HUBBLE SPACE TELESCOPE DAILY REPORT # 3131 PERIOD COVERED: DOY 156: 0000Z (UTC) 06/04/02 - 0000Z (UTC) 06/05/02 OBSERVATIONS SCHEDULED AND ACCOMPLISHED: 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/MA1 8919 MAMA Sensitivity and Focus Monitor C10. grating mode to detect any change due to contamination or other causes, and also to monitor the STIS focus in a spectroscopic and an imaging mode. 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. NICMOS 8980 NICMOS Focus Monitor The purpose of this activity is to determine if the best focus determined in the NICMOS FINE ALIGNMENT program is stable. This program must execute 2-3 weeks after the NICMOS FINE ALIGNMENT program STIS/CCD 9074 The Origin and Physics of Gamma-Ray Bursts. The Space Telescope Imaging Spectrograph (CCD) was used to make observations that will provide the most stringent tests yet performed of the hypothesis that GRBs are powered by the collapse of massive stars. STIS CCD spectroscopy will be used to detect broad atomic features of supernovae underlying GRB optical transients, at flux levels more than a factor of three fainter than SN 1998bw. FGS/1 9089 Parallaxes of Cataclysmic Variables: Understanding Their Peculiar Secondary Stars. Fine Guidance Sensor #1 was used to measure precise parallaxes for three additional CVs {WZ Sge, RU Peg, and YZ Cnc}, whose orbital periods span a much larger range than explored in previous observations, allowing examination of how the accretion luminosity and secondary star change with orbital period. 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. 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. STIS/CCD/MA1 9459 The Response of the White Dwarf in WZ Sge to the Unexpected July 2001 Superoutburst. The Space Telescope Imaging Spectrograph (CCD and MA1) was used to observe WZ Sge, the most extreme dwarf nova and one of the closest known cataclysmic variables, that has undergone a superoutburst in July 2001 after 22 years in quiescence. Because of the uniqueness of this event, two DD proposals were approved, one to observe the outburst itself, and another for us to observe the early decline phase. Here it is proposed to complete our fundamental study of the response of a dwarf nova system to an outburst by continuing our UV coverage of this most extreme outbursting system during its decline to quiescence. This decline is expected to take more than 3 yrs, with the most dramatic changes occurring in the first 2 years. This once-in-a-lifetime chance to obtain high quality, high time {and spectral} resolution FUV data as the decline progresses into the critical transition from the disk- dominated phase to the bare white dwarf, provides an unique opportunity to study the response of the emerging white dwarf, whose chemical abundances, rotation and temperature variation with time bear the imprint of this extraordinary gigantic accretion event. ACS/HRC 9473 Masses and IMF Variations in Super Star Clusters We are proposing to obtain high spatial resolution images of a set of super star clusters for which we have been granted observing time to measure velocity dispersions via high- resolution ground-based optical echelle and K-band spectroscopy. The images will allow us to fit the light profiles and measure the radii of the clusters, and when combined with the velocity dispersions, will enable us to estimate the cluster masses. By comparing the mass-to-light ratios with those predicted from spectral synthesis models, we will investigate possible variations in the slope and lower mass cut-offs of the initial mass functions in these clusters. Correlations of the variations of these parameters with cluster environment may provide insight into the formation mechanisms for super star clusters. By comparing the light profiles obtained in a blue and red filter, we will also search for evidence of mass segregation in the clusters. Since these clusters are too young to have experienced dynamical mass segregation, differences in the light profiles of the clusters in the two filters could be due to processes that differentiate between high and low mass stars during the birth of the clusters and would provide further constraints on theoretical models of cluster formation. Since these clusters are far too compact to be resolved by any ground-based observations, the ACS/HRC on board HST is the only instrument capable of carrying out these observations. 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 9564 ACS Cycle 11: UV Earth Flats This proposal will obtain sequences of UV flats by observing the bright Earth. The HRC UV filters were chosen for modes which were not obtained in the lab. Since the UV transmission is likely to vary as a function of position on the Pol_UV filters and on the coronograph, and since this behavior is currently unconstrained by measurement, a good estimate for the missing UV flats cannot be made. Although POL_UV and CORON transmissions change little at long wavelengths, the UV transmission may change by amounts larger than can be estimated in the absence of actual UV transmission measurements 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. FLIGHT OPERATIONS SUMMARY: HSTARs: 8674 Flat Line @ 156/14:00:00z 8675 GSacq (2,3,3) results in Fine Lock Backup (2,0,0) @ 156/15:40:58z. The GSacq (2,3,3) of 156/15:40:58 showed Scan Step Limit Exceeded flags on FGS2, then resulted to Fine Lock Backup using FGS# 2 (2,0,0). FGS#3 started the walkdown process but was stopped after Crtrk and did not continue after that. No flags remained after the Acquisition completed and no error message was sent to the 486 STB events record. 8676 JHAS2P5(Hrc ceb ASpc 2 +5v) OOL @ 156/20:53:56z 8677 OPSSCV2 out of limit for one sample @ 157/04:53:33z 8678 Battery 2 Pressure Out-of-limit Low @ 157/01:41:25z 8679 CCS-C Incomplete Handover and REQACC Messages @ 157/01:56:57z COMPLETED OPS REQs: None OPS NOTES EXECUTED: 945-2 Update to EPS Key Monitors Post SM3B SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 8 8 FGS REacq 6 6 FHST Update 20 20 LOSS of LOCK None Operations Notes: None SIGNIFICANT EVENTS: None