HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3134<br /><br />PERIOD COVERED: DOY 161: 0000Z (UTC) 06/9/02 - 0000Z (UTC) 06/10/02<br /><br />OBSERVATIONS SCHEDULED AND ACCOMPLISHED:<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 />STIS/CCD 8906<br /><br />Hot Pixel Annealing.<br /><br />pixel annealing process by measuring the dark current behavior before and after<br />annealing and by searching for any window contamination effects. In addition,<br />CTE performance is examined by looking for traps in a low signal level flat.<br /><br />STIS/CCD 8907<br /><br />Spectroscopic Flats C10.<br /><br />The Space Telescope Imaging Spectrograph (CCD) was used to obtain CCD flats in<br />the spectrographic mode.<br /><br />STIS/MA1/MA2 8920<br /><br />Cycle 10 MAMA Dark Measurements.<br /><br />The Space Telescope Imaging Spectrograph (MA1 and MA2) was used to perform the<br />routine monitoring of the MAMA detector dark noise, and is the primary means of<br />checking on health of the MAMA detectors systems through frequent monitoring of<br />the background count rate.<br /><br />WFPC2 8938<br /><br />WFPC2 CYCLE 9 SUPPLEMENTAL DARKS pt3/3.<br /><br />characterizing the evolution of hot pixels.<br /><br />WF/PC-2 8939<br /><br />Cycle 10 Internal Monitor.<br /><br />The WF/PC-2 was used to calibrate the internal monitor, to be run weekly to<br />monitor the health of the cameras.<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 />NICMOS 8983<br /><br />NICMOS Mode-2 Target Acquisition Test<br /><br />NICMOS coronagraphy is extremely sensitive to small centering errors which can<br />result from imperfections in the target acquisition {TA} process. During HST<br />Cycle 7 the on-board {TA} process was augmented which resulted in<br />post-acquisition dispersions of target placements w.r.t. the fiducial position<br />in the occulting system with 1-sigma RSX dispersions of 0.08 mas {or ~ 1/10<br />pixel}. This level of acquisition precision is required to enable high-contrast<br />imaging near occulted targets of which the system is capable. With the elevated<br />detector temperatures {relative to Cycle 7} which we anticipate in Cycle 11, the<br />change in detector characteristics, if incorrectly compensated in on-board<br />mode-2 image processing, would result in degraded TA accuracy, and ultimately in<br />coronagraphic gain. In addition, we posit the susceptibility of the system to<br />metrological changes with further dewar stress/relaxation which could alter TA<br />performance. This test will evaluate the TA performance, following a number of<br />apriori changes to "tunable constants" in the FSW data, which we anticipate<br />would result in performance comparable to that seen in Cycle 7. This test will<br />verify the operability of the TA FSW, the precision of the "hole finding"<br />algorithm, the dynamic range {exposure time} requirements for acquiring<br />coronagraphic targets to high precision, the astrometric calibration of the TA<br />process {image scales and rotation}, the stability of sub-orbital and<br />multi-orbital acquisitions. We will specifically re-evaluate the efficacy of the<br />Target Location, Image Centration, and Coordinate Transformation algorithms in<br />the on-board S/W working with contemporaneously acquired TA mode imaging, and<br />"hole finding" reference flats. Flight S/W data table updates derived from the<br />pre and post target acquisition images and FGS data may follow the execution of<br />this test as noted for Cycle 7 in SMO-2021/2.13.9. We will also explore the<br />operating characteristics of the target acquisition process in the regime of a<br />low S/N {underexposed} targets and saturated targets.<br /><br />WF/PC-2 9057<br /><br />Host Galaxies of Obscured QSOs Identified by 2MASS.<br /><br />The WF/PC-2 was used to perform a snapshot survey of red QSOs discovered in The<br />Two Micron All Sky Survey {2MASS} to investigate the detailed properties of<br />their host galaxies. This large, possibly dominant, population of QSOs in the<br />local universe has been previously overlooked because reddening by {intrinsic}<br />obscuration along our line of sight causes their colors to be too red for<br />identification by traditional "UV- excess" techniques. Their near-IR colors are<br />similar to PG- type {UV-excess} QSOs, but it is far from certain whether they<br />are indeed from the same parent population or represent a completely new class<br />of QSO.<br /><br />STIS/CCD 9074<br /><br />The Origin and Physics of Gamma-Ray Bursts.<br /><br />The Space Telescope Imaging Spectrograph (CCD) was used to make observations<br />that will provide the most stringent tests yet performed of the hypothesis that<br />GRBs are powered by the collapse of massive stars. STIS CCD spectroscopy will be<br />used to detect broad atomic features of supernovae underlying GRB optical<br />transients, at flux levels more than a factor of three fainter than SN 1998bw.<br /><br />ACS/WFC/HRC 9075<br /><br />Cosmological Parameters from Type Ia Supernovae at High Redshift.<br /><br />The Advanced Camera for Surveys (WFC and HRC) was used to obtain a Hubble<br />diagram of Type Ia supernovae {SNe Ia} that will be of long lasting value as a<br />record of the expansion history of the universe.<br /><br />STIS/CCD 9077<br /><br />Survey of the LMC Planetary Nebulae.<br /><br />The Space Telescope Imaging Spectrograph (CCD) was used to perform a snapshot<br />survey of all known LMC planetary nebulae {PNe} in order to study the<br />co-evolution of the nebulae and their central stars, and to probe the chemical<br />enrichment history of the LMC.<br /><br />STIS/CCD 9088<br /><br />Next Generation Spectral Library of Stars.<br /><br />The Space Telescope Imaging Spectrograph (CCD) was used to produce a "Next<br />Generation'' Spectral Library of 600 stars for use in modeling the integrated<br />light of galaxies and clusters by using the low dispersion UV and optical<br />gratings of STIS. The library will be roughly equally divided among four<br />metallicities, very low {Fe/H < -1.5}, low {-1.5 < Fe/H < -0.5}, near-solar<br />{-0.5 < Fe/H < 0.1}, and super-solar {Fe/H > 0.1}, well-sampling the entire<br />HR-diagram in each bin. Such a library will surpass all extant compilations and<br />have lasting archival value, well into the Next Generation Space Telescope era.<br /><br />FGS/1 9168<br /><br />The Distances to AM CVn Stars.<br /><br />brightest of the seven known AM CVn systems. AM CVn systems are binaries where<br />mass is transferred from a completely hydrogen-deficient, degenerate mass donor<br />to a white dwarf primary through a helium accretion disk. A better understanding<br />of these systems is crucial for a number of reasons: (1) to study the late<br />stages of binary evolution, (2) to study the effect of chemical composition on<br />the physics of accretion discs, (3) to estimate their contribution to the<br />Supernovae Ia rate, and (4) to estimate their contribution to the gravitational<br />radiation background.<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 />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 />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 9617<br /><br />STIS CCD Spectroscopic Dispersion Monitor<br /><br />Constrain wavelength and spatial distortion maps using internal wavecals<br />obtained with all 6 gratings {G230LB, G230MB, G430L, G430M, G750L, G750M}<br />supported for use with the CCD. Data will be obtained for the nearly identical<br />set of 38 central wavelengths used in Cycle 10 or requested in Cycle 11.<br /><br />STIS 9618<br /><br />STIS MAMA Dispersion Solutions<br /><br />Obtain wavecals just deep enough to constrain wavelength and spatial distorion<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 />8689 STIS 557 Status Buffer Message, No Observation Lost @ 162/00:18:12z<br /><br />COMPLETED OPS REQs:<br />16787-0 Eclipse Management, ROC Test GMT Day 161/162 @162/02:22:27z<br /><br />OPS NOTES EXECUTED:<br />0900-1 Command Problem 0910-2 SI Console response to MCE Resets after<br />FSW 4.8 is activated<br />0910-2 SI Console response to MCE Resets after FSW 4.8 is activated<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 10 10<br />FGS REacq 7 7<br />FHST Update 13 13<br />LOSS of LOCK None<br /><br />Operations Notes:<br /><br />1. STIS-557 is "MAMA1_HV_IS_OFF" This message is sent when one of the voltage<br />ramping routines detects a MAMA 1 ramp is in progress and the MAMA 1 high<br />voltage is off. This check is performed between each step of both timed and<br />monitored ramps. (Ref. DM-03D, App. L) (HSTAR # 8689)<br />2. SSSP down 161/2320 to 162/0736z for fan replacement.<br /><br />SIGNIFICANT EVENTS: None