HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3147<br /><br />PERIOD COVERED: DOY 178<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 />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/MA1/MA2 9151<br /><br />UV Snapshot Observation of Nearby Star Forming Galaxies.<br /><br />The Space Telescope Imaging Spectrograph [MA1 and MA2] was used to obtain FUV<br />and NUV images of nearby emission- line galaxies with existing star-formation<br />rate {SFR} measurements from their HAlpha flux. Recently, the use of the UV flux<br />as a measure of SFR has gained much popularity for estimating SFRs at different<br />cosmic epochs. However, the SFR estimated from UV flux could be greatly biased<br />due to dust extinction. The KPNO International Spectroscopic Survey {KISS}<br />provides a large sample of nearby HAlpha-selected starforming galaxies for which<br />rich optical spectra are available for measuring metallicity and dust extinction<br />through line ratios. By observing a subset of nearby emission-line galaxies in<br />the KISS sample with the STIS FUV and NUV MAMA, a direct comparison between UV<br />and Halpha SFR estimates will be possible. This will allow us to understand the<br />effect of dust extinction on UV flux for star- forming galaxies over a wide<br />range of HAlpha luminosity, metallicity absolute magnitude, and B-V color . A<br />rough dust extinction curve will be constructed for such objects, making it<br />possible to test plausible dust extinction curves used in previous SFR studies<br />of the distant universe. Also, high-resolution UV images will allow us to search<br />for plausible local counterparts to high redshift galaxies whose rest-frame UV<br />morphology is available from existing optical HST data.<br /><br />STIS/CCD/MA2 9166<br /><br />Fossil Gaseous Halos of Massive Galaxies at z~1.<br /><br />The Space Telescope Imaging Spectrograph [CCD and MA2] was used to observe host<br />galaxies of high-redshift, powerful radio sources that are likely the<br />progenitors of present-day gE and cD galaxies, and therefore provide important<br />laboratories in which to investigate the formation of massive galaxies in the<br />early Universe. Many high-redshift radio galaxies exhibit giant, Ly-alpha halos.<br />Similar nebulae without associated radio sources have recently been discovered<br />in a galaxy over density at z = 3.09. The LyAlpha luminosity of these halos is<br />comparable to the total X-ray luminosities of low--z X--ray clusters, and may<br />reflect the hot, cooling gas reservoir from which the galaxy/cluster is forming.<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 />GTO/ACS 9290<br /><br />The Nature of Galaxies at z > 4.<br /><br />The Morphological, Photometric, and Spectroscopic Properties of Intermediate<br />Redshift Cluster.New and fundamental constraints on the evolutionary state of<br />high redshift clusters will be made by obtaining deep, multiband images {SDSS g,<br />r, i, z} over the central 1.5 Mpc regions of seven distant clusters in the range<br />0.76 < z < 1.27. In addition, slitless spectroscopy, using the WFC GRISM, will<br />be performed over the central 750 kpc region of each system galaxy.<br /><br />ACS/HRC/WFC 9292<br /><br />The Nature of Galaxies at z > 4<br /><br />The Advanced Camera for Surveys [HRC and WFC] was used to further look into<br />recent discoveries of a number of galaxies and quasars at redshifts greater than<br />5 that has identified the z>5-6 epoch as key to understanding the earliest<br />formation phases for galaxies. However, establishing the characteristics and<br />properties of these earliest galaxies is proving to be a particularly difficult.<br />They are faint, with I{AB} magnitudes around 26-27. Thus, substantial<br />investments of time are needed to obtain high S/N images, while ground-based<br />spectroscopy, even with 8-10 m class telescopes, has provided little more than<br />redshifts. Establishing the physical properties of these galaxies will be a<br />challenge for the foreseeable future. However, there is a subset of this high<br />redshift population that is amenable to more detailed study. These are sources<br />that have been strongly lensed by low redshift clusters.<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 9442<br /><br />Optical Counterparts for Low-Luminosity X-ray Sources in Omega Centauri<br /><br />We propose to use narrow-band HAlpha imaging with ACS to search for the optical<br />counterparts of low-luminosity X-ray sources {Lx ~ 2 x 10^30 - 5 x 10^32 erg/s}<br />in the globular cluster Omega Centauri. With 9 WFC fields, we will cover the<br />inner two core radii of the cluster, and encompass about 90 of the faint sources<br />we have identified with Chandra. Approximately 30-50 of these sources should be<br />cluster members, the remainder being mostly background galaxies plus a smaller<br />number of foreground stars. This large population of low-Lx cluster X-ray<br />sources is second only to the more than 100 faint sources recently discovered in<br />47 Tuc with Chandra {Grindlay et al. 2001a}, which have been identified as a<br />mixture of cataclysmic variables, quiescent low-mass X-ray binaries, millisecond<br />pulsars, and coronally active main-sequence binaries. Our Cycle 6 WFPC2 program<br />successfully identified 2 of the 3 then-known faint X-ray sources in the core of<br />Omega Cen using H-alpha imaging. We now propose to expand the areal coverage by<br />a factor of about 18 to encompass the much larger number of sources that have<br />since been discovered with Chandra. The extreme crowding in the central regions<br />of Omega Cen requires the resolution of HST to obtain optical IDs. These<br />identifications are key to making meaningful comparisons between the populations<br />of faint X-ray sources in different clusters, in an effort to understand their<br />origins and role in cluster dynamics.<br /><br />STIS 9505<br /><br />The Evolution of Molecular Clouds.<br /><br />of ablation in the evolution of the central clouds.<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 />CAL/WF2 9597<br /><br />Intflat Sweep, Visflat Sweep, and Filter Anomaly Check<br /><br />No abstract available.<br /><br />STIS 9646<br /><br />Wind Accretion and State Transitions in the Black Hole Binary Cyg X-1<br /><br />The black hole binary, Cyg X-1, is now {May 2002} in the high/soft X-ray state,<br />the first one to occur since 1996. Models predict that this state corresponds to<br />a high mass transfer phase in the binary, but several lines of observational<br />evidence cast doubt on this assumption. The best test of this hypothesis is to<br />observe the UV P Cygni lines of the supergiant that are formed in its wind<br />outflow. We propose to obtain the first ever high resolution UV spectra of the<br />system using STIS to determine {1} the mass loss rate and the dynamical {density<br />and velocity} structure of the wind of the supergiant star in both X-ray states,<br />and {2} how the X-ray source ionizes the wind. These spectra will be useful for<br />many investigations and will form an important resource for many in the research<br />community.<br /><br />FLIGHT OPERATIONS SUMMARY:<br /><br />HSTARS: [For details see ]http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf]<br /><br />8717 EQUATION SERVER NOT INCREMENTING @ 178/10:15z.CCS "A" String Equation Server<br /> not incrementing @ 178/10:15Z. Two javaw.exe were not present, re-cycled<br /> Equation Server, problem cleared. Under investigation.<br /><br />COMPLETED OPS REQs: NONE<br /><br />OPS NOTES EXECUTED: NONE<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 6 6<br />FGS REacq 7 7<br />FHST Update 11 11<br />LOSS of LOCK None<br /><br />Operations Notes: FOT moved to building 23 control center facility<br />to accommodate PMs on PDU-1<br /><br />SIGNIFICANT EVENTS: None