HUBBLE SPACE TELESCOPE DAILY REPORT # 3132 PERIOD COVERED: DOY 157: 0000Z (UTC) 06/05/02 - 0000Z (UTC) 06/06/02 OBSERVATIONS SCHEDULED AND ACCOMPLISHED: 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/CCD 8902 Dark Monitor-Part 2. The Space Telescope Imaging Spectrograph (CCD) was used to monitor the darks. 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. WFPC2 8938 WFPC2 CYCLE 9 SUPPLEMENTAL DARKS pt3/3. characterizing the evolution of hot pixels. ACS/WFC/HRC 8947 Weekly Test. 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. STIS/CCD 9074 The Origin and Physics of Gamma-Ray Bursts. The Space Telescope Imaging Spectrograph (CCD) was used to make observations that will provide the most stringent tests yet performed of the hypothesis that GRBs are powered by the collapse of massive stars. STIS CCD spectroscopy will be used to detect broad atomic features of supernovae underlying GRB optical transients, at flux levels more than a factor of three fainter than SN 1998bw. ACS/WFC/HRC 9075 Cosmological Parameters from Type Ia Supernovae at High Redshift. {SNe Ia} that will be of long lasting value as a record of the expansion history of the universe. STIS/CCD 9077 Survey of the LMC Planetary Nebulae. The Space Telescope Imaging Spectrograph (CCD) was used to perform a snapshot survey of all known LMC planetary nebulae {PNe} in order to study the co-evolution of the nebulae and their central stars, and to probe the chemical enrichment history of the LMC. STIS/CCD/MA2 9105 Determination of the Distances and Masses of 3 Galactic Cepheids. The Space Telescope Imaging Spectrograph (CCD and MA2) was used to continue a successful observing strategy which enabled the proposers to accurately measure angular separations < 10^-2'' with the FOC for binaries with Cepheid primaries and main sequence B or A star secondaries {our accuracy should improve to ~10^-3'' with STIS}. Once measurements are available at two carefully selected phases and these are combined with spectroscopic orbits, the angular information will enable the masses and distances for the binaries to be determined from Newton's laws and Euclidean geometry. The distances determinations amount to bypassing two rungs of the cosmic distance ladder: the moving-cluster distance to the Hyades and main sequence fitting of clusters containing Cepheids. The mass determinations will provide the first direct dynamical mass measurements for Cepheids, providing sorely needed quantitative information on this poorly understood stage of massive star evolution. STIS/MA1/MA2 9151 UV Snapshot Observation of Nearby Star Forming Galaxies. The Space Telescope Imaging Spectrograph (MA1 and MA2) was used to obtain FUV and NUV images of nearby emission- line galaxies with existing star-formation rate {SFR} measurements from their HAlpha flux. Recently, the use of the UV flux as a measure of SFR has gained much popularity for estimating SFRs at different cosmic epochs. However, the SFR estimated from UV flux could be greatly biased due to dust extinction. The KPNO International Spectroscopic Survey {KISS} provides a large sample of nearby HAlpha-selected starforming galaxies for which rich optical spectra are available for measuring metallicity and dust extinction through line ratios. By observing a subset of nearby emission-line galaxies in the KISS sample with the STIS FUV and NUV MAMA, a direct comparison between UV and Halpha SFR estimates will be possible. This will allow us to understand the effect of dust extinction on UV flux for star- forming galaxies over a wide range of HAlpha luminosity, metallicity absolute magnitude, and B-V color . A rough dust extinction curve will be constructed for such objects, making it possible to test plausible dust extinction curves used in previous SFR studies of the distant universe. Also, high-resolution UV images will allow us to search for plausible local counterparts to high redshift galaxies whose rest-frame UV morphology is available from existing optical HST data. FGS/1 9168 The Distances to AM CVn Stars. Fine Guidance Sensor (FGS) #1R was used to determine the parallaxes and proper motions of the five brightest of the seven known AM CVn systems. AM CVn systems are binaries where mass is transferred from a completely hydrogen-deficient, degenerate mass donor to a white dwarf primary through a helium accretion disk. A better understanding of these systems is crucial for a number of reasons: (1) to study the late stages of binary evolution, (2) to study the effect of chemical composition on the physics of accretion discs, (3) to estimate their contribution to the Supernovae Ia rate, and (4) to estimate their contribution to the gravitational radiation background. STIS/CCD 9176 LMC Eclipsing Binaries with Cepheid Components: The Key to the Extragalactic Distance Scale. The Space Telescope Imaging Spectrograph (CCD) was used to determine the distance to the LMC and to observe the Cepheid P-L that form the backbone of the Cosmic Distance Scale and the determination of H_degrees. Unfortunately, in spite of concerted efforts of many investigators, the zero point of the Cepheid P-L law and the LMC distance remain controversial and uncertain to ~10-15, using eclipsing binaries {EBs} as "standard candles'' to include two recently discovered LMC eclipsing binaries {EBs} with Cepheid components. These observations of these extraordinary systems hold the key to determining simultaneously the Cepheid P-L zero point and the LMC distance, and to provide a direct test of the Baade-Wesselink parallax method. 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. 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. 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. 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/WFC 9575 Default {Archival} Pure Parallel Program. The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels in POMS. FLIGHT OPERATIONS SUMMARY: HSTARs: 8680 GSACQ(3,2,3) search radius limit exceeded, 2nd try successful @ 157/09:00:00z GSACQ(3,2,3) beginning at 08:59:10 had a search radius limit exceeded flag at 09:03:16,second try was successful in reaching Fine Lock and Science Init., no observations affected. 486 Status Buffer message A05 was received. 8681 CORE login failure on the B string @ 157/17:30:00z COMPLETED OPS REQs: 16780-0 RMGA Calibration for June 2002 @ 157/1524z 16783-3 NICMOS MEB Temperature Limit Updates @ 157/1655z 16784-0 On-Board NICMOS Suspend Sequence Patch @ 157/1657z 16785-1 NICMOS Gain Table Updates @ 157/1851z OPS NOTES EXECUTED: 900-1 Command Problem 910-2 SI Console response to MCE Resets after FSW 4.8 is activated SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 7 7 FGS REacq 9 9 FHST Update 17 17 LOSS of LOCK None Operations Notes: 1. ESB code a05 is "FGS Coarse Track failed - Search Radius Limit exceeded" 2. 32K Engineering data loss due to STGT equipment failure 158 / 06:21:11 06:28:26z. (Reference DR # 44490). SIGNIFICANT EVENTS: None