HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3155<br /><br />PERIOD COVERED: DOY 192<br /><br />OBSERVATIONS SCHEDULED [see HSTARS below for possible observation problems]<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 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 />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 />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/HRC 9445<br /><br />Gravitational Microlensing in the NGC 3314A-B Galaxy Pair.<br /><br />The Advanced Camera for Surveys [WFC and HRC] was used to determine the<br />composition of the dark matter that dominates the masses of galaxies which is an<br />important unsolved problem.<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 />STIS 9506<br /><br />A SNAPSHOT SURVEY OF HIGH COLUMN DENSITY, LOW-Z LyAlpha ABSORBERS<br /><br />We propose a STIS G140L spectroscopic Snapshot program of bright {V<=16.5} AGN<br />not previously observed in the UV to discover new high-column density {N_H >=<br />10^15 cm^-2} LyAlpha absorbers in the local Universe {z <= 0.45}. Many more of<br />these high column density systems are needed because: {1} They contribute most<br />of the baryons to the local IGM; {2} They include systems for which valuable<br />metallicity and D/H measurements can be made with the Cosmic Origins<br />Spectrograph {COS}; {3} They include many of the ``warm-hot'' absorbers, thought<br />to be a large baryon reservoir in the local Universe; and {4} They are most<br />likely to be ``associated'' with galaxy halos. Because of their low-z, many of<br />these absorbers can be located relative to galaxies of known redshifts, allowing<br />an immediate scientific return from these snapshots. Perhaps the most important,<br />lasting results of this survey require higher resolution reobservations with COS<br />by our GTO team. Using these snapshots to select the best targets, we will<br />obtain COS R~22, 000 spectra to determine the D/H and metallicity of absorbers<br />in galaxy halos, groups, and voids. We will use pairs and ``constellations'' of<br />AGN to determine absorber sizes, shapes, and covering factors. Candidate<br />``warm-hot'' absorbers will be reobserved with COS to determine their numbers<br />accurately and to assess their metallicity, sizes, and relationships to galaxies<br />and galaxy groups.<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 9562<br /><br />Cycle 11 Internal Flat Field Stability.<br /><br />The Advance Camera for Surveys [WFC and HRC] was used to obtain flat field<br />stability and characterization samples of the ACS filter set. Only internal<br />exposures using the calibration lamps were required.<br /><br />ACS 9563<br /><br />Preliminary ACS Sensitivity<br /><br />A spectrophotometric standard star is observed through a popular subset of<br />filters of each camera to assess the sensitivity of the instrument. The star is<br />placed at the centre of the aperture, and two images are taken through each<br />filter. This programme is based on proposal 9020 designed for SMOV. There are<br />three groups of visits, numbered respectively 1 through 3, 4 through 6 and 7<br />through 9. The three visits in each group must be executed about one month apart<br />from one another, as indicated in the visit requirements. The first visit in<br />each group {namely visits 1, 4 and 7} ought to be scheduled during the month of<br />July 2002. During SMOV the standard star GD71 could be used, which is not<br />visible during the Cycle 11 interim calibration period. We have selected<br />GRW+705824 instead. The latter is a WD slightly brighter than GD71 in V but with<br />very similar spectral properties. The exposure times with this object have been<br />selected to reach, on average, SNR~350 in the central pixel for broad band<br />filters.<br /><br />ACS 9567<br /><br />SBC Dark Current<br /><br />Dark current measurements will be made for the ACS SBC once a week.<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 />STIS 9635<br /><br />UV Zeeman spectroscopy of AM Herculis<br /><br />AM Herculis, the brightest strongly magnetic cataclysmic variable, entered in<br />December 2001 an extended state of low accretion activity. During such low<br />states, the magnetic white dwarf totally dominates the ultraviolet emission of<br />the system, and only then an in-depth study of its photospheric properties<br />becomes feasible. We propose to obtain an exploratory HST/STIS observation of<br />the magnetic white dwarf in AM Herculis. We will use these data to measure for<br />the first time the Zeeman splittings of metal {C, N, O, Si} resonance lines in a<br />magnetic field that is far beyond the reach of any terrestrial laboratory<br />{B=14MG}. These observations will provide fundamental experimental input that<br />should enable significant progress of our understanding of the behavior of<br />matter in strong magnetic fields. Four HST orbits will be sufficient to map both<br />the abundance and temperature variation over the surface of the WD.<br /><br />FLIGHT OPERATIONS SUMMARY:<br /><br />HSTARS: [For details see ]http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf]<br /><br />HSTARS: None<br /><br />COMPLETED OPS REQs:<br />16800-0 - Genslew for proposal 9110 - slot 4 @ 192/2157z<br /><br />OPS NOTES EXECUTED:<br />939-1 - NSSC-1 Load in Count Mode @ 193/0346z<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 11 11<br />FGS REacq 6 6<br />FHST Update 17 17<br />LOSS of LOCK None<br /><br />Operations Notes: STIS MCE 1 Reset[HV off, outside SAA] @ 192/19:02:25Z.<br />See STIS MCE Reset Log at URL: http://edocs1.hst.nasa.gov/doc/publish/mop/STISReset.htm<br />for details. Reset STIS FSW Error Counter [STIS 734] @ 192/21:55Z [ROP NS-12].<br /><br />HST CCS "G" String Command testing scheduled 193/12:00Z - 20:00Z with GDOC, SOC, HITT,<br />and CCS using CCS "G" String with CCS Release 4.0.1.<br /><br />SIGNIFICANT EVENTS: None