HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3136<br /><br />PERIOD COVERED: DOY 163: 0000Z (UTC) 06/11/02 - 0000Z (UTC) 06/12/02<br /><br />OBSERVATIONS SCHEDULED AND ACCOMPLISHED:<br /><br />STIS/CCD 8588<br /><br />Gamma-Ray Bursts and their Host Environments.<br /><br />The Space Telescope Imaging Spectrograph (CCD) was used to investigate the<br />physics of gamma-ray bursts {GRBs} and the nature of their host galaxies. The<br />approach is three-pronged: 1} rapid HST ultraviolet spectroscopy and Chandra<br />imaging obtained within two days of an outburst will allow probing the physics<br />of the relativistic fireball and the nature of the ISM surrounding the GRB; 2}<br />long-term optical monitoring of the optical transient {OT} will permit testing<br />the hypothesis that GRBs are frequently highly collimated and to determine<br />whether supernovae underlie GRBs; 3} Chandra and HST observations of "dark" GRBs<br />will allow probing one of the greater mysteries surrounding GRBs, the nature of<br />the bursts without optical counterparts.<br /><br />STIS 8643<br /><br />Ultraviolet Properties of the Metal Rich M87 Globular Cluster System<br /><br />We propose to use STIS imaging to obtain far-ultraviolet photometry of the metal<br />rich globular cluster system of the elliptical galaxy M87. This system<br />represents a key link between the well understood populations of the clusters<br />and the hot stars in elliptical galaxies, where our physical insight is<br />presently limited. Our goal is to establish the relationship between cluster<br />metal abundance and the production of UV-bright populations of stars on the<br />``extreme horizontal branch" at T{eff} > 16000K. These stars are the source of<br />the surprising ``ultraviolet-upturn'' phenomenon in elliptical galaxies. Our<br />observations will fill a major gap in the present coverage of cluster metal<br />abundances. This would be an important step in understanding the dependence of<br />the upturn on its parent stellar population. A basic motivation is the<br />expectation that the UV-upturn could be the most sensitive probe of the ages and<br />abundances of elliptical galaxy populations. We plan to observe 3 fields in M87,<br />which will provide a sample of ~ 30--50 UV-detected objects in the brightest 3<br />magnitudes of its cluster luminosity function. The program is technically<br />challenging but appears feasible. Relatively long integrations are needed, under<br />conditions of minimum dayglow emission from Earth's atmosphere.<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 />STIS/CCD 8906<br /><br />Hot Pixel Annealing.<br /><br />The Space Telescope Imaging Spectrograph (CCD) was used to measure the<br />effectiveness of the CCD hot pixel annealing process by measuring the dark<br />current behavior before and after annealing and by searching for any window<br />contamination effects. In addition, CTE performance is examined by looking for<br />traps in a low signal level flat.<br /><br />WFPC2 8934<br /><br />WFPC2 Decontaminations and Associated Observations Pt. 3/3<br /><br />This proposal is for the monthly WFPC2 decons. Also included are instrument<br />monitors tied to decons: photometric stability check, focus monitor, pre- and<br />post-decon internals {bias, intflats, kspots, & darks}, UV throughput check,<br />VISFLAT sweep, and internal UV flat check.<br /><br />WFPC2 8938<br /><br />WFPC2 CYCLE 9 SUPPLEMENTAL DARKS pt3/3.<br /><br />This dark calibration program obtains 3 dark frames every day to provide data<br />for monitoring and characterizing the evolution of hot pixels.<br /><br />ACS/WFC/HRC 8947<br /><br />Weekly Test.<br /><br />The Advanced Camera for Surveys (WFC and HRC) was used to perform basic tests to<br />monitor, the read noise, the development of hot pixels and test for any source<br />of noise in ACS CCD detectors. This program will be executed at least once a day<br />for the entire lifetime of ACS.<br /><br />STIS/CCD 9066<br /><br />Closing in on the Hydrogen Reionization Edge of the Universe.<br /><br />The Space Telescope Imaging Spectrograph (CCD) was used in parallel constrain<br />the Hydrogen reionization edge in emission that marks the transition from a<br />neutral to a fully ionized IGM at a predicted redshifts.<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 />ACS 9289<br /><br />Low Redshift Cluster Gravitational Lensing Survey<br /><br />This proposal has two main scientific goals: to determine the dark matter<br />distribution of massive galaxy clusters, and to observe the high redshift<br />universe using these clusters as powerful cosmic telescopes. Deep, g, r, i, z<br />imaging of a sample of low-z {0.2-0.4} clusters will yield a large sample of<br />lensed background galaxies with reliable photometric redshifts. Using multiple<br />pointings with a central overlap region we will reach HDF-like depth in the<br />central, highly magnified cluster region and a shallower but wider coverage in<br />the outer cluster regions. By combining strong and weak lensing constraints with<br />the photometric redshift information it will be possible to precisely measure<br />the cluster dark matter distribution with an unprecedented combination of high<br />spatial resolution and area coverage, avoiding many of the uncertainties which<br />plague ground-based studies and yielding definitive answers about the structure<br />of massive dark matter haloes. In addition, the cosmological parameters can be<br />constrained in a largely model independent way using the multiply lensed objects<br />due to the dependence of the Einsteinng radius on the distance to the source. We<br />can also expect to detect several highly magnified dropout galaxies behind the<br />clusters in the redshift ranges 4-5 5-6 and 7-8, corresponding to a drop in the<br />flux in the g, r, and i bands relative to longer wavelength. We will obtain the<br />best information to date on the giant arcs already known in these clusters,<br />making possible detailed, pixel-by-pixel studies of their star formation rate,<br />dust distribution and structural components, including spiral arms, out to a<br />redshift of around z~2.5 in several passbands.<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 />ACS/WFC 9584<br /><br />ACS Default {Archival} Pure Parallel Program II.<br /><br />The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels.<br /><br />STIS 9618<br /><br />STIS MAMA Dispersion Solutions<br /><br />Obtain wavecals just deep enough to constrain wavelength and spatial distortion<br />maps without overusing the calibration lamp. For the first time on orbit, data<br />will be obtained at all available central wavelengths. This information will<br />help constrain global models of STIS optical performance being developed at ECF<br />and STScI. During the observations, MSM monthly offsets will be set to zero to<br />complement observations over the past couple of cycles, which occurred at extreme<br />monthly offsets. The echelle observations at zero offset will yield dispersion<br />solutions that are directly applicable to all echelle science data obtained<br />after monthly offsets are disabled.<br /><br />FLIGHT OPERATIONS SUMMARY:<br /><br />HSTARS: (For additional details on see<br />http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf)<br /><br />8692 - 'A' string backbone data server hung @ 164/0530z<br /><br />COMPLETED OPS REQs: None<br /><br />OPS NOTES EXECUTED:<br />911-0 - Limit Management During WFPC2 Decontamination (M001) @ 163/1425z<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 7 7<br />FGS REacq 9 9<br />FHST Update 14 14<br />LOSS of LOCK None<br /><br />Operations Notes:<br />'C' string configured for R/T Operations @ 164/0720z (see HSTAR 8692)<br /><br />SIGNIFICANT EVENTS: None