HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3162<br /><br />PERIOD COVERED: DOY 203<br /><br />OBSERVATIONS SCHEDULED [see HSTARS below for possible observation problems]<br /><br />STIS 8672<br /><br />Establishing the Gaseous Phases of Galaxies Following the Epoch of Star<br />Formation<br /><br />We propose an ambitious program designed to: {1} establish if high ionization,<br />metal-rich halos/coronae were in place as early as z~1, which would imply that<br />extended, early-epoch, galactic halos result from reprocessed galactic gas and<br />that the kinematics are mechanically driven; {2} obtain the first comparison of<br />the relative kinematics of low and high ionization species in z~1 galaxies,<br />covering a wide range of N{HI} environments and MgII kinematic spreads up to<br />~400 km/s; {3} discriminate between single-phase and multi-phase ionization, and<br />therefore spatial, absorbing structures {eg. MgII clouds embedded in diffuse<br />high ionization halos}; and {4} place constraints on the gas-phase metallicites<br />in early-epoch galaxies. We propose to obtain STIS R=30, 000 {Delta v = 10 km/s}<br />spectra of five bright quasars, for which the FOS/HST data are fully analyzed.<br />Our observational goal is to resolve the absorption profiles of several low,<br />intermediate, and high ionization species, including OVI, OI, NV, NIII, CIV,<br />CIII, CII, SiIV, SiIII, and SiII, in 18 MgII absorption systems covering<br />0.5<=z<=1.3. We incorporate our high signal-to-noise HIRES/Keck {Delta v=6.6<br />km/s} profiles of MgII, MgI, and FeII of the low ionization absorbing gas, and<br />our database of the absorbing galaxy luminosities, colors, and impact<br />parameters.<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 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 />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 />WF/PC-2 8939<br /><br />Cycle 10 Internal Monitor.<br /><br />The WF/PC-2 was used to calibrate the internal monitor, to be run weekly to<br />monitor the health of the cameras.<br /><br />STIS/CCD 9074<br /><br />The Origin and Physics of Gamma-Ray Bursts.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to make observations<br />that will provide the most stringent tests yet performed of the hypothesis that<br />GRBs are powered by the collapse of massive stars. STIS CCD spectroscopy will be<br />used to detect broad atomic features of supernovae underlying GRB optical<br />transients, at flux levels more than a factor of three fainter than SN 1998bw.<br /><br />9130<br /><br />STIS/CCD/MA1 9179<br /><br />Calibrating Convection Efficiency With Quasi-Molecular Features In Magnetic<br />White Dwarfs.<br /><br />The Space Telescope Imaging Spectrograph [CCD and MA1] was used to observe<br />recently-discovered quasi-molecular absorption features of Lyman Alpha in UV<br />spectra of magnetic white dwarfs taken with IUE. Hitherto, such features have<br />only been known in non-magnetic objects where they offered a very accurate<br />determination of the atmospheric parameters.<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 />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 />NICMOS 9322<br /><br />NICMOS ACCUM Darks<br /><br />The goal is to obtain ACCUM darks with exposure time=256 seconds with NREADS=25,<br />taken away from the SAA. These are needed to calibrate the post-SAA darks that<br />will be used to remove CR persistence from NICMOS science images. In the early<br />Cycle 11 calibration plan they should be obtained every 4 weeks. We will<br />evaluate need for repeats later<br /><br />NICMOS 9323<br /><br />NICMOS Focus Stability<br /><br />The purpose of this activity is to determine if the best focus determined in<br />SMOV is stable. This program will execute in approximately one month intervals<br />starting about 1 month after the last execution of proposal 8980.<br /><br />ACS 9468<br /><br />ACS Grism Parallel Survey of Emission- line Galaxies at Redshift z pl 7<br /><br />We propose an ACS grism parallel survey to search for emission-line galaxies<br />toward 50 random lines of sight over the redshift interval 0 < zpl 7. We<br />request ACS parallel observations of duration more than one orbit at high<br />galactic latitude to identify ~ 300 HAlpha emission-line galaxies at 0.2pl zpl<br />0.5, ~ 720 O IILambda3727 emission-line galaxies at 0.3pl zpl 1.68, and pg<br />1000 Ly-alpha emission-line galaxies at 3pl zpl 7 with total emission line<br />flux fpg 2* 10^-17 ergs s^-1 cm^-2 over 578 arcmin^2. We will obtain direct<br />images with the F814W and F606W filters and dispersed images with the WFC/G800L<br />grism at each position. The direct images will serve to provide a zeroth order<br />model both for wavelength calibration of the extracted 1D spectra and for<br />determining extraction apertures of the corresponding dispersed images. The<br />primary scientific objectives are as follows: {1} We will establish a uniform<br />sample of HAlpha and O II emission-line galaxies at z<1.7 in order to obtain<br />accurate measurements of co-moving star formation rate density versus redshift<br />over this redshift range. {2} We will study the spatial and statistical<br />distribution of star formation rate intensity in individual galaxies using the<br />spatially resolved emission-line morphology in the grism images. And {3} we will<br />study high-redshift universe using Ly-alpha emitting galaxies identified at z<br />pl 7 in the survey. The data will be available to the community immediately as<br />they are obtained.<br /><br />ACS 9480<br /><br />Cosmic Shear With ACS Pure Parallels<br /><br />Small distortions in the shapes of background galaxies by foreground mass<br />provide a powerful method of directly measuring the amount and distribution of<br />dark matter. Several groups have recently detected this weak lensing by<br />large-scale structure, also called cosmic shear. The high resolution and<br />sensitivity of HST/ACS provide a unique opportunity to measure cosmic shear<br />accurately on small scales. Using 260 parallel orbits in Sloan textiti {F775W}<br />we will measure for the first time: beginlistosetlength sep0cm setlengthemsep0cm<br />setlength opsep0cm em the cosmic shear variance on scales <0.7 arcmin, em the<br />skewness of the shear distribution, and em the magnification effect. endlist Our<br />measurements will determine the amplitude of the mass power spectrum<br />sigma_8Omega_m^0.5, with signal-to-noise {s/n} ~ 20, and the mass density<br />Omega_m with s/n=4. They will be done at small angular scales where non-linear<br />effects dominate the power spectrum, providing a test of the gravitational<br />instability paradigm for structure formation. Measurements on these scales are<br />not possible from the ground, because of the systematic effects induced by PSF<br />smearing from seeing. Having many independent lines of sight reduces the<br />uncertainty due to cosmic variance, making parallel observations ideal.<br /><br />SNAP 9485<br /><br />Completing A Near-Infrared Search for Very Low Mass Companions to Stars within<br />10 pc of the Sun<br /><br />Most stars are fainter and less massive than the Sun. Nevertheless, our<br />knowledge of very low mass {VLM} red dwarfs and their brown dwarf cousins is<br />quite limited. Unknown are the true luminosity function {LF}, multiplicity<br />fraction, mass function, and mass-luminosity relation for red and brown dwarfs,<br />though they dominate the Galaxy in both numbers and total mass. The best way to<br />constrain these relations is a search for faint companions to nearby stars. Such<br />a search has several advantages over field surveys, including greater<br />sensitivity to VLM objects and the availability of precise parallaxes from which<br />luminosities and masses can be derived. We propose to complete our four-filter<br />NICMOS snapshot search for companions to stars within 10 pc. With a 10 sigma<br />detection limit of M_J ~ 20 at 10 pc, we can detect companions between 10 and<br />100 AU that are at least 9 mag fainter than the empirical end of the main<br />sequence and at least 6.5 mag fainter than the brown dwarf Gl 229B. When<br />completed, our search will be the largest, most sensitive, volume-limited search<br />for VLM companions ever undertaken. Ourfour-filter search will permit<br />unambiguous identification of VLM-companion candidates for follow-up<br />observation. Together with IR speckle and deep imaging surveys, our program will<br />firmly establish the LF for VLM companions at separations of 1-1000 AU and the<br />multiplicity fraction of all stars within 10 pc.<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 9567<br /><br />SBC Dark Current<br /><br />Dark current measurements will be made for the ACS SBC once a week.<br /><br />STIS 9617<br /><br />STIS CCD Spectroscopic Dispersion Monitor<br /><br />Constrain wavelength and spatial distortion maps using internal wavecals<br />obtained with all 6 gratings {G230LB, G230MB, G430L, G430M, G750L, G750M}<br />supported for use with the CCD. Data will be obtained for the nearly identical<br />set of 38 central wavelengths used in Cycle 10 or requested in Cycle 11.<br /><br />WFPC2 9676<br /><br />POMS Test Proposal: WFII parallel archive proposal<br /><br />This is the generic target version of the WFPC2 Archival Pure Parallel program.<br />The program will be used to take parallel images of random areas of the sky,<br />following the recommendations of the 2002 Parallels Working Group.<br /><br />POMS 9677<br /><br />POMS Test Proposal: WFII backup parallel archive proposal<br /><br />This is a POMS test proposal designed to simulate scientific plans. FLIGHT<br />OPERATIONS SUMMARY:<br /><br />HSTARS: [For details see ]http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf]<br /><br />8742 - HST Ephemeris Load Accuracy Check Failure for 2002.204 @203/1442z.The<br /> Ephemeris Load generated on 2002.203 for uplink on 2002.204 [covering<br /> the period from 2002.204 to 2002.211] failed the accuracy check. The<br /> magnitude of the maximum position difference exceeded the limit of<br /> 10 km. by 0.6 km. HSTAR 8657 documents a previous accuracy check failure.<br /> Under investigation.<br /><br />8743 - A-string BackBone Data Server MOPSS, message deamon process count zero<br /> @203/2023z.A-String BackBone Data Server MOPSS of CCS, message<br /> deamon process count dropped to zero vice one. - Nabil Afram of Sys.<br /> Admin. informed IDOC that one of the Raid disk drives failed.<br /> Under investigation.<br /><br />8744 - NICMOS SUSPEND @204/0342z.NICMOS Suspended at 204/0342:19 due to<br /> a status buffer message NICMOS 104 with a parameter of 2. [INTEL EXCEPTION]<br /> While in boot mode a control section reset was detected. SI SE and<br /> Institute SE were notified. NICMOS observations NIC 29 were occurring<br /> at the time. Under investigation.<br /><br />COMPLETED OPS REQs: None<br /><br />OPS NOTES EXECUTED: None<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 4 4<br />FGS REacq 10 10<br />FHST Update 7 7<br />LOSS of LOCK None<br /><br />Operations Notes:<br /><br />SIGNIFICANT EVENTS:<br /><br />NICMOS suspended @ 204/03:42:19Z, see HSTAR 8744. NSSC-1 Status Buffer message<br />NICMOS 104, Parameter 2 was posted, indicating an Intel Exception debug error.<br />This message has been seen previously on-orbit. Instrument was in Observe and<br />executing exposures when the Suspend occurred. NICMOS memory dump was performed<br />per ROP NS-9 @ 204/06:49Z and the files were made available to Code 582 Payload<br />FSW for analysis.<br /><br />Successfully completed CCS-O-0013 R/T ESTR and SSR Operations Test 203/11:00Z -<br />15:18Z. Verified in telemetry all science and engineering records and playbacks<br />occurred. Verified on the Events page files were opened and the playbacks were<br />being processed correctly. The PSS hung and a reboot was necessary, no impact<br />to testing.<br /><br />Performed CCC Command Communication Controller Test 203/17:00Z -18:30Z. A<br />Packet Filter Flush was performed, but only partially successful. Connections<br />were disconnected at the Packet Filter but not at the CCS interface. TSAR is<br />pending. Further testing will be performed, all other objectives were met.<br /><br />HST CCS 4.0 Operational Readiness for Source/Destination Code testing scheduled<br />204/12:00Z - 16:00Z with GDOC, SOC, HITT, and CCS using CCS "G" String with<br />Release 4.0.1 and PRD D06100R2.<br /><br />HST IP Transition/CCC "B" String to VEST testing scheduled 204/13:00Z - 17:00Z<br />with GDOC, CCS, HITT, and VEST/DSTIF using CCS "B" String with CCS Release<br />4.0.1 and latest PRD release.