HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3149<br /><br />PERIOD COVERED: DOY 182<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 />STIS/MA1/MA2 8920<br /><br />Cycle 10 MAMA Dark Measurements.<br /><br />the MAMA detector dark noise, and is the primary means of checking on health of<br />the MAMA detectors systems through frequent monitoring of the background count<br />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 />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 />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 />ACS 9301<br /><br />PHOTOMETRY AND GRISM SPECTROSCOPY IN HDF NORTH/SOUTH<br /><br />Take deep ACS images and grism exposures of fields with very deep infrared<br />imaging data. The combined optical - infrared data and grisms will be uniquely<br />suited to study galaxies at high redshift: very high redshift galaxies from the<br />grism data, and internally red galaxies from the combined optical - IR imaging.<br />The comparison of the grism redshifts with ground based spectroscopy will enable<br />an evaluation of the effectiveness of the grism for redshift studies. The 3<br />fields of interest for this study are: 1} HDF North, 2} HDF South, 3} MS1054-03.<br /><br />STIS/CCD 9317<br /><br />Pure Parallel Imaging Program: Cycle 10.<br /><br />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 program was used to take parallel images of random areas of the sky,<br />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 />ACS 9363<br /><br />Ultra Low Surface Brightness Galaxies<br /><br />Extremely low surface brightness galaxies have been detected in the Virgo<br />cluster, which are 2 magnitudes fainter than any previously known in that<br />cluster or even in the Local Group. ACS images of three of these should resolve<br />stars at the giant branch tip, and allow us to determine distances, mean metal<br />abundance of the stars, and rough ages. Confirmation of the nature of these<br />galaxies will provide evidence that dark matter halos are pervasive in the<br />universe, extending to galaxies with stellar densities 6 times lower than<br />currently known. These resolved stars would be the most distant yet observed<br />accurately by HST.<br /><br />FLIGHT OPERATIONS SUMMARY:<br /><br />HSTARS: [For details see ]http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf]<br /><br />Guide Star Acquisitions:<br /><br />Scheduled Acquisitions: Successful:<br /><br />Scheduled Re-acquisitions Successful:<br /><br />FHST Updates: Scheduled: Successful:<br /><br />Operations Notes:<br /><br />SIGNIFICANT EVENTS:<br /><br />ACS 9454<br /><br />The Nature of the UV Continuum in LINERs: A Variability Test<br /><br />LINERs may be the most common AGNs, and the signposts of accretion onto the<br />massive black holes present in most galaxies. However, the LINER spectrum is the<br />result of UV excitation, and, in at least some LINERs, a nuclear cluster of hot<br />stars, rather than an AGN, dominates the energetics in the UV. Thus, it is still<br />unknown if the UV continuum, or the optical emission lines it excites, have<br />anything to do with an AGN. The demographics and accretion physics of<br />low-luminosity AGNs hinge on this question. We propose to search for variability<br />in a sample of 17 LINERs with compact UV nuclei. Variability can reveal an AGN<br />component in the UV continuum, even when its light is not dominant. We will test<br />systematically the handful of non-definitive reports of UV variability, and<br />potentially quantify the AGN contribution to the UV emission. Variability in all<br />or most objects will be strong evidence that LINERs mark dormant AGNs in most<br />galaxies. Alternatively, a general null detection of variability will suggest<br />that, even in LINERs with additional AGN signatures, the UV continuum is stellar<br />in origin. Contemporaneous monitoring with the VLA/VLBA of 11 objects which have<br />radio cores {five of which we already know are radio-variable} will reveal the<br />relations between UV and radio variations. The UV-variable objects will be<br />targeted for future, better-sampled, monitoring.<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 />CAL/WF2 9597<br /><br />Intflat Sweep, Visflat Sweep, and Filter Anomaly Check<br /><br />No abstract available.<br /><br />WFPC2 9599<br /><br />WFPC2 Cycle 11 UV Earth Flats<br /><br />Monitor flat field stability. This proposal obtains sequences of earth streak<br />flats to improve the quality of pipeline flat fields for the WFPC2 UV filter<br />set. These Earth flats will complement the UV earth flat data obtained during<br />cycles 8-10.<br />FLIGHT OPERATIONS SUMMARY:<br /><br />HSTARS:<br />[For details see ]http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf]<br /><br />8723 BATTERY 5 CURRENT @ 181/20:26:35z.Battery 5 current[CBAT5CUR] flagged<br /> high= 18.2 amps, current upper yellow limit 18.0 amps. Initial limit<br /> violation was 2 samples and battery 5 current continued to toggle high<br /> for another 5 minutes. The first OOL occurred at the end of orbit night<br /> and continued to flag high at the end of several orbit nights during the<br /> shift. Battery 2 Pressure[CBAT2PRS] also flagged low= 820.757 PSI.<br /> Current CBAT2PRS lower yellow limit set at 825.0 PSI. Under investigation.<br /><br />COMPLETED OPS REQs: NONE<br /><br />OPS NOTES EXECUTED: NONE<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 3 3<br />FGS REacq 11 11<br />FHST Update 7 7<br />LOSS of LOCK None<br /><br />Operations Notes: None<br /><br />SIGNIFICANT EVENTS: None