HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3132<br /><br />PERIOD COVERED: DOY 157: 0000Z [UTC] 06/05/02 - 0000Z [UTC] 06/06/02<br /><br />OBSERVATIONS SCHEDULED AND ACCOMPLISHED:<br /><br />NICMOS 8790<br /><br />NICMOS Post-SAA calibration - CR Persistence Part 1.<br /><br />A new procedure proposed to alleviate the CR-persistence problem of NICMOS. Dark<br />frames will be obtained immediately upon exiting the SAA contour 23, and every<br />time a NICMOS exposure is scheduled within 50 minutes of coming out of the SAA.<br />The darks will be obtained in parallel in all three NICMOS Cameras. The POST-SAA<br />darks will be non-standard reference files available to users with a USEAFTER<br />date/time mark.<br /><br />STIS/CCD 8902<br /><br />Dark Monitor-Part 2.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to monitor the darks.<br /><br />STIS/CCD 8904<br /><br />Bias Monitor-Part 2.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to monitor the bias in<br />the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4 in order<br />to build up high-S/N superbiases and track the evolution of hot columns.<br /><br />WFPC2 8938<br /><br />WFPC2 CYCLE 9 SUPPLEMENTAL DARKS pt3/3.<br /><br />characterizing the evolution of hot pixels.<br /><br />ACS/WFC/HRC 8947<br /><br />Weekly Test.<br /><br />noise, the development of hot pixels and test for any source of noise in ACS CCD<br />detectors. This program will be executed at least once a day for the entire<br />lifetime of ACS.<br /><br />STIS/CCD 9074<br /><br />The Origin and Physics of Gamma-Ray Bursts.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to make observations<br />that will provide the most stringent tests yet performed of the hypothesis that<br />GRBs are powered by the collapse of massive stars. STIS CCD spectroscopy will be<br />used to detect broad atomic features of supernovae underlying GRB optical<br />transients, at flux levels more than a factor of three fainter than SN 1998bw.<br /><br />ACS/WFC/HRC 9075<br /><br />Cosmological Parameters from Type Ia Supernovae at High Redshift.<br /><br />{SNe Ia} that will be of long lasting value as a record of the expansion history<br />of the universe.<br /><br />STIS/CCD 9077<br /><br />Survey of the LMC Planetary Nebulae.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to perform a snapshot<br />survey of all known LMC planetary nebulae {PNe} in order to study the<br />co-evolution of the nebulae and their central stars, and to probe the chemical<br />enrichment history of the LMC.<br /><br />STIS/CCD/MA2 9105<br /><br />Determination of the Distances and Masses of 3 Galactic Cepheids.<br /><br />The Space Telescope Imaging Spectrograph [CCD and MA2] was used to continue a<br />successful observing strategy which enabled the proposers to accurately measure<br />angular separations < 10^-2'' with the FOC for binaries with Cepheid primaries<br />and main sequence B or A star secondaries {our accuracy should improve to<br />~10^-3'' with STIS}. Once measurements are available at two carefully selected<br />phases and these are combined with spectroscopic orbits, the angular information<br />will enable the masses and distances for the binaries to be determined from<br />Newton's laws and Euclidean geometry. The distances determinations amount to<br />bypassing two rungs of the cosmic distance ladder: the moving-cluster distance<br />to the Hyades and main sequence fitting of clusters containing Cepheids. The<br />mass determinations will provide the first direct dynamical mass measurements<br />for Cepheids, providing sorely needed quantitative information on this poorly<br />understood stage of massive star evolution.<br /><br />STIS/MA1/MA2 9151<br /><br />UV Snapshot Observation of Nearby Star Forming Galaxies.<br /><br />The Space Telescope Imaging Spectrograph [MA1 and MA2] was used to obtain FUV<br />and NUV images of nearby emission- line galaxies with existing star-formation<br />rate {SFR} measurements from their HAlpha flux. Recently, the use of the UV flux<br />as a measure of SFR has gained much popularity for estimating SFRs at different<br />cosmic epochs. However, the SFR estimated from UV flux could be greatly biased<br />due to dust extinction. The KPNO International Spectroscopic Survey {KISS}<br />provides a large sample of nearby HAlpha-selected starforming galaxies for which<br />rich optical spectra are available for measuring metallicity and dust extinction<br />through line ratios. By observing a subset of nearby emission-line galaxies in<br />the KISS sample with the STIS FUV and NUV MAMA, a direct comparison between UV<br />and Halpha SFR estimates will be possible. This will allow us to understand the<br />effect of dust extinction on UV flux for star- forming galaxies over a wide<br />range of HAlpha luminosity, metallicity absolute magnitude, and B-V color . A<br />rough dust extinction curve will be constructed for such objects, making it<br />possible to test plausible dust extinction curves used in previous SFR studies<br />of the distant universe. Also, high-resolution UV images will allow us to search<br />for plausible local counterparts to high redshift galaxies whose rest-frame UV<br />morphology is available from existing optical HST data.<br /><br />FGS/1 9168<br /><br />The Distances to AM CVn Stars.<br /><br />Fine Guidance Sensor [FGS] #1R was used to determine the parallaxes and proper<br />motions of the five brightest of the seven known AM CVn systems. AM CVn systems<br />are binaries where mass is transferred from a completely hydrogen-deficient,<br />degenerate mass donor to a white dwarf primary through a helium accretion disk.<br />A better understanding of these systems is crucial for a number of reasons: [1]<br />to study the late stages of binary evolution, [2] to study the effect of<br />chemical composition on the physics of accretion discs, [3] to estimate their<br />contribution to the Supernovae Ia rate, and [4] to estimate their contribution<br />to the gravitational radiation background.<br /><br />STIS/CCD 9176<br /><br />LMC Eclipsing Binaries with Cepheid Components: The Key to the Extragalactic<br />Distance Scale.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to determine the<br />distance to the LMC and to observe the Cepheid P-L that form the backbone of the<br />Cosmic Distance Scale and the determination of H_degrees. Unfortunately, in<br />spite of concerted efforts of many investigators, the zero point of the Cepheid<br />P-L law and the LMC distance remain controversial and uncertain to ~10-15, using<br />eclipsing binaries {EBs} as "standard candles'' to include two recently<br />discovered LMC eclipsing binaries {EBs} with Cepheid components. These<br />observations of these extraordinary systems hold the key to determining<br />simultaneously the Cepheid P-L zero point and the LMC distance, and to provide a<br />direct test of the Baade-Wesselink parallax method.<br /><br />NICMOS 9269<br /><br />NICMOS Parallel Thermal Background<br /><br />NICMOS Camera 3 pure parallel exposures in the F222M filter will be obtained for<br />the entire duration of SMOV to establish the stability of the HST+NCS+Instrument<br />thermal emission.<br /><br />STIS/CCD 9317<br /><br />Pure Parallel Imaging Program: Cycle 10.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to perform the default<br />archival pure parallel program for STIS during cycle 10.<br /><br />WF/PC-2 9318<br /><br />POMS Test Proposal: WFII Parallel Archive Proposal Continuation.<br /><br />The WF/PC-2 was used to perform the generic target version of the WFPC2 Archival<br />Pure Parallel program. The program was used to take parallel images of random<br />areas of the sky, following the recommendations of the Parallels Working Group.<br /><br />ACS/CAL 9558<br /><br />ACS weekly Test<br /><br />This program consists of basic tests to monitor, the read noise, the development<br />of hot pixels and test for any source of noise in ACS CCD detectors. This<br />programme will be executed once a day for the entire lifetime of ACS.<br /><br />ACS/WFC 9575<br /><br />Default {Archival} Pure Parallel Program.<br /><br />The Advanced Camera for Surveys [WFC] was used to test ACS pure parallels in<br />POMS.<br /><br />FLIGHT OPERATIONS SUMMARY:<br /><br />HSTARs:<br /><br />8680 GSACQ[3,2,3] search radius limit exceeded, 2nd try successful @ 157/09:00:00z<br /> GSACQ[3,2,3] beginning at 08:59:10 had a search radius limit exceeded flag at<br /> 09:03:16,second try was successful in reaching Fine Lock and Science Init., no<br /> observations affected. 486 Status Buffer message A05 was received.<br /><br />8681 CORE login failure on the B string @ 157/17:30:00z<br /><br />COMPLETED OPS REQs:<br />16780-0 RMGA Calibration for June 2002 @ 157/1524z<br />16783-3 NICMOS MEB Temperature Limit Updates @ 157/1655z<br />16784-0 On-Board NICMOS Suspend Sequence Patch @ 157/1657z<br />16785-1 NICMOS Gain Table Updates @ 157/1851z<br /><br />OPS NOTES EXECUTED:<br />900-1 Command Problem<br />910-2 SI Console response to MCE Resets after FSW 4.8 is activated<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 7 7<br />FGS REacq 9 9<br />FHST Update 17 17<br />LOSS of LOCK None<br /><br />Operations Notes:<br />1. ESB code a05 is "FGS Coarse Track failed - Search Radius Limit exceeded"<br />2. 32K Engineering data loss due to STGT equipment failure 158 / 06:21:11<br />06:28:26z. [Reference DR # 44490].<br /><br />SIGNIFICANT EVENTS: None