HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3146<br /><br />PERIOD COVERED: DOY 177<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 />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 9043<br /><br />Cepheid Distances to Early-type Galaxies.<br /><br />The WF/PC-2 was used to continue observations in the HST Key Project on the<br />Extragalactic Distance Scale and the HST project on the "Calibration of Nearby<br />Type Ia Supernovae'' that have greatly improved our knowledge of the Hubble<br />Constant by providing a solid zero point for the Tully- Fisher {TF} relation and<br />Type Ia Supernovae {SNIa}. However, severe inconsistencies remain for distance<br />estimators to early-type galaxies such as surface brightness fluctuations {SBF},<br />the planetary nebula luminosity function {PNLF}, the fundamental plane {FP}, and<br />the globular cluster luminosity function {GCLF}. As a result, the distance to<br />the Virgo cluster core remains uncertain by as much as 20 determination is<br />directly affected by a lingering 0.1 mag {5 uncertainty in the photometric<br />calibration of the WFPC2. Resolving these issues is essential not only to firm<br />up the extragalactic distance scale, but also to understand the mass and<br />velocity structure of the local universe. SBF in particular is emerging as the<br />method of choice for mapping local velocity fields to 10, 000 kms because it<br />offers an order of magnitude less Malmquist bias than TF, and SNIa are too rare<br />to study large scale flows effectively. This project will tighten the<br />photometric calibration of the WFPC2, and provide a solid Cepheid calibration<br />for SBF and PNLF.<br /><br />STIS/CCD/MA1 9051<br /><br />Identifying Damped Lyman-alpha Galaxies at z~1.<br /><br />The Space Telescope Imaging Spectrograph [CCD and MA1] was used to look for<br />damped Lyman-alpha absorption systems that contain the bulk of the neutral gas<br />in the Universe in the redshift range z = 0.5 - 5, yet the nature of the<br />galaxies responsible for the absorption is not well understood. Only recently<br />have observers found more than a handful of damped absorbers at redshifts z <<br />1.5. Using the FIRST Bright Quasar Survey {FBQS}, with over a 1000 quasars, the<br />proposers have undertaken a survey to build a complete picture of he nature of<br />the galaxies responsible for damped Lyman-alpha absorption systems at z~1 and to<br />double the sample size at this redshift.<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/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 />NICMOS 9269<br /><br />NICMOS Parallel Thermal Background<br /><br />SMOV to establish the stability of the HST+NCS+Instrument thermal emission.<br /><br />ACS/HRC/WFC 9292<br /><br />The Nature of Galaxies at z > 4<br /><br />number of galaxies and quasars at redshifts greater than 5 that has identified<br />the z>5-6 epoch as key to understanding the earliest formation phases for<br />galaxies. However, establishing the characteristics and properties of these<br />earliest galaxies is proving to be a particularly difficult. They are faint,<br />with I{AB} magnitudes around 26-27. Thus, substantial investments of time are<br />needed to obtain high S/N images, while ground-based spectroscopy, even with<br />8-10 m class telescopes, has provided little more than redshifts. Establishing<br />the physical properties of these galaxies will be a challenge for the<br />foreseeable future. However, there is a subset of this high redshift population<br />that is amenable to more detailed study. These are sources that have been<br />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 9353<br /><br />Direct imaging of the progenitors of massive, core-collapse supernovae<br /><br />Modern supernovae searches in the nearby Universe are discovering vast numbers<br />of SNe which have massive star progenitors {Types II, Ib and Ic}. The extensive<br />HST {and ground-based} image archives of galaxies within ~20 Mpc enables their<br />individual bright stellar content to be resolved. As massive, evolved stars are<br />the most luminous single objects in a galaxy, the progenitors of core-collapse<br />SNe should be directly detectable on pre-explosion images. Within the last year<br />we have set direct mass limits on the progenitors of two SNe Type II-P by<br />analyzing pre-explosion archive images and follow up HST exposures. We have now<br />identified six other recent, nearby SNe which have WFPC2 archive exposures of<br />the site taken before explosion. Additionally, our Cycle 10 SNAP program will<br />double the WFPC2 image archive of nearby galaxies which significantly increases<br />the chances of having multi-colour photometry of pre-explosion sites for future<br />SNe. In this Cycle, we request time on two fronts. Firstly we require imaging of<br />the six SNe with existing pre-explosion data in order to perform exact<br />astrometry of the SNe positions to around 0.05''. Secondly, as a follow on from<br />our two successful Cycle 10 programs, we request ToO status for any nearby<br />core-collapse SN which explodes during Cycle 11 and which has pre-explosion HST<br />images. The goal of this proposal is to directly identify the progenitor stars<br />of core-collapse SNe.<br /><br />ACS/HRC 9473<br /><br />Masses and IMF Variations in Super Star Clusters<br /><br />We are proposing to obtain high spatial resolution images of a set of super star<br />clusters for which we have been granted observing time to measure velocity<br />dispersions via high- resolution ground-based optical echelle and K-band<br />spectroscopy. The images will allow us to fit the light profiles and measure the<br />radii of the clusters, and when combined with the velocity dispersions, will<br />enable us to estimate the cluster masses. By comparing the mass-to-light ratios<br />with those predicted from spectral synthesis models, we will investigate<br />possible variations in the slope and lower mass cut-offs of the initial mass<br />functions in these clusters. Correlations of the variations of these parameters<br />with cluster environment may provide insight into the formation mechanisms for<br />super star clusters. By comparing the light profiles obtained in a blue and red<br />filter, we will also search for evidence of mass segregation in the clusters.<br />Since these clusters are too young to have experienced dynamical mass<br />segregation, differences in the light profiles of the clusters in the two<br />filters could be due to processes that differentiate between high and low mass<br />stars during the birth of the clusters and would provide further constraints on<br />theoretical models of cluster formation. Since these clusters are far too<br />compact to be resolved by any ground-based observations, the ACS/HRC on board<br />HST is the only instrument capable of carrying out these observations.<br /><br />STIS 9499<br /><br />Brown Dwarf Binaries as Tests of Substellar Evolution<br /><br />We propose to obtain STIS spectroscopy of two brown dwarf binaries for which<br />dynamical masses are being obtained by monitoring the orbital motion using<br />ground-based telescopes with adaptive optics. The HST/STIS spectra will allow to<br />study the LiI resonance line at 670.8 nm. The lithium depletion of the members<br />of these binaries will be estimated with the aid of synthetic spectra. These<br />observations will be compared to model predictions of lithium depletion as a<br />function of age and mass, and hence will provide an observational test to the<br />theory of substellar objects. Spin-offs will be the measurement of the strength<br />of Halpha emission, an indicator of chromospheric activity in cool atmospheres,<br />and comparing the shape of the optical continuum with model spectra with<br />different dust opacities.<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 9567<br /><br />SBC Dark Current<br /><br />Dark current measurements will be made for the ACS SBC once a week.<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 />FLIGHT OPERATIONS SUMMARY:<br /><br />HSTARS: [For details see ]http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf]<br /><br />8715 Low + Wing Panel Temperature @ 177/17:03:32z At 177/17:03:32, B%WPANLT<br /> [+ wing panel temperature] flagged to a yellow low limit of -81.2765<br /> degrees C for 4 minutes 12 seconds [back in bounds at 17:07:44]. The<br /> yellow low limit is -80.0 degrees C, the yellow high limit is 77.0<br /> degrees C, and the sample rate is every six seconds. The violation<br /> occurred during the last four minutes of orbit night. Under investigation.<br /><br />8716 Roll Delay Tracker Update Failed @ 177/17:24:32z.On day 177, U2,3RD at<br /> 17:24:32 failed due to tracker 3. The following guide star acquisition<br /> was successful. Under investigation.<br /><br />COMPLETED OPS REQs:<br />16792-0 NICMOS C-Spot Gain Table FSW Uplink<br /><br />OPS NOTES EXECUTED:<br />1020-0 RWA Limit Adjustment<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 9 9<br />FGS REacq 7 7<br />FHST Update 20 20<br />LOSS of LOCK None<br />Operations Notes:<br /><br />COMMENTS: None<br /><br />SIGNIFICANT EVENTS: Successfully completed NICMOS Coronagraphic<br />Spot Gain Table EDAC RAM and EEPROM uplink [NICMOS SCR 37] @ 177/19:00Z<br />[OR 16792 and Script fswscr37install_ops_rev1.doc]. This update included<br />the latest numbers supplied by U of A. This modification is needed for<br />observations scheduled in SMS 189.