HUBBLE SPACE TELESCOPE DAILY REPORT # 3136 PERIOD COVERED: DOY 163: 0000Z (UTC) 06/11/02 - 0000Z (UTC) 06/12/02 OBSERVATIONS SCHEDULED AND ACCOMPLISHED: STIS/CCD 8588 Gamma-Ray Bursts and their Host Environments. The Space Telescope Imaging Spectrograph (CCD) was used to investigate the physics of gamma-ray bursts {GRBs} and the nature of their host galaxies. The approach is three-pronged: 1} rapid HST ultraviolet spectroscopy and Chandra imaging obtained within two days of an outburst will allow probing the physics of the relativistic fireball and the nature of the ISM surrounding the GRB; 2} long-term optical monitoring of the optical transient {OT} will permit testing the hypothesis that GRBs are frequently highly collimated and to determine whether supernovae underlie GRBs; 3} Chandra and HST observations of "dark" GRBs will allow probing one of the greater mysteries surrounding GRBs, the nature of the bursts without optical counterparts. 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. 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. STIS/CCD 8906 Hot Pixel Annealing. The Space Telescope Imaging Spectrograph (CCD) was used to measure the effectiveness of the CCD hot pixel annealing process by measuring the dark current behavior before and after annealing and by searching for any window contamination effects. In addition, CTE performance is examined by looking for traps in a low signal level flat. WFPC2 8934 WFPC2 Decontaminations and Associated Observations Pt. 3/3 This proposal is for the monthly WFPC2 decons. Also included are instrument monitors tied to decons: photometric stability check, focus monitor, pre- and post-decon internals {bias, intflats, kspots, & darks}, UV throughput check, VISFLAT sweep, and internal UV flat check. 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. 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. 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. 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. ACS 9289 Low Redshift Cluster Gravitational Lensing Survey This proposal has two main scientific goals: to determine the dark matter distribution of massive galaxy clusters, and to observe the high redshift universe using these clusters as powerful cosmic telescopes. Deep, g, r, i, z imaging of a sample of low-z {0.2-0.4} clusters will yield a large sample of lensed background galaxies with reliable photometric redshifts. Using multiple pointings with a central overlap region we will reach HDF-like depth in the central, highly magnified cluster region and a shallower but wider coverage in the outer cluster regions. By combining strong and weak lensing constraints with the photometric redshift information it will be possible to precisely measure the cluster dark matter distribution with an unprecedented combination of high spatial resolution and area coverage, avoiding many of the uncertainties which plague ground-based studies and yielding definitive answers about the structure of massive dark matter haloes. In addition, the cosmological parameters can be constrained in a largely model independent way using the multiply lensed objects due to the dependence of the Einsteinng radius on the distance to the source. We can also expect to detect several highly magnified dropout galaxies behind the clusters in the redshift ranges 4-5 5-6 and 7-8, corresponding to a drop in the flux in the g, r, and i bands relative to longer wavelength. We will obtain the best information to date on the giant arcs already known in these clusters, making possible detailed, pixel-by-pixel studies of their star formation rate, dust distribution and structural components, including spiral arms, out to a redshift of around z~2.5 in several passbands. 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. ACS/WFC 9584 ACS Default {Archival} Pure Parallel Program II. The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels. STIS 9618 STIS MAMA Dispersion Solutions Obtain wavecals just deep enough to constrain wavelength and spatial distortion maps without overusing the calibration lamp. For the first time on orbit, data will be obtained at all available central wavelengths. This information will help constrain global models of STIS optical performance being developed at ECF and STScI. During the observations, MSM monthly offsets will be set to zero to complement observations over the past couple of cycles, which occurred at extreme monthly offsets. The echelle observations at zero offset will yield dispersion solutions that are directly applicable to all echelle science data obtained after monthly offsets are disabled. FLIGHT OPERATIONS SUMMARY: HSTARS: (For additional details on see http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf) 8692 - 'A' string backbone data server hung @ 164/0530z COMPLETED OPS REQs: None OPS NOTES EXECUTED: 911-0 - Limit Management During WFPC2 Decontamination (M001) @ 163/1425z SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 7 7 FGS REacq 9 9 FHST Update 14 14 LOSS of LOCK None Operations Notes: 'C' string configured for R/T Operations @ 164/0720z (see HSTAR 8692) SIGNIFICANT EVENTS: None