HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3157<br /><br />PERIOD COVERED: DOY 196<br /><br />OBSERVATIONS SCHEDULED (see HSTARS below for possible observation problems)<br /><br />STIS/CCD 8591<br /><br />The Smallest Nuclear Black Holes.<br /><br />The Space Telescope Imaging Spectrograph (CCD) was used to observe small nuclear<br />black holes which are the last major unexplored part of BH parameter space,<br />searching for the smallest BHs that HST can possibly find.<br /><br />STIS 8659<br /><br />High Resolution Spectrum of the Venus Lyman-Alpha Line Profile<br /><br />We propose to record a single high spectral resolution observation of the Venus<br />Lyman-alpha line, while HST is within Earth shadow and Venus is at 47.1 degrees<br />solar elongation, with a supporting observation of the Lyman-alpha geocorona<br />outside the exclusion zone {50 degrees}. This Lyman-alpha line profile will be<br />compared with emergent line profiles from Venus thermosphere radiative transfer<br />models to assess the energetics and contributions from supra-thermal sources of<br />hydrogen, a long-standing issue in Venus aeronomy. This information will enhance<br />understanding of the pathways of hydrogen escape from Venus and constrain models<br />of Venus climate evolution. The line profile will be used to assess the<br />abundance of deuterium in the Venus atmosphere, a quantity with great importance<br />to atmospheric evolution models. The HST STIS instrument is the only instrument<br />capable of making these far UV observations with sufficient spectral resolution<br />to address the details of hydrogen energetics in the Venus thermosphere and<br />exosphere. HST previously observed Venus with Esposito as PI {P4518 and P5783}.<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/MA1 8919<br /><br />MAMA Sensitivity and Focus Monitor C10.<br /><br />The Space Telescope Imaging Spectrograph (CCD and MA1) was used to monitor the<br />sensitivity of each MAMA grating mode to detect any change due to contamination<br />or other causes, and also to monitor the STIS focus in a spectroscopic and an<br />imaging 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 />WF/PC-2 8935<br /><br />Cycle 10 Standard Darks.<br /><br />The WF/PC-2 was used to obtain dark frames every week in order to provide data<br />for the ongoing calibration of the CCD dark current rate, and to monitor and<br />characterize the evolution of hot pixels. Over an extended period these data<br />will also provide a monitor of radiation damage to the CCDs.<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 />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 />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 />STIS/CCD 9110<br /><br />A Search for Kuiper Belt Object Satellites.<br /><br />The Space Telescope Imaging Spectrograph (CCD) was used to investigate whether<br />the large number of collisions thought to have taken place in the primordial<br />Kuiper belt suggest that many Kuiper belt objects {KBOs} could have suffered<br />binary-forming collisions similar to that which formed the Pluto -- Charon<br />binary. Detection of such KBO satellites would allow measurement of KBO masses,<br />would help to understand the past collisional environment of the Kuiper belt,<br />and would give a context to the otherwise unique-seeming formation of the Pluto<br />-- Charon binary.<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 />NICMOS 9321<br /><br />Dark current, shading profile, and read noise monitoring program<br /><br />The purpose of this proposal is to monitor the detector dark current, read<br />noise, and shading profile for all three NICMOS cameras from the onset of normal<br />NCS operations throughout the start of Cycle 11.<br /><br />NICMOS 9360<br /><br />Paschen-alpha Imaging of a SIRTF-Selected Nearby Galaxy Sample<br /><br />We propose to carry out a NICMOS snapshot survey in the Paschen-alpha {PAlpha}<br />emission line and H-band of the sample of galaxies being observed at 3.5 -- 160<br />microns as part of SIRTF Nearby Galaxies Survey {SINGS} and a related guaranteed<br />time survey of starburst galaxies. The PAlpha images, accessible only from HST,<br />will be combined with ground based HAlpha imaging to measure the extinction in<br />the star-forming centers of these galaxies, and obtain robust, extinction-<br />corrected maps of the massive star formation rate {SFR}. The PAlpha data by<br />themselves will provide reliable `extinction- free' SFRs, and a<br />cross-calibration of the {dust--affected} HAlpha-- and UV--based SFRs. The<br />PAlpha--based SFR measurements will extend the SFR-vs.-gas density law<br />{Schmidt--law} to surface densities at least 30 times higher than what is<br />accessible using HAlpha--based SFR measurements alone, bridging the gap between<br />normal galaxies and IR--luminous starbursts. Furthermore, the combination of the<br />HST PAlpha images with the SIRTF images and spectra, as well as ancillary<br />ground--based UBVRIJHK images and GALEX UV images being obtained as part of the<br />SINGS project, will provide a definitive study of the radiative transfer of<br />starlight and dust heating in star--forming galaxies. The processed NICMOS<br />images will be incorporated into the public SINGS Legacy Data Archive, to enable<br />scores of follow-up studies by the astronomical community at large.<br /><br />ACS 9395<br /><br />Is Bulge Formation Still Going-On? An ACS Survey of Pseudo-Bulges<br /><br />Pseudo-bulges, i.e., bulges with an exponential light profile, have been<br />unveiled in the centers of many intermediate-type disks. Their structural<br />similarity with the disks provides support to theoretical scenarios in which<br />bulges may form due to secular evolution processes within the host disks. If at<br />play, these processes would likely be active throughout a large fraction of<br />cosmic history down to our days: `young' bulges should exist. Our previous HST<br />WFPC2 and NICMOS survey of ~100 spirals has provided V-H colors for 11 Sb-Sc<br />pseudo-bulges, and these could be interpreted as suggestive of relatively young<br />stellar ages. Furthermore, dense nuclei have been discovered in these<br />pseudo-bulges, and their V-H colors may imply stellar masses sufficiently large<br />to activate the formation of the pseudo- bulge by means of dynamical dissolution<br />of progenitor bars. However, the V-H color, on its own, is fully degenerate<br />towards stellar ages, metallicities and masses, as well as dust content. We<br />therefore propose to use ACS to observe the 11 pseudo-bulges of our combined<br />WFPC2 and NICMOS sample in the F330W, F435W, and F814W filters. Extending the<br />wavelength baseline to the bluer passbands is essential to break the<br />mass-age-metallicity-dust degeneracy, and will provide far more accurate<br />estimates for the stellar population properties of the pseudo-bulges and their<br />nuclei. Proving the existence of `young' bulges in the local Universe would have<br />a big impact in our understanding of the formation of the Hubble sequence.<br /><br />ACS 9472<br /><br />A Snapshot Survey for Gravitational Lenses among z >= 4.0 Quasars<br /><br />Over the last few years, the Sloan Digital Sky Survey has revolutionized the<br />study of high-redshift quasars by discovering over 200 objects with redshift<br />greater than 4.0, more than doubling the number known in this redshift interval.<br />The sample includes eight of the ten highest redshift quasars known. We propose<br />a snapshot imaging survey of a well-defined sample of 250 z > 4.0 quasars in<br />order to find objects which are gravitationally lensed. Lensing models including<br />magnification bias predict that at least 4% of quasars in a flux-limited sample<br />at z > 4 will be multiply lensed. Therefore this survey should find of order 10<br />lensed quasars at high redshift; only one gravitationally lensed quasar is<br />currently known at z > 4. This survey will provide by far the best sample to<br />date of high-redshift gravitational lenses. The observed fraction of lenses can<br />put strong constraints on cosmological models, in particular on the cosmological<br />constant Lambda. In addition, magnification bias can significantly bias<br />estimates of the luminosity function of quasars and the evolution thereof; this<br />work will constrain how important an effect this is, and thereby give us a<br />better understanding of the evolution of quasars and black holes at early<br />epochs, as well as constrain models for black hole formation.<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/HRC 9566<br /><br />CCD Hot Pixel Annealing.<br /><br />The Advanced Camera for Surveys (WFC and HRC) was used to perform hot pixel<br />annealing that will be performed once per month. The CCD TECs will be turned off<br />and heaters will be activated to bring the WFC detector temperature to about<br />+10C. The HRC temperature will reach about 30C. This state will be held for<br />approximately 24 hours, after which the heaters are turned off, the TECs turned<br />on, and the CCDs returned to normal operating condition.<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 />NICMOS 9641<br /><br />Dark Generator Tool Test<br /><br />This program will test the NICMOS Dark Generator Tool by obtaining dark frames<br />that probe MULTIACCUM sequences not usually observed during the dark monitoring<br />programs.<br /><br />FLIGHT OPERATIONS SUMMARY:<br /><br />HSTARS: (For details see http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf)<br />8735 A-String AppServer @ 193/1635z.A-string AppServer grayed out around<br /> 1635z. Called Response team George Gibson. George requested that a<br /> shutdown be done on the AppServer. Doc was unable to shutdown the<br /> AppServer, it was hung. Sys Admin was asked to shutdown the server.<br /> Sys Admin reported that the AppServer had 57 processes running on the<br /> ScheduleReqMgrServe. Server ran out of swap spaces. At 1650z AppServer<br /> was started and everything came up OK. Under investigation.<br /><br />8736 - FHST Full Maneuver Update U2,3FM failed @ 196/1804z.FHST Full Maneuver<br /> Updates scheduled at 196/18:04:30, and at 196/18:07:15 using FHST 2 and<br /> 3 (optimal pair 2,3) failed completely.The error box results (i.e "3Failed")<br /> for mnemonics QEBSTFG0, QEBSTFG1, QEBSTFG2. Fhst Update: ROLL, DEL, 2,3<br /> showed vehicle error: V1 = -78.598, V2 = 48.292, V3 = -30.822 (arc-sec.<br /> Subsequent GSACQ (3,1,3) of 196/18:24:54 Z with Primary FGS Search Radius<br /> = 58 arc-sec was successful. Under investigation.<br /><br />8737 - SMAMT3A, SMAMT4A, SMAMT4B (all are Monitor Control Electronics MTE status<br /> indicators)broke limit for one sample (1.5 seconds) at 196/22:20:07,<br /> indicating a possible misconfiguration of Magnetic Torquer control electronics,<br /> or more likely a bit flip in the telemetry since all three mnemonics share MF<br /> 9, MFword 145 in telemetry definition.HSTAR written at request of on-call<br /> safing SE for tracking purposes. Under investigation.<br /><br />COMPLETED OPS REQs:<br />16799-0 - SI ROPs NS-2, 5, 9, 11 and 16 @ 196/1520z<br /><br />OPS NOTES EXECUTED: None<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 10 10<br />FGS REacq 5 5<br />FHST Update 25 23 See HSTAR # 8736<br />LOSS of LOCK None<br /><br />Operations Notes: None<br /><br />SIGNIFICANT EVENTS: