HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3153<br /><br />PERIOD COVERED: DOY 190<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/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 />WFPC2 8934<br /><br />WFPC2 Decontaminations and Associated Observations Pt. 3/3<br /><br />This proposal is for the monthly WFPC2 decons. Also included are instrument<br />monitors tied to decons: photometric stability check, focus monitor, pre- and<br />post-decon internals {bias, intflats, kspots, & darks}, UV throughput check,<br />VISFLAT sweep, and internal UV flat check.<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 />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 />GTO/ACS 9291<br /><br />Formation of High Redshift Radio Galaxies<br /><br />galaxy and cluster formation in the early Universe. By carrying out deep<br />observations of a few z > 3.8 targets the following four questions will be<br />studied: {1} Are HzRGs massive central-cluster galaxies formed through<br />hierarchical assembly of Lyman break galaxies? Detailed brightness distributions<br />colors and morphologies of HzRG clumps will be measured and compared with those<br />of Lyman break galaxies. {2} Are HzRGs located in dense {proto-} clusters and if<br />so what are the properties of the associated large-scale structures? Lyman alpha<br />excesses, colors and morphologies of objects in field will be used to search for<br />companion galaxies of HzRGs. {3} What are the origin and fate of giant gas halos<br />associated with HzRGs and what role do they play in the formation of massive<br />galaxies? The morphologies and locations of Ly-alpha clumps will be compared<br />with those of continuum clumps. {4} Is nuclear activity a source of star<br />formation in the early Universe? The properties of continuum and Ly-alpha clumps<br />along will be compared in relation to the radio jet.<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/WFC 9373<br /><br />Reaching the Horizontal Branch in NGC 5128: Deepest Probe of a Giant Elliptical<br /><br />NGC 5128 is the nearest easily observable giant E galaxy, and is a unique<br />testing ground for stellar population models. Previous WFPC2 photometry of its<br />halo red-giant stars has shown that they are predominantly metal-rich<br />{<m/H>~-0.45}, but little is yet known about their spread in ages. With the<br />ACS/WFC camera, we propose to obtain deep {V, I} photometry down to the level of<br />its horizontal-branch population, with the goal of refining the metallicity<br />distribution function and gaining quantitative information on its age<br />distribution. This will be unique data for any giant elliptical galaxy and will<br />provide major new input to population synthesis techniques for such galaxies.<br /><br />HST/ACS 9403<br /><br />Galaxy Formation in Nearby Voids: Reflections of the High-Redshift Universe?<br /><br />Galaxy voids, at the opposite environmental extreme from galaxy clusters,<br />present an ideal yet under- utilized laboratory for probing the relationship<br />between environment and the mechanisms of galaxy formation and evolution.<br />Mounting evidence from ground-based surveys of galaxies in voids suggests that<br />they have formed comparatively recently {and many are still forming} from<br />gas-rich, low velocity-dispersion surroundings: a picture in accordance with<br />models of hierarchical structure formation. The superior resolution of HST<br />allows us to verify this hypothesis with the first directed HST imaging survey<br />of void galaxies {VGs}. With HST/ACS deep imaging of a subset of E+S0 VGs from<br />our earlier ground-based imaging and spectroscopic survey, we will investigate<br />their globular cluster {GC} systems to unravel their formation history and to<br />constrain the age of their oldest GCs. The HST resolution of their inner light<br />profiles will reveal whether they have significantly under-massive central black<br />holes, as might be expected if these are young systems. HST will also detect the<br />presence of morphological fine structure indicative of recent merger activity.<br />If the present-day VGs truly reflect the early stages of galaxy formation which<br />occurred at higher redshift outside the voids, their proximity enables the<br />investigation of galaxy formation processes in much greater detail than possible<br />from observations of the high-redshift field, even with NGST.<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 />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 /><br />NICMOS 9645<br /><br />NICMOS Tilt Test<br /><br />The purpose of this activity is to determine the best tilt positions for NIC2<br />and NIC3 FLIGHT OPERATIONS SUMMARY:<br /><br />HSTARS: (For details see http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf)<br /><br />8731 EquationServer_A down @ 191/0650z. Paul called and said he could not connect<br /> to the EquationServer_A. The following message kept appearing when I started<br /> the Geneq_check.ccs on the A string: "Unable to establish connection with<br /> EquationServer. All Equations will be marked as missing." I checked outside<br /> on the server and the two javaw.exe processess were not up. Paul asked me to<br /> get someone to look into this as soon as day shift started. Under<br /> investigation.<br /><br />COMPLETED OPS REQs:<br />16798-0 GENSLEW for proposal 9110 slot 5 @ 190/16:52:00z<br /><br />OPS NOTES EXECUTED:<br />1004-2 Update Pressure-Based Battery Capacity Equations<br />1004-2 Update Pressure-Based Battery Capacity Equations<br /> Guide Star Acquisitions:<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 5 5<br />FGS REacq 10 10<br />FHST Update 7 7<br />LOSS of LOCK None<br />Operations Notes:<br /><br />COMMENTS: None<br /><br />SIGNIFICANT EVENTS: HST IP Transition/CCC "G" String to SOC testing scheduled<br />191/14:00Z - 20:00Z with GDOC, SOC, HITT, and CCS using CCS "G" String with<br />CCS Release 4.0.1.