HUBBLE SPACE TELESCOPE DAILY REPORT # 3137 PERIOD COVERED: DOY 164: 0000Z (UTC) 06/12/02 - 0000Z (UTC) 06/13/02 OBSERVATIONS SCHEDULED (see HSTARS below for possible observation problems) 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 8934 WFPC2 Decontaminations and Associated Observations Pt. 3/3 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. 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. 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. FGS/1 9234 Calibrating the Mass-Luminosity Relation at the End of the Main Sequence. Fine Guidance Sensor #1 was used to calibrate the mass-luminosity relation for stars less massive than 0.2 Msun, with special emphasis on objects near the stellar/brown dwarf border. 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. GO 9276 Localization of Optically-Dark Gamma-Ray bursts by Chandra and HST We propose Chandra {CXO} observations of 4 GRBs detected by the HETE soft X-ray camera, with contemporaneous observations with HST. These observations are "relaxed" TOOs, performed 7-16 days after burst detection. To optimize the chance of isolating Z>10 GRBs, we will select "dark GRBs" for which no optical counterpart has been found by ground-based searches within 2 days of GRB onset. Previous CXO GRB searches have required that observations start within ~24 hours of burst onset, placing an enormous strain on CXO operations. We have determined that 30 ks observations made 7-16 days after burst onset will detect sufficient photons to allow <0.7" localization of the GRB afterglow. We will immediately place all CXO and HST positions and intensities in the public domain via the GCN. 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. 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. 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. ACS 9352 The Deceleration Test from Treasury Type Ia Supernovae at Redshifts 1.2 to 1.6 Type Ia supernovae {SNe Ia} provide the only direct evidence for an accelerating universe, an extraordinary result that needs a rigorous test. The case for cosmic acceleration rests on the observation that SNe Ia at z ~ 0.5 are ~ 0.25 mag fainter than they would be in a universe without acceleration. A powerful and straightforward way to assess the reliability of the SN Ia measurement and the conceptual framework of its interpretation is to look for cosmic deceleration at z >= 1. This would be a clear signature of a mixed dark-matter and dark-energy universe. Systematic errors in the SN Ia result attributed to grey dust or cosmic evolution of the SN Ia peak luminosity would not show this change of sign. We have demonstrated proof of this concept with a single SN Ia, SN 1997ff at z = 1.7, found and followed by HST. The results suggest an early epoch of deceleration, but this is too important a conclusion to rest on just one object. Here we propose to use HST for observations of six SNe Ia in the range 1.2 <= z <= 1.6, that will be discovered as a byproduct from proposed Treasury programs for high-latitude ACS surveys. Six objects will provide a much firmer foundation for a conclusion that touches on important questions of fundamental physics. 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. 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) 8693 - Data Server on A/string B/B process count drops from 1.0 to 0.0 @ 164/0555z 8694 - NICMOS Detector 3 VSRC voltage OOL high @ 164/1107z At 164/11:07:47 the mnemonic ND3VSRCV(DETECTOR 3 VSRC VOLTAGE) flagged out of limits red high EV=5.40402v and went back in bounds at 11:08:17. Red limits L=-0.1 H=5.15. NICMOS was in observe configuration. We were in orbit night and we were not in a SAA. The anomaly happened during a continuous scan. Observation NIC 110 at 11:07:59 may have been affected. 8695 - A-String AppServer home fills up @ 163/1848z 8696 - EquationServer_A not running @ 163/2030z 8697 - Please disregard this entry 8698 - Archive on the A/string was hung @ 164/2313z 8699 - SADE 2 - SADM Temp 3 @ 165/0416z COMPLETED OPS REQs: None OPS NOTES EXECUTED: None SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 5 5 FGS REacq 10 10 FHST Update 8 8 LOSS of LOCK None Operations Notes: 'B' string configured for Prime R/T Operations @ 164/1230z 'A' string configured for Prime R/T Operations @ 164/1340z SIGNIFICANT EVENTS: Continuation of Servicing Mission Orbital Verification and the gradual resumption of normal science observations and calibrations.