HUBBLE SPACE TELESCOPE DAILY REPORT # 3133 PERIOD COVERED: DOY 158-160: 0000Z (UTC) 06/07/02 - 0000Z (UTC) 06/09/02 OBSERVATIONS SCHEDULED AND ACCOMPLISHED: 9353 Direct imaging of the progenitors of massive, core-collapse supernovae Modern supernovae searches in the nearby Universe are discovering vast numbers of SNe which have massive star progenitors {Types II, Ib and Ic}. The extensive HST {and ground-based} image archives of galaxies within ~20 Mpc enables their individual bright stellar content to be resolved. As massive, evolved stars are the most luminous single objects in a galaxy, the progenitors of core-collapse SNe should be directly detectable on pre-explosion images. Within the last year we have set direct mass limits on the progenitors of two SNe Type II-P by analyzing pre-explosion archive images and follow up HST exposures. We have now identified six other recent, nearby SNe which have WFPC2 archive exposures of the site taken before explosion. Additionally, our Cycle 10 SNAP program will double the WFPC2 image archive of nearby galaxies which significantly increases the chances of having multi-colour photometry of pre-explosion sites for future SNe. In this Cycle, we request time on two fronts. Firstly we require imaging of the six SNe with existing pre-explosion data in order to perform exact astrometry of the SNe positions to around 0.05''. Secondly, as a follow on from our two successful Cycle 10 programs, we request ToO status for any nearby core-collapse SN which explodes during Cycle 11 and which has pre-explosion HST images. The goal of this proposal is to directly identify the progenitor stars of core-collapse SNe. ACS 9027 ACS SBC Geometric Distortion Calibration This activity will obtain a series of images to evaluate the geometric distortion over the field of view of the ACS SBC channel, after its image quality has been optimized with the corrector mechanism. Images will be obtained in filter F125LP, with a pattern of POS-TARG offsets in each axis. These data will be complemented by the images of the same field obtained in proposal 9024, "ACS SBC Flat Field Strability", which utilizes a similar image offsetting technique at larger spatial scales. The observations may be scheduled back-to-back with those from proposal 9024. NGC 6681 {18.7 h, -32 deg} will be the target, as this star field has been used extensively by the STIS program for UV PSF measurement and photometry ACS 9476 Galaxy Evolution in the Richest Clusters at z=0.8: the EDisCS Cluster Sample The study of distant cluster galaxies requires two key ingredients: {1} deep high-resolution imaging, to constrain galaxy structure; and {2} 8m-class spectroscopy, to measure stellar content, star-formation rates, dynamics, and cluster membership. We will reach both conditions with the addition of HST/ACS imaging to our suite of VLT {36 nights} and NTT {20 nights} observations of 10 confirmed clusters at z~0.8, drawn from the ESO Distant Cluster Survey {EDisCS}. The proposed HST/ACS data will complement our existing optical/IR imaging and spectroscopy with quantitative measures of cluster galaxy morphologies {i.e. sizes and shapes, bulge-disk decompositions, asymmetry parameters}, and with measurements of cluster masses via weak lensing. Major advantages unique to the EDisCS project include: {i} uniform selection of clusters; {ii} large enough sample sizes to characterize the substantial cluster-to-cluster variation in galaxy populations; {iii} large quantities of high quality data from 8m telescopes; {iv} uniform measurements of morphologies, spectroscopic and photometric redshifts, SEDs, star-formation/AGN activities, and internal kinematics; {v} optical selection of clusters to complement the X-ray selection of almost all high-z clusters in the ACS GTO programs; {vi} forefront numerical simulations designed specifically to allow physical interpretation of observed differences between the high-z and local clusters. ACS 9395 Is Bulge Formation Still Going-On? An ACS Survey of Pseudo-Bulges Pseudo-bulges, i.e., bulges with an exponential light profile, have been unveiled in the centers of many intermediate-type disks. Their structural similarity with the disks provides support to theoretical scenarios in which bulges may form due to secular evolution processes within the host disks. If at play, these processes would likely be active throughout a large fraction of cosmic history down to our days: `young' bulges should exist. Our previous HST WFPC2 and NICMOS survey of ~100 spirals has provided V-H colors for 11 Sb-Sc pseudo-bulges, and these could be interpreted as suggestive of relatively young stellar ages. Furthermore, dense nuclei have been discovered in these pseudo-bulges, and their V-H colors may imply stellar masses sufficiently large to activate the formation of the pseudo- bulge by means of dynamical dissolution of progenitor bars. However, the V-H color, on its own, is fully degenerate towards stellar ages, metallicities and masses, as well as dust content. We therefore propose to use ACS to observe the 11 pseudo-bulges of our combined WFPC2 and NICMOS sample in the F330W, F435W, and F814W filters. Extending the wavelength baseline to the bluer passbands is essential to break the mass-age-metallicity-dust degeneracy, and will provide far more accurate estimates for the stellar population properties of the pseudo-bulges and their nuclei. Proving the existence of `young' bulges in the local Universe would have a big impact in our understanding of the formation of the Hubble sequence. ACS 9024 SBC flat field uniformity The stability and uniformity of the low-frequency flat fields {L-flat} of all ACS detectors will be assessed by using multiple pointing observations of the globular cluster NGC6681 - thus imaging moderately dense stellar fields. By placing the same star over different portions of the detectors and measuring relative changes in its brightness it will be possible to determine local variations in the response of the detectors. Based on previous experience with STIS, it is deemed that a total of nine different pointings will suffice to provide adequate characterization of the flat field stability in any given band. For each filter to be tested, the baseline consists of 9 pointings with steps of ~20% of the FOV in a diagonal cross pattern. During SMOV, the complement of filters to be tested is limited to the following: for the SBC, F125LP and F150LP. In order to provide complementary data for the geometric distortion programmes {9027 and 9028}, and also to check that the distortion is not chromatic, three additional exposures will be taken with F125LP with a very small {~10 pixel} offset from the centre {see proposals 9027 and 9028}. Execution of this programme must await completion of programme 9011 {ACS to FGS alignment} and the ensuing PDB update. ACS/CAL 9558 ACS weekly Test This program consists of basic tests to monitor, the read noise, the development of hot pixels and test for any source of noise in ACS CCD detectors. This programme will be executed once a day for the entire lifetime of ACS. ACS/HRC 9473 Masses and IMF Variations in Super Star Clusters We are proposing to obtain high spatial resolution images of a set of super star clusters for which we have been granted observing time to measure velocity dispersions via high- resolution ground-based optical echelle and K-band spectroscopy. The images will allow us to fit the light profiles and measure the radii of the clusters, and when combined with the velocity dispersions, will enable us to estimate the cluster masses. By comparing the mass-to-light ratios with those predicted from spectral synthesis models, we will investigate possible variations in the slope and lower mass cut-offs of the initial mass functions in these clusters. Correlations of the variations of these parameters with cluster environment may provide insight into the formation mechanisms for super star clusters. By comparing the light profiles obtained in a blue and red filter, we will also search for evidence of mass segregation in the clusters. Since these clusters are too young to have experienced dynamical mass segregation, differences in the light profiles of the clusters in the two filters could be due to processes that differentiate between high and low mass stars during the birth of the clusters and would provide further constraints on theoretical models of cluster formation. Since these clusters are far too compact to be resolved by any ground-based observations, the ACS/HRC on board HST is the only instrument capable of carrying out these observations. ACS/HRC 9020 Preliminary ACS Sensitivity. The Advanced Camera for Surveys (HrC) was used to observe a spectrophotometric standard star through each filter of each camera to assess the sensitivity of the instrument. The star is placed at the center of the aperture, and two images are taken through each filter. ACS/WFC 9575 Default {Archival} Pure Parallel Program. The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels in POMS. ACS/WFC/HRC 8947 Weekly Test. The Advanced Camera for Surveys (WFC and HRC) was used to perform basic tests to monitor, the read noise, the development of hot pixels and test for any source of noise in ACS CCD detectors. This program will be executed at least once a day for the entire lifetime of ACS. FGS/1 9034 The Masses and Luminosities of Population II Stars. Fine Guidance Sensor 11R was used to observe the mass-luminosity relation {MLR} of Population II stars of which very little is currently known. With the advent of the Hipparcos Catalogue, improved distances to many spectroscopic binaries known to be Pop II systems are now available. After surveying the literature and making reasonable estimates of the secondary masses, we find 13 systems whose minimum separation should be larger than the resolution limit of FGS #1. NICMOS 9269 NICMOS Parallel Thermal Background NICMOS Camera 3 pure parallel exposures in the F222M filter will be obtained for the entire duration of SMOV to establish the stability of the HST+NCS+Instrument thermal emission. NICMOS 8986 NICMOS Photometry Test This proposal contains the necessary exposures to re-calibrate NICMOS. NICMOS 8790 NICMOS Post-SAA calibration - CR Persistence Part 1. A new procedure proposed to alleviate the CR-persistence problem of NICMOS. Dark frames will be obtained immediately upon exiting the SAA contour 23, and every time a NICMOS exposure is scheduled within 50 minutes of coming out of the SAA. The darks will be obtained in parallel in all three NICMOS Cameras. The POST-SAA darks will be non-standard reference files available to users with a USEAFTER date/time mark. STIS 9328 Comprehensive STIS Spectroscopy of the Supernova Remnant 1987A's Formation The visible consequences of the hard shock of the impact of SN 1987A's ejecta upon the inner circumstellar ring are apparent and developing rapidly. Over the past year, this phenomenon has made a transition, from emission originating in just a few "hot spots" at restricted locations in position angle {PA} around the ER, to a collision producing optical emission over a nearly continuous distribution {with few breaks larger than 45 degrees in PA} and indications of low-level emission arising from nearly all PAs. We propose a modest but effective program to trace superbly the development of the entire interaction region by drawing on capabilities of STIS which are well-matched to the task, and on the strength of comparison with existing STIS data. STIS 9619 Echelle Blaze Shift vs. MSM Monthly Offset In the near future, monthly MSM offsets will probably be disabled for STIS echelle gratings, alleviating to some extent calibration problems associated with the monthly offsets. The data from this program will be used to improve empirical and optical models relating wavelength and blaze function shifts. These models will in turn be used to improve the calibration of archival echelle data obtained while monthly MSM offsets were enabled. The flux standard HZ43 will be observed with the E230H echelle grating at a central wavelength of 2513 Angstroms. Five exposures will be obtained, each with a different monthly offset applied to the Mode Select Mechanism {MSM}. STIS 8643 Ultraviolet Properties of the Metal Rich M87 Globular Cluster System We propose to use STIS imaging to obtain far-ultraviolet photometry of the metal rich globular cluster system of the elliptical galaxy M87. This system represents a key link between the well understood populations of the clusters and the hot stars in elliptical galaxies, where our physical insight is presently limited. Our goal is to establish the relationship between cluster metal abundance and the production of UV-bright populations of stars on the ``extreme horizontal branch'' at T{eff} > 16000K. These stars are the source of the surprising ``ultraviolet-upturn'' phenomenon in elliptical galaxies. Our observations will fill a major gap in the present coverage of cluster metal abundances. This would be an important step in understanding the dependence of the upturn on its parent stellar population. A basic motivation is the expectation that the UV-upturn could be the most sensitive probe of the ages and abundances of elliptical galaxy populations. We plan to observe 3 fields in M87, which will provide a sample of ~ 30--50 UV-detected objects in the brightest 3 magnitudes of its cluster luminosity function. The program is technically challenging but appears feasible. Relatively long integrations are needed, under conditions of minimum dayglow emission from Earth's atmosphere. STIS/CCD 8904 Bias Monitor-Part 2. The Space Telescope Imaging Spectrograph (CCD) was used to monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4 in order to build up high-S/N superbiases and track the evolution of hot columns. STIS/CCD 8908 CCD Imaging Flats C10. The Space Telescope Imaging Spectrograph (CCD) was used to investigate flat-field stability over a monthly period. STIS/CCD 9066 Closing in on the Hydrogen Reionization Edge of the Universe. The Space Telescope Imaging Spectrograph (CCD) was used in parallel constrain the Hydrogen reionization edge in emission that marks the transition from a neutral to a fully ionized IGM at a predicted redshifts. STIS/CCD 8902 Dark Monitor-Part 2. The Space Telescope Imaging Spectrograph (CCD) was used to monitor the darks. STIS/CCD 9317 Pure Parallel Imaging Program: Cycle 10. The Space Telescope Imaging Spectrograph (CCD) was used to perform the default archival pure parallel program for STIS during cycle 10. STIS/CCD/MA1 9067 UV Detectability of Bright Quasars in the Sloan Fields. The Space Telescope Imaging Spectrograph (CCD and MA1) was used to take MAMA spectra of approximately 30 new, bright, high-redshift quasars in each of the next three cycles. WF/PC-2 9043 Cepheid Distances to Early-type Galaxies. The WF/PC-2 was used to continue observations in the HST Key Project on the Extragalactic Distance Scale and the HST project on the "Calibration of Nearby Type Ia Supernovae'' that have greatly improved our knowledge of the Hubble Constant by providing a solid zero point for the Tully- Fisher {TF} relation and Type Ia Supernovae {SNIa}. However, severe inconsistencies remain for distance estimators to early-type galaxies such as surface brightness fluctuations {SBF}, the planetary nebula luminosity function {PNLF}, the fundamental plane {FP}, and the globular cluster luminosity function {GCLF}. As a result, the distance to the Virgo cluster core remains uncertain by as much as 20 determination is directly affected by a lingering 0.1 mag {5 uncertainty in the photometric calibration of the WFPC2. Resolving these issues is essential not only to firm up the extragalactic distance scale, but also to understand the mass and velocity structure of the local universe. SBF in particular is emerging as the method of choice for mapping local velocity fields to 10, 000 kms because it offers an order of magnitude less Malmquist bias than TF, and SNIa are too rare to study large scale flows effectively. This project will tighten the photometric calibration of the WFPC2, and provide a solid Cepheid calibration for SBF and PNLF. WF/PC-2 9157 Fundamental Properties Of L-Type Dwarfs In Binaries. The WF/PC-2 was used to characterize the physical properties of eight L-dwarfs in four binary systems. The goal is to obtain astrometric, photometric and spectroscopic measurements of each component that will yield basic information on atmospheric and dynamical properties. WF/PC-2 9345 Fundamental Properties of L-type Dwarfs in Binaries. The WF/PC-2 was used to characterize the physical properties of eight L-dwarfs in four binary systems. The goal is to obtain astrometric, photometric and spectroscopic measurements of each component that will yield basic information on their atmospheric and dynamical properties. WF/PC-2 9180 Gamma-ray Burst Progenitors: Probing Their Environment. The WF/PC-2 was used to perform a target of opportunity observation of gamma ray burster (GRB), GRB-011121. GRB astronomy is a field maturing at a phenomenal rate. Three important new observational and theoretical discoveries, formulated over the last twelve months, allow the proposer to address new, and in many cases, more sophisticated questions than could have been posed previously. These developments: the discovery of X-ray lines in GRB 991216; the observation that N_H as deduced from X-ray afterglow are one to two orders of magnitude larger than the dust extinction inferred from optical afterglow; and the growing realization that the afterglow emission may exhibit features of dust echoes, appear to offer unexpected and new diagnostics that will directly inform us about the progenitor, the circum-progenitor material and the immediate interstellar environs. WF/PC-2 9050 Outflow Collimation in Bipolar Symbiotic Nebulae. The WF/PC-2 was used to observe flow collimation in evolved stars that is neither expected nor understood. Classical theories of stellar evolution do not predict and cannot explain this bipolarity. More exotic concepts {binary interactions, spun-up atmospheres, poloidal or toroidal magnetized winds} have been proposed, but observations are yet to verify or falsify any of their predictions. This proposal will probe the near-nuclear morphology and kinematics of four bright, low-extinction targets whose large-scale structure is highly bipolar. The goal is to provide a detailed description of the circumnuclear outflows, to uncover the physical structure and nature of the collimator, and to evaluate the speculative collimation mechanisms. The bright nucleus has hampered efforts to explore the nebular collimators that lie close to the star, so we'll use STIS to disperse the nuclear light and, thus, to avoid its glare. A secondary goal is to obtain second-epoch WFPC2 images of all targets. WF/PC-2 9319 POMS Test Proposal: WFII Backup Parallel Archive Proposal II. The WF/PC-2 was used to execute a POMS test proposal, designed to simulate future scientific plans. WF/PC-2 9318 POMS Test Proposal: WFII Parallel Archive Proposal Continuation. The WF/PC-2 was used to perform the generic target version of the WFPC2 Archival Pure Parallel program. The program was used to take parallel images of random areas of the sky, following the recommendations of the Parallels Working Group. WFPC2 8938 WFPC2 CYCLE 9 SUPPLEMENTAL DARKS pt3/3. This dark calibration program obtains 3 dark frames every day to provide data for monitoring and characterizing the evolution of hot pixels. FLIGHT OPERATIONS SUMMARY: HSTARs: (for further details see http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf) 8682 GRG2_3GT out of limits @ 158/10:56:27z 8683 GRG2_4GT out of limits @ 158/13:26:00z 8684 C string FOF queue buffer overflow errors @ 158/18:46:00z 8685 Gyro 3 Motor Current OOL 158/22:44:33 GRG2_3MC (RGA 2-3 Motor current) flagged out of limits yellow high at EV=232.4mA. At 22:44:39 it flagged out red high at EV= 330.4mA. At 22:45:51 it flagged out yellow high EV= 252mA and went back inbounds at 158/22:46:03. The yellow limits L=195 H=220. The red limits L=70 H=270. During the time of the OOL we were not guiding, we were in orbit day and we were not in a SAA. The following Reacqs using gyro 3 were successful. Motor safemode test count reached 1795 which is equivalent to 45 seconds of a 90 second timer. PCS SE, MOSES, and NASA on call were contacted. Under investigation. 8686 GSACQ(1,3,3) Fine Lock backup on FGS 3, scan step limit on FGS 1 @ 160/05:08:20z 8687 486 status buffer message D08, SYSTEM_MOMENTUM_LIMIT_EXCEEDED @ 160/160/23:44:37z 8688 Core Data Server /CCS Process /Ccl Isp alarm @ 160/03:03:00z COMPLETED OPS REQs: 16786-2 NICMOS EEPROM Dump @ 158/1316z OPS NOTES EXECUTED: 0900-1 Command Problem 0900-1 Command Problem 1012-0 Change Limits MAMA1Threshold Voltage 1013-0 Gyro 3 and 4 Temperature Adjust 0996-1 Raise Battery Temperature Upper limits to 2 deg 1012-1 Change Limits MAMA1Threshold Voltage 0916-0 Tabulation of Slew Attitude Error (Miss-distance) SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 28 28 FGS REacq 26 26 FHST Update 52 52 LOSS of LOCK None COMMENTS: 1. TTR #'s have been replaced by CDS #'s and DR #'s. Generic problems have CDS #'s. Any problem may have a unique DR #. A given occurrence of a generic problem will have a CDS #, but may or may not have a DR # assigned by CSC. 2. Loads for SA161M02_F1 are approved and available on CCS-C & CCS-B. 3. ESB code d08 is "System momentum exceeded limit" (Ref: HSTAR # 8687) 4. No new OOL values for gyro 3 current have been observed since HSTAR # 8685. Continuation of Servicing Mission Orbital Verification and the gradual resumption of normal science observations and calibrations.