HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3145<br /><br />PERIOD COVERED: DOY 176<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 8914<br /><br />Sensitivity Monitor C10.<br /><br />mode to detect any change due to contamination or other causes. The STIS focus<br />is also monitored in an 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 />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 9077<br /><br />Survey of the LMC Planetary Nebulae.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to perform a snapshot<br />survey of all known LMC planetary nebulae {PNe} in order to study the<br />co-evolution of the nebulae and their central stars, and to probe the chemical<br />enrichment history of the LMC.<br /><br />STIS/CCD/MA2 9105<br /><br />Determination of the Distances and Masses of 3 Galactic Cepheids.<br /><br />The Space Telescope Imaging Spectrograph [CCD and MA2] was used to continue a<br />successful observing strategy which enabled the proposers to accurately measure<br />angular separations < 10^-2'' with the FOC for binaries with Cepheid primaries<br />and main sequence B or A star secondaries {our accuracy should improve to<br />~10^-3'' with STIS}. Once measurements are available at two carefully selected<br />phases and these are combined with spectroscopic orbits, the angular information<br />will enable the masses and distances for the binaries to be determined from<br />Newton's laws and Euclidean geometry. The distances determinations amount to<br />bypassing two rungs of the cosmic distance ladder: the moving-cluster distance<br />to the Hyades and main sequence fitting of clusters containing Cepheids. The<br />mass determinations will provide the first direct dynamical mass measurements<br />for Cepheids, providing sorely needed quantitative information on this poorly<br />understood stage of massive star evolution.<br /><br />WF/PC-2/STIS/CCD/MA2 9127<br /><br />The UV interstellar Extinction in Nearby Galaxies: M33.<br /><br />The WF/PC-2 and the Space Telescope Imaging Spectrograph [CCD and MA2] were used<br />to investigate further the dust properties that vary in different environments<br />and from galaxy to galaxy. The proposers had previously used HST to determine<br />the UV extinction curve in M31. That result, together with other studies of the<br />Magellanic Clouds and Milky Way, suggested that the dust particles vary and the<br />proposers plan to enlarge the sample by studying the UV extinction properties of<br />dust in M33, sampling different galactocentric distances and levels of star<br />formation activity.<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 overdensity 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 />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 />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 9586<br /><br />ACS Polarization Calibration<br /><br />This proposal aims to calibrate the polarization modes most heavily used in<br />Cycle 11. We need L-flat observations, observations of a polarized star and an<br />unpolarized star, and an observation of an extended polarized source.<br /><br />CAL/WF2 9597<br /><br />Intflat Sweep, Visflat Sweep, and Filter Anomaly Check<br /><br />No abstract available.<br /><br />FLIGHT OPERATIONS SUMMARY:<br /><br />HSTARS: [For details see ]http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf]<br /><br />8713 - C string NCC [HRS Cross point] @172/1600z<br /> NCC and CMD was moved to C string for the 6.1 burn in. NCC messages<br /> were not being received on the C string. CD manager verified that he<br /> was able to see data leaving and coming back on VIS_CD4_P2, HRS<br /> cross point. After several troubleshooting efforts, the HRS was hard<br /> patched for NCC. Maintenance replaced a bad board on the C string VEDA<br /> box. First board was bad. Second board that was installed in the VEDA was<br /> good. NCC still hard patched unable to interface NCC thought HRS. Under<br /> investigation.<br /><br />COMPLETED OPS REQs: None<br /><br />OPS NOTES EXECUTED: None<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 9 9<br />FGS REacq 5 5<br />FHST Update 23 23<br />LOSS of LOCK None<br /><br />Comments: Successfully completed DSMC SN Transition @ 176/22:00Z,<br /> with the exception of the scheduling interface to/from JSC.<br /><br />SIGNIFICANT EVENTS: None