HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3137<br /><br />PERIOD COVERED: DOY 164: 0000Z [UTC] 06/12/02 - 0000Z [UTC] 06/13/02<br /><br />OBSERVATIONS SCHEDULED [see HSTARS below for possible observation problems]<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 8934<br /><br />WFPC2 Decontaminations and Associated Observations Pt. 3/3<br /><br />photometric stability check, focus monitor, pre- and post-decon internals {bias,<br />intflats, kspots, & darks}, UV throughput check, VISFLAT sweep, and internal UV<br />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 />WF/PC-2 9043<br /><br />Cepheid Distances to Early-type Galaxies.<br /><br />The WF/PC-2 was used to continue observations in the HST Key Project on the<br />Extragalactic Distance Scale and the HST project on the "Calibration of Nearby<br />Type Ia Supernovae'' that have greatly improved our knowledge of the Hubble<br />Constant by providing a solid zero point for the Tully- Fisher {TF} relation and<br />Type Ia Supernovae {SNIa}. However, severe inconsistencies remain for distance<br />estimators to early-type galaxies such as surface brightness fluctuations {SBF},<br />the planetary nebula luminosity function {PNLF}, the fundamental plane {FP}, and<br />the globular cluster luminosity function {GCLF}. As a result, the distance to<br />the Virgo cluster core remains uncertain by as much as 20 determination is<br />directly affected by a lingering 0.1 mag {5 uncertainty in the photometric<br />calibration of the WFPC2. Resolving these issues is essential not only to firm<br />up the extragalactic distance scale, but also to understand the mass and<br />velocity structure of the local universe. SBF in particular is emerging as the<br />method of choice for mapping local velocity fields to 10, 000 kms because it<br />offers an order of magnitude less Malmquist bias than TF, and SNIa are too rare<br />to study large scale flows effectively. This project will tighten the<br />photometric calibration of the WFPC2, and provide a solid Cepheid calibration<br />for SBF and PNLF.<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 />FGS/1 9234<br /><br />Calibrating the Mass-Luminosity Relation at the End of the Main Sequence.<br /><br />Fine Guidance Sensor #1 was used to calibrate the mass-luminosity relation for<br />stars less massive than 0.2 Msun, with special emphasis on objects near the<br />stellar/brown dwarf border.<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 />GO 9276<br /><br />Localization of Optically-Dark Gamma-Ray bursts by Chandra and HST<br /><br />We propose Chandra {CXO} observations of 4 GRBs detected by the HETE soft X-ray<br />camera, with contemporaneous observations with HST. These observations are<br />"relaxed" TOOs, performed 7-16 days after burst detection. To optimize the<br />chance of isolating Z>10 GRBs, we will select "dark GRBs" for which no optical<br />counterpart has been found by ground-based searches within 2 days of GRB onset.<br />Previous CXO GRB searches have required that observations start within ~24 hours<br />of burst onset, placing an enormous strain on CXO operations. We have determined<br />that 30 ks observations made 7-16 days after burst onset will detect sufficient<br />photons to allow <0.7" localization of the GRB afterglow. We will immediately<br />place all CXO and HST positions and intensities in the public domain via the<br />GCN.<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 />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 />WF/PC-2 9345<br /><br />Fundamental Properties of L-type Dwarfs in Binaries.<br /><br />The WF/PC-2 was used to characterize the physical properties of eight L-dwarfs<br />in four binary systems. The goal is to obtain astrometric, photometric and<br />spectroscopic measurements of each component that will yield basic information<br />on their atmospheric and dynamical properties.<br /><br />ACS 9352<br /><br />The Deceleration Test from Treasury Type Ia Supernovae at Redshifts 1.2 to 1.6<br /><br />Type Ia supernovae {SNe Ia} provide the only direct evidence for an accelerating<br />universe, an extraordinary result that needs a rigorous test. The case for<br />cosmic acceleration rests on the observation that SNe Ia at z ~ 0.5 are ~ 0.25<br />mag fainter than they would be in a universe without acceleration. A powerful<br />and straightforward way to assess the reliability of the SN Ia measurement and<br />the conceptual framework of its interpretation is to look for cosmic<br />deceleration at z >= 1. This would be a clear signature of a mixed dark-matter<br />and dark-energy universe. Systematic errors in the SN Ia result attributed to<br />grey dust or cosmic evolution of the SN Ia peak luminosity would not show this<br />change of sign. We have demonstrated proof of this concept with a single SN Ia,<br />SN 1997ff at z = 1.7, found and followed by HST. The results suggest an early<br />epoch of deceleration, but this is too important a conclusion to rest on just<br />one object. Here we propose to use HST for observations of six SNe Ia in the<br />range 1.2 <= z <= 1.6, that will be discovered as a byproduct from proposed<br />Treasury programs for high-latitude ACS surveys. Six objects will provide a much<br />firmer foundation for a conclusion that touches on important questions of<br />fundamental physics.<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 />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 />8693 - Data Server on A/string B/B process count drops from 1.0 to 0.0 @ 164/0555z<br />8694 - NICMOS Detector 3 VSRC voltage OOL high @ 164/1107z<br /> At 164/11:07:47 the mnemonic ND3VSRCV[DETECTOR 3 VSRC VOLTAGE] flagged out<br /> of limits red high EV=5.40402v and went back in bounds at<br /> 11:08:17. Red limits L=-0.1 H=5.15. NICMOS was in observe configuration.<br /> We were in orbit night and we were not in a SAA. The anomaly happened during a<br /> continuous scan. Observation NIC 110 at 11:07:59 may have been affected.<br /><br />8695 - A-String AppServer home fills up @ 163/1848z<br />8696 - EquationServer_A not running @ 163/2030z<br />8697 - Please disregard this entry<br />8698 - Archive on the A/string was hung @ 164/2313z<br />8699 - SADE 2 - SADM Temp 3 @ 165/0416z<br /><br />COMPLETED OPS REQs: None<br /><br />OPS NOTES EXECUTED: None<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 5 5<br />FGS REacq 10 10<br />FHST Update 8 8<br />LOSS of LOCK None<br /><br />Operations Notes:<br />'B' string configured for Prime R/T Operations @ 164/1230z<br />'A' string configured for Prime R/T Operations @ 164/1340z<br /><br />SIGNIFICANT EVENTS:<br /><br />Continuation of Servicing Mission Orbital Verification and the gradual<br />resumption of normal science observations and calibrations.