HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3139<br /><br />PERIOD COVERED: DOY 168<br /><br />OBSERVATIONS SCHEDULED:[see HSTARS below for possible observation problems]<br /><br />STIS/CCD/MA2 8614<br /><br />NUV Extension of the Arcturus Project: Probing the Onset of Chromospheric<br />Heating.<br /><br />The Space Telescope Imaging Spectrograph [CCD and MA2] was used to observe two<br />stars that have multi-wavelength atlases at resolutions high enough to resolve<br />dynamically interesting line structure: the Sun {G2 V} and Arcturus {K2 III}.<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/CCD/MA1/MA2 8916<br /><br />Spectroscopic Sensitivity Workout: First-order Modes.<br /><br />The Space Telescope Imaging Spectrograph [CCD, MA1 and MA2] was used to measure<br />the basic sensitivity for all supported MAMA and CCD first-order spectroscopic<br />modes. Sensitivity measurements are done for all supported tilts of the<br />gratings, at a S/N suitable to any particular setting, in order to get all<br />measurements done in a reasonable number of orbits but still get a very accurate<br />sensitivity measurement.<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 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 />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 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 />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 />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 />ACS/WFC 9584<br /><br />ACS Default {Archival} Pure Parallel Program II.<br /><br />The Advanced Camera for Surveys [WFC] was used to test ACS pure parallels.<br /><br />FLIGHT OPERATIONS SUMMARY:<br /><br />HSTARS: [For details ]http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf]<br /><br />8705 - Equation Display Utility Does not show "<" symbol @ 168/1800z<br /> The Equation Display Utility does not show the "less than"<br /> symbol ["<"] in equation descriptions. The attachments show<br /> an equation as displayed on the CCS-A EQUATION EDITOR<br /> [which includes the "<" symbols], and on the EQUATION DISPLAY<br /> UTILITY [which does not show the "<" symbol]. Under investigation.<br /><br />COMPLETED OPS REQs:<br />16788-0 - Gyro Motor Current Max Count Limit Change @ 168/1521z<br /> Successfully patched Gyro 3 motor current timer limit from<br /> 90 seconds to 300 seconds [OR 16788]. During a recent anomaly<br /> Gyro 3 motor current indicated a value near the existing gyro<br /> motor current maximum error count of 3600 counts. Project has<br /> directed this increase to 12000 counts to avoid ZGSP entry.<br /> The DMS configuration tracking table will be updated to reflect<br /> this change.<br /><br />OPS NOTES EXECUTED: None<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 6 6<br />FGS REacq 9 9<br />FHST Update 17 16 168/2143z<br />LOSS of LOCK None<br />Operations Notes:<br /><br />SIGNIFICANT EVENTS:<br /><br />Continuation of Servicing Mission Orbital Verification and the gradual<br />resumption of normal science observations and calibrations.