G.; Robinson, R.D.; Judge, P.G. “GHRS observa- AJ 110: 652-681, 946-947, 1995 tions of cool, low-gravity stars. II. Flow and turbulent velocities in the outer atmosphere of gamma Crucis (M3.4 III)” ApJ 444: Garnett, D.R.; Dufour, R.J.; Peimbert, M.; Torres-Peimbert, S.; 424-437, 1995 Shields, G.A.; Skillman, E.D.; Terlevich, E.; Terlevich, R.J. “Si/ O abundance ratios in extragalactic H II regions from Hubble Clarke, J.T.; Lallement, R.; Bertaux, J.-L.; Quemerais, E. Space Telescope UV spectroscopy” ApJ 449: L77-L81, 1995 “HST/GHRS observations of the interplanetary medium downwind and in the inner solar system” ApJ 448: 893-904, Gilliland, R.L.; Edmonds, P.D.; Petro, L.; Saha, A.; Shara, 1995 M.M. “Stellar variability in the central populations of 47 Tucanae from WF/PC observations with the Hubble Space Clayton, G.C.; Wolff, M.j.; Allen, R.G.; Lupie, O.L. “Ultravio- Telescope. I. Project overview, reduction techniques, and first let interstellar linear polarization. II. The wavelength depen- results” ApJ 447: 191-203, 1995 dence” ApJ 445: 947-957, 1995 Glazebrook, K.; Ellis, R.; Santiago, B.; Griffiths, R. “The Deharveng, J.-M.; Buat, V.; Bergeron, J. “Lyman alpha morphological identification of the rapidly evolving population emission from galaxies: the case of absorption line selected of faint galaxies” MNRAS 275: L19-L22, 1995 galaxies at z ~ 0.3 - 0.4” A&A 298: 57-62, 1995 Hammel, H.B.; Lockwood, G.W.; Mills, J.R.; Barnet, C.D. Disney, M.J.; Boyce, P.J.; Blades, J.C.; Boksenberg, A.; Crane, “Hubble Space Telescope imaging of Neptune’s cloud structure P.; Deharveng, J.M.; Macchetto, F.; Mackay, C.D.; Sparks, in 1994" Science 268: 1740-1742, 1995 W.B.; Phillipps, S. “Interacting elliptical galaxies as hosts of intermediate-redshift quasars” Nature 376: 150-153, 1995 Hester, J.J.; Scowen, P.A.; Sankrit, R.; Burrows, C.J.; Gallagher, J.S. III; Holtzman, J.A.; Watson, A.; Trauger, J.T.; Driver, S.P.; Windhorst, R.A.; Ostrander, E.J.; Keel, W.C.; Ballester, G.E.; Casertano, S.; Clarke, J.T.; Crisp, D.; Evans, Griffiths, R.E.; Ratnatunga, K.U. “The morphological mix of R.W.; Griffiths, R.E.; Hoessel, J.G.; Krist, J.; Lynds, R.; Mould, field galaxies to m(I) = 24.25 magnitudes b(j) =26˜ magnitudes) J.R.; O’Neil, E.J. Jr.; Stapelveldt, K.R.; Westphal, J.A. “WFPC2 from a deep Hubble Space Telescope WFPC2 image” ApJ 449: studies of the Crab Nebula: I. HST and ROSAT imaging of the L23-L27, 1995 synchrotron nebula” ApJ 448: 240-263, 1995

21 STSpace ScI NewsletterTelescope Science • Institute Institute News • Newsletter

HST Related Publications Continued

Hunter, D.A.; Shaya, E.J.; Holtzman, J.A.; Light, R.M.; O’Neil, Marsh, T.R.; Wood, J.H.; Horne, K.; Lambert, D. “The E.J. Jr.; Lynds, R. “The intermediate stellar mass population in discovery of high-velocity flares inN v and the detection of R136 determined from Hubble Space Telescope Planetary carbon in the double degenerate binary GP Com” MNRAS 274: Camera 2 images” ApJ 448: 179-194, 1995 452-460, 1995

Hunter, D.A.; Shaya, E.J.; Scowen, P.; Hester, J.J.; Groth, E.J.; Mason, K.o.; Drew, J.e.; Cordova, F.a.; Horne, K.; Hilditch, R.; Lynds, R.; O’Neil, E.J. Jr. “Gas near the center of 30 Doradus Knigge, C.; Lanz, T.; Meylan, T. “Eclipse observations of an as revealed by Hubble Space Telescope images” ApJ 444: 758- accretion disc wind” MNRAS 274: 271-286, 1995 764, 1995 Mould, J.; Huchra, J.R.; Bresolin, F.; Ferrarese, L.; Ford, H.C.; Im, M.; Ratnatunga, K.U.; Griffiths, R.E.; Casertano, S. “The Freedman, W.L.; Graham, J.; Harding, P.; Hill, R.; Hoessel, axis ratio distribution of faint galaxies: evidence for a popula- J.G.; Hughes, S.M.; Illingworth, G.D.; Kelson, D.; Kennicutt, tion of dwarf galaxies at I ~ 20.5” ApJ 445: L15-L18, 1995 R.C. Jr.; Madore, B.F.; Phelps, R.; Stetson, P.B.; Turner, A. “Limits on the Hubble constant from the HST distance of Jackson, N.; Sparks, W.B.; Miley, G.K.; Macchetto, F. “HST M100” ApJ 449: 413-421, 1995 observations of 3C 305” A&A 296: 339-346, 1995 Netzer, H.; Brotherton, M.S.; Wills, B.J.; Han, M.; Wills, D.; Johansson, S.; Brage, T.; Leckrone, D.S.; Nave, G.; Wahlgren, Baldwin, J.A.; Ferland, G.J.; Browne, I.W.A. “The Hubble G.M. “Interpretation of anomalous ultraviolet transitions of Fe Space Telescope sample of radio-loud quasars: the Ly alpha/H II observed in laboratory Fourier transform spectra and stellar beta ratio” ApJ 448: 27-40, 1995 HST and IUE spectra” ApJ 446: 361-370, 1995 Neuschaefer, L.W.; Ratnatunga, K.U.; Griffiths, R.E.; Valdes, F. Kim, Y.H.; Caldwell, J.J.; Fox, J.L. “High-resolution ultraviolet “Detection, photometry and completeness of FOCAS catalogs spectroscopy of Jupiter’s aurora with the Hubble Space for the HST Medium Deep Survey” PASP 107: 590-599, 1995 Telescope” ApJ 447: 906-914, 1995 O’Connell, R.W.; Gallagher, J.S. III; Hunter, D.A.; Colley, Krist, J.E.; Burrows, C.J. “Phase retrieval analysis of pre- and W.N. “Hubble Space Telescope imaging of super star clusters in post-repair Hubble Space Telescope images” Appl. Opt. 34: M82” ApJ 446: L1-L4, 1995 4951-4964, 1995 Paresce, F. “HST observations of high density globular cluster Lagrange, A.M.; Vidal-Madjar, A.; Deleuil, M.; Emerich, C.; cores” Mem. Soc. Astron. Ital. 65: 713-721, 1994 Beust, H.; Ferlet, R. “The Beta Pictoris circumstellar disk. XVII. Physical and chemical parameters of the disk” A&A 296: Paresce, F.; Livio, M.; Hack, W.; Korista, K. “The structure and 499-508, 1995 evolution of the nova V1974 Cygni shell from HST observa- tions” A&A 299: 823-834, 1995 Lanz, T.; Heap, S.R.; Hubeny, I. “HST/GHRS observations of the beta Pictoris system: basic parameters and the age of the Parker, J.M.; Heap, S.R.; Malumuth, E.M. “Identification of system” ApJ 447: L41-L44, 1995 emission-line stars in 30 Doradus using HST observations” ApJ 448: 705-714, 1995 Laor, A.; Bahcall, J.N.; Jannuzi, B.T.; Schneider, D.P.; Green, R.F. “The ultraviolet emission properties of 13 quasars” ApJS Percival, J.W.; Boyd, P.T.; Biggs, J.D.; Dolan, J.F.; Bless, R.C.; 99: 1-26, 1995 Elliot, J.L.; Nelson, M.J.; Robinson, E.L.; Taylor, M.J.; Van Citters, G.W.; Wolinski, K.G. “A search for a pulsar in the Longair, M.S.; Best, P.N.; Rottgering, H.J.A. “HST observa- remnant of SN 1987A with the Hubble Space Telescope High tions of three radio galaxies at redshift z~=1” MNRAS 275: Speed Photometer” ApJ 446: 832-837, 1995 L47-L51, 1995 Phillips, A.C.; Bershady, M.A.; Forbes, D.A.; Koo, D.C.; Lyu, C.-H.; Bruhweiler, F.C.; Smith, A.M. “Tomography/power Illingworth, G.D.; Reitzel, D.B.; Griffiths, R.E.; Windhorst, spectrum techniques for removal of fixed pattern noise from R.A. “Structure and photometry of an I < 20.5 galaxy sample Hubble Space Telescope spectra” ApJ 447: 880-888, 1995 from the Hubble Space Telesope medium deep survey” ApJ 444: 21-40, 1995

22 October 1995

HST Related Publications Continued

Rao, S.M.; Turnshek, D.A.; Briggs, F.H. “The incidence of Thomson, R.C.; Crane, P.; Mackay, C.D. “Optical structure and damped Ly alpha systems in the redshift interval 0 < z < 4” ApJ polarization of the western hot spot of Pictor A” ApJ 446: L93- 449: 488-496, 1995 L95, 1995

Roth, K.C.; Blades, J.C. “An HST archival study of galactic Wahlgren, G.M.; Leckrone, D.S.; Johansson, S.G.; Rosberg, interstellar zinc and chromium” ApJ 445: L95-L98, 1995 M.; Brage, T. “The abundances of Pt, Au, and Hg in the chemically peculiar HgMn-type stars kappa Cancri and chi Sartoretti, P.; McGrath, M.A.; McEwen, A.S.; Spencer, J.R. Lupi” ApJ 444: 438-451, 1995 “Post-Voyager brightness variations on Io” JGR 100: 7523- 7530, 1995 Walter, F.M.; Matthews, L.D.; Linsky, J.L. “New insights into nonradiative heating in late A star chromospheres” ApJ 447: Savage, B.D.; Sembach, K.R.; Lu, L. “Probing the galactic disk 353-363, 1995 and halo. III. The galactic and intergalactic sight line to H1821+643” ApJ 449: 145-155, 1995 Weiland, J.L.; Shore, S.N.; Beaver, E.A.; Lyons, R.W.; Rosenblatt, E.I. “Goddard High-Resolution Spectrograph Shara, M.M.; Drissen, L. “Cataclysmic and close binaries in observations of the interacting binary system W Serpentis” ApJ star clusters. III. Recovery of the quiescent nova 1860 A.D. (T 447: 401-407, 1995 Scorpii) in the core of the globular cluster M80” ApJ 448: 203- 206, 1995 Welty, D.E.; Hobbs, L.M.; Lauroesch, J.T.; Morton, D.C.; York, D.G. “Interstellar lead” ApJ 449: L135-L138, 1995 Sion, E.M.; Huang, M.; Szkody, P.; Cheng, F-H. “Hubble Space Telescope high-resolution spectroscopy of the exposed white Werner, K.; Dreizler, S.; Wolff, B. “Spectral analysis of the hot dwarf in the dwarf nova VW Hydri in quiescence: a rapidly DO white dwarf PG 1034+001” A&A 298: 567-576, 1995 rotating white dwarf” ApJ 445: L31-L34, 1995 Wills, B.J.; Thompson, K.L.; Han, M.; Netzer, H.; Wills, D.; Sion, E.M.; Szkody, P.; Cheng, F-H.; Huang, M. “A Hubble Baldwin, J.A.; Ferland, G.I.; Browne, I.W.A.; Brotherton, M.S. Space Telescope study of the underlying white dwarf in the “The Hubble Space Telescope sample of radio-loud quasars: dwarf nova VW Hydri during quiescence” ApJ 444: L97-L100, ultraviolet spectra of the first 31 quasars” ApJ 447: 139-158, 1995 1995

Smith, P.S.; Schmidt, G.D.; Allen, R.G.; Angel, J.R.P. “The Windhorst, R.A.; Fomalont, E.B.; Kellermann, K.I.; Partridge, polarization and ultraviolet spectrum of Markarian 231” ApJ R.B.; Richards, E.; Franklin, B.E.; Pascarelle, S.M.; Griffiths, 444: 146-156, 1995 R.E. “Identifications of faint radio sources with optically luminous interacting disk galaxies” Nature 375: 471-474, 1995 Spitzer, L. Jr.; Fitzpatrick, E.L. “Composition of interstellar clouds in the disk and halo. III. HD 149881” ApJ 445: 196-210, 1995

Stapelfeldt, K.R.; Burrows, C.J.; Krist, J.E.; Trauger, J.T.; Hester, J.J.; Holtzman, J.A.; Ballester, G.E.; Casertano, S.; Clarke, J.T.; Crisp, D.; Evans, R.W.; Gallagher, J.S. III; Griffiths, R.E.; Hoessel, J.G.; Mould, J.R.; Scowen, P.A.; Watson, A.M.; Westphal, J.A. “WFPC2 imaging of the circumstellar nebulosity of HL Tauri” ApJ 449: 888-893, 1995

Stern, S.A.; Trafton, L.M.; Flynn, B. “Rotationally resolved studies of the mid-ultraviolet spectrum of Triton. II. HST surface and atmospheric results” AJ 109: 2855-2868, 1995

Sulentic, J.W.; Marziani, P.; Dultzin-Hacyan, D.; Calvani, M.; Moles, M. “First direct comparison of high and low ionization line kinematics in active galactic nuclei” ApJ 445: L85-L89, 1995

23 Contents How to contact ST ScI All services and most of the documentation provided by STScI can be Science News found at: Atomic Physics with the http://www.stsci.edu Goddard High Resolution Spectrograph ...... 1 Director's Perspective ...... 2 by sending mail to [email protected] GHRS Archival Spectra of or calling +1-410-338-1082 Interstellar Zinc and Chromium ...... 4 Additionally, documentation and support can be requested at: The Hubble Deep Field project ...... 5 WFPC2 UV Parallel Survey ...... 7 Phase I [email protected] HST Data Archive [email protected] New Methods of Observing for the 21st Century...... 7 Instrument Information: http://www.stsci.edu/instruments.html STSDAS http://ra.stsci.edu/STSDAS.html HST Observatory

Scientific Instruments Status ...... 9 Any questions about the scheduling of your observations should be Hubble Data Archive News ...... 9 addressed to your Program Coordinator. After program execution, you STIS Hardware Status ...... 10 can always contact your Contact Scientist. PRESTO’s Mosaic page NICMOS Status ...... 10 (http://presto.stsci.edu/public/propinfo.html) contains that informa- tion, if you do not know who these persons are. Manifest for the Servicing Mission 1997 ...... 11 Filter choice for the Advanced Camera for Surveys ...... 11

Observers and Proposers Cycle 6 Proposal Selection Schedule ...... 13 Newsletter Notes General Observer/Archival Researcher Funding ...... 13 Comments, suggestions and mailing list corrections can be HST Long-Range Observing Plan addressed to the Editors, Daniel Golombek (+1-410-338-4974, Now Available via the World Wide Web ...... 13 [email protected]) or Helmut Jenkner (+1-410-338-4842, [email protected]). AURA News Design and Layout: John Godfrey. Welcome New Members...... 14 The STScI Newsletter is issued by the Space Telescope Science Key AURA Committees ...... 14 Institute, which is operated by the Association of Universities for Institute News Research in Astronomy, Inc., for the National Aeronautics and Space Administration. Office of Public Outreach ...... 15 Time for a Good IDEA ...... 15 Keeping the Public Tuned-in to Hubble’s Discoveries ...... 15 ST ScI Education Awareness Workshop ...... 17 NON PROFIT SPACE U.S. POSTAGE Hubble Postdoctoral Fellowship Program ...... 17 TELESCOPE PAID Sabbatical Visitors at ST ScI ...... 18 SCIENCE PERMIT NO. 8928 Recent Staff Changes...... 18 INSTITUTE BALTIMORE MD Recent ST ScI Preprints...... 20 HST Related Publications...... 20 How to contact ST ScI ...... 24 Newsletter Notes...... 24

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