HUBBLE SPACE TELESCOPE DAILY REPORT # 3134 PERIOD COVERED: DOY 161: 0000Z (UTC) 06/9/02 - 0000Z (UTC) 06/10/02 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 8906 Hot Pixel Annealing. 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. STIS/CCD 8907 Spectroscopic Flats C10. The Space Telescope Imaging Spectrograph (CCD) was used to obtain CCD flats in the spectrographic mode. STIS/MA1/MA2 8920 Cycle 10 MAMA Dark Measurements. The Space Telescope Imaging Spectrograph (MA1 and MA2) was used to perform the routine monitoring of the MAMA detector dark noise, and is the primary means of checking on health of the MAMA detectors systems through frequent monitoring of the background count rate. WFPC2 8938 WFPC2 CYCLE 9 SUPPLEMENTAL DARKS pt3/3. characterizing the evolution of hot pixels. WF/PC-2 8939 Cycle 10 Internal Monitor. The WF/PC-2 was used to calibrate the internal monitor, to be run weekly to monitor the health of the cameras. 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 8983 NICMOS Mode-2 Target Acquisition Test NICMOS coronagraphy is extremely sensitive to small centering errors which can result from imperfections in the target acquisition {TA} process. During HST Cycle 7 the on-board {TA} process was augmented which resulted in post-acquisition dispersions of target placements w.r.t. the fiducial position in the occulting system with 1-sigma RSX dispersions of 0.08 mas {or ~ 1/10 pixel}. This level of acquisition precision is required to enable high-contrast imaging near occulted targets of which the system is capable. With the elevated detector temperatures {relative to Cycle 7} which we anticipate in Cycle 11, the change in detector characteristics, if incorrectly compensated in on-board mode-2 image processing, would result in degraded TA accuracy, and ultimately in coronagraphic gain. In addition, we posit the susceptibility of the system to metrological changes with further dewar stress/relaxation which could alter TA performance. This test will evaluate the TA performance, following a number of apriori changes to "tunable constants" in the FSW data, which we anticipate would result in performance comparable to that seen in Cycle 7. This test will verify the operability of the TA FSW, the precision of the "hole finding" algorithm, the dynamic range {exposure time} requirements for acquiring coronagraphic targets to high precision, the astrometric calibration of the TA process {image scales and rotation}, the stability of sub-orbital and multi-orbital acquisitions. We will specifically re-evaluate the efficacy of the Target Location, Image Centration, and Coordinate Transformation algorithms in the on-board S/W working with contemporaneously acquired TA mode imaging, and "hole finding" reference flats. Flight S/W data table updates derived from the pre and post target acquisition images and FGS data may follow the execution of this test as noted for Cycle 7 in SMO-2021/2.13.9. We will also explore the operating characteristics of the target acquisition process in the regime of a low S/N {underexposed} targets and saturated targets. WF/PC-2 9057 Host Galaxies of Obscured QSOs Identified by 2MASS. The WF/PC-2 was used to perform a snapshot survey of red QSOs discovered in The Two Micron All Sky Survey {2MASS} to investigate the detailed properties of their host galaxies. This large, possibly dominant, population of QSOs in the local universe has been previously overlooked because reddening by {intrinsic} obscuration along our line of sight causes their colors to be too red for identification by traditional "UV- excess" techniques. Their near-IR colors are similar to PG- type {UV-excess} QSOs, but it is far from certain whether they are indeed from the same parent population or represent a completely new class of QSO. 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. ACS/WFC/HRC 9075 Cosmological Parameters from Type Ia Supernovae at High Redshift. The Advanced Camera for Surveys (WFC and HRC) was used to obtain a Hubble diagram of Type Ia supernovae {SNe Ia} that will be of long lasting value as a record of the expansion history of the universe. STIS/CCD 9077 Survey of the LMC Planetary Nebulae. The Space Telescope Imaging Spectrograph (CCD) was used to perform a snapshot survey of all known LMC planetary nebulae {PNe} in order to study the co-evolution of the nebulae and their central stars, and to probe the chemical enrichment history of the LMC. STIS/CCD 9088 Next Generation Spectral Library of Stars. The Space Telescope Imaging Spectrograph (CCD) was used to produce a "Next Generation'' Spectral Library of 600 stars for use in modeling the integrated light of galaxies and clusters by using the low dispersion UV and optical gratings of STIS. The library will be roughly equally divided among four metallicities, very low {Fe/H < -1.5}, low {-1.5 < Fe/H < -0.5}, near-solar {-0.5 < Fe/H < 0.1}, and super-solar {Fe/H > 0.1}, well-sampling the entire HR-diagram in each bin. Such a library will surpass all extant compilations and have lasting archival value, well into the Next Generation Space Telescope era. FGS/1 9168 The Distances to AM CVn Stars. brightest of the seven known AM CVn systems. AM CVn systems are binaries where mass is transferred from a completely hydrogen-deficient, degenerate mass donor to a white dwarf primary through a helium accretion disk. A better understanding of these systems is crucial for a number of reasons: (1) to study the late stages of binary evolution, (2) to study the effect of chemical composition on the physics of accretion discs, (3) to estimate their contribution to the Supernovae Ia rate, and (4) to estimate their contribution to the gravitational radiation background. 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. 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 9617 STIS CCD Spectroscopic Dispersion Monitor Constrain wavelength and spatial distortion maps using internal wavecals obtained with all 6 gratings {G230LB, G230MB, G430L, G430M, G750L, G750M} supported for use with the CCD. Data will be obtained for the nearly identical set of 38 central wavelengths used in Cycle 10 or requested in Cycle 11. STIS 9618 STIS MAMA Dispersion Solutions Obtain wavecals just deep enough to constrain wavelength and spatial distorion 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) 8689 STIS 557 Status Buffer Message, No Observation Lost @ 162/00:18:12z COMPLETED OPS REQs: 16787-0 Eclipse Management, ROC Test GMT Day 161/162 @162/02:22:27z OPS NOTES EXECUTED: 0900-1 Command Problem 0910-2 SI Console response to MCE Resets after FSW 4.8 is activated 0910-2 SI Console response to MCE Resets after FSW 4.8 is activated SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 10 10 FGS REacq 7 7 FHST Update 13 13 LOSS of LOCK None Operations Notes: 1. STIS-557 is "MAMA1_HV_IS_OFF" This message is sent when one of the voltage ramping routines detects a MAMA 1 ramp is in progress and the MAMA 1 high voltage is off. This check is performed between each step of both timed and monitored ramps. (Ref. DM-03D, App. L) (HSTAR # 8689) 2. SSSP down 161/2320 to 162/0736z for fan replacement. SIGNIFICANT EVENTS: None