HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3211<br /><br />PERIOD COVERED: DOY 273<br /><br />OBSERVATIONS SCHEDULED<br /><br />NICMOS 8791<br /><br />NICMOS Post-SAA calibration - CR Persistence Part 2<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. The keyword 'USEAFTER=date/time' will also be added to the<br />header of each POST-SAA DARK frame. The keyword must be populated with the time,<br />in addition to the date, because HST crosses the SAA ~8 times per day so each<br />POST-SAA DARK will need to have the appropriate time specified, for users to<br />identify the ones they need. Both the raw and processed images will be archived<br />as POST-SAA DARKSs. Generally we expect that all NICMOS science/calibration<br />observations started within 50 minutes of leaving an SAA will need such maps to<br />remove the CR persistence from the science images. Each observation will need<br />its own CRMAP, as different SAA passages leave different imprints on the NICMOS<br />detectors.<br /><br />STIS/CCD 8907<br /><br />Spectroscopic Flats C10.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to obtain CCD flats in<br />the spectrographic mode.<br /><br />STIS/CCD 8908<br /><br />CCD Imaging Flats C10.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to investigate<br />flat-field stability over a monthly period.<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 9116<br /><br />Understanding High-Redshift and Starburst Galaxies: A UV Spectroscopic Survey of<br />B- Stars in the SMC.<br /><br />The Space Telescope Imaging Spectrograph [CCD and MA2] was used to construct a<br />high quality spectral library at low metallicity in order to synthesize the UV<br />spectra of high redshift star-forming galaxies and nearby starbursts.<br /><br />FGS/1 9171<br /><br />High Speed Photometry of the Transiting Planet HD 209458b.<br /><br />Fine Guidance Sensor #1 was used to observe HD 209458b, the only extrasolar<br />giant planet {EGP} detected that has an orbit inclined enough toward the Sun for<br />the transits to be detected. Differential photometry with respect to comparison<br />stars showed a transit depth of 1.5 a transit time of 3.2 hours. Transit ingress<br />and egress are ~25 minutes in duration suggesting the planet transits along a<br />short chord instead of the full stellar disk. It is proposed to observe the<br />transit ingress {1-orbit} and egress {1-orbit} with a FGS used as a high- speed<br />photometer.<br /><br />ACS 9281<br /><br />Complete Compact Object and Binary Survey of 47Tuc<br /><br />Our Cycle 1 observation of 47Tuc has shown its promise as the ultimate<br />laboratory for study of the production and evolution of compact binaries and<br />compact objects in globular clusters. We propose a deep {4x75ksec} ACIS-S<br />observation to measure the complete populations of millisecond pulsars {MSPs}<br />and cataclysmic variables {CVs} by their variability and spectra and to<br />constrain the main sequence binary population. Coordinated HST {ACS} data would<br />provide unique identifications of CVs and many MSPs and allow the full<br />population of quiescent low mass X-ray binaries to be distinguished from CVs.<br />This dataset would provide fundamental constraints for the origins of neutron<br />stars, millisecond pulsars, magnetic white dwarfs and compact binaries in<br />globular clusters.<br /><br />NICMOS 9321<br /><br />Dark current, shading profile, and read noise monitoring program<br /><br />for all three NICMOS cameras from the onset of normal NCS operations throughout<br />the start of Cycle 11.<br /><br />NICMOS 9360<br /><br />Paschen-alpha Imaging of a SIRTF-Selected Nearby Galaxy Sample<br /><br />We propose to carry out a NICMOS snapshot survey in the Paschen-alpha {PAlpha}<br />emission line and H-band of the sample of galaxies being observed at 3.5 -- 160<br />microns as part of SIRTF Nearby Galaxies Survey {SINGS} and a related guaranteed<br />time survey of starburst galaxies. The PAlpha images, accessible only from HST,<br />will be combined with groundbased HAlpha imaging to measure the extinction in<br />the star-forming centers of these galaxies, and obtain robust, extinction-<br />corrected maps of the massive star formation rate {SFR}. The PAlpha data by<br />themselves will provide reliable `extinction- free' SFRs, and a<br />cross-calibration of the {dust--affected} HAlpha-- and UV--based SFRs. The<br />PAlpha--based SFR measurements will extend the SFR-vs.-gas density law<br />{Schmidt--law} to surface densities at least 30 times higher than what is<br />accessible using HAlpha--based SFR measurements alone, bridging the gap between<br />normal galaxies and IR--luminous starbursts. Furthermore, the combination of the<br />HST PAlpha images with the SIRTF images and spectra, as well as ancillary<br />ground--based UBVRIJHK images and GALEX UV images being obtained as part of the<br />SINGS project, will provide a definitive study of the radiative transfer of<br />starlight and dust heating in star--forming galaxies. The processed NICMOS<br />images will be incorporated into the public SINGS Legacy Data Archive, to enable<br />scores of follow-up studies by the astronomical community at large.<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 />ACS/NICMOS 9483<br /><br />Origin and Evolution of IR Luminous Galaxies: Are z>=1 Dusty Starbursts and z=0<br />ULIRGs the Same?<br /><br />Interactions and mergers involving gas-rich galaxies are the main driving<br />mechanism behind the luminous IR galaxy phenomenon. However it is dangerous to<br />extrapolate this model directly to high redshifts because massive spiral<br />progenitors may have been relatively uncommon at earlier epochs. Mergers and<br />interactions involving less massive but more gas-rich progenitors may have<br />occurred instead. We propose to test this hypothesis directly by imaging 12<br />FIR-selected, dusty starbursts at z~1 at sub-kpc resolution afforded by HST in<br />the rest frame B and I {observed I and H} bands using ACS and NICMOS. While<br />studying higher redshift systems is clearly desirable, band-shifting and surface<br />brightness dimming makes the investigations of tidal features and the nature of<br />progenitors possible only out to z~ 1 {Hibbard & Vacca 1997}. From the<br />morphologies, surface brightnesses, and color distribution, we will determine<br />the physical status of the starburst hosts, the history of tidal<br />interactions/mergers, and the nature of the progenitors. We will also test for<br />the presence of hidden AGNs and for enhanced galaxy number density. Our 12<br />target galaxies form a complete sample of known ultraluminous and hyperluminous<br />galaxies at 0.7<z<1.4 and represent the most distant and the best statistical<br />set for investigating the nature and roles played by tidal interactions and<br />mergers in the dusty starburst phenomenon at high redshift.<br /><br />ACS 9564<br /><br />ACS Cycle 11: UV Earth Flats<br /><br />This proposal will obtain sequences of UV flats by observing the bright Earth.<br />The HRC UV filters were chosen for modes which were not obtained in the lab.<br />Since the UV transmission is likely to vary as a function of position on the<br />Pol_UV filters and on the coronograph, and since this behavior is currently<br />unconstrained by measurement, a good estimate for the missing UV flats cannot be<br />made. Although POL_UV and CORON transmissions change little at long wavelengths,<br />the UV transmission may change by amounts larger than can be estimated in the<br />absence of actual UV transmission measurements<br /><br />ACS/WFC 9584<br /><br />ACS Default {Archival} Pure Parallel Program II.<br /><br />WFPC2 9592<br /><br />WFPC2 CYCLE 11 Standard Darks<br /><br />calibration of the CCD dark current rate, and to monitor and characterize the<br />evolution of hot pixels. Over an extended period these data will also provide a<br />monitor of radiation damage to the CCDs.<br /><br />WFPC2 9593<br /><br />WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt1/3<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 />WFPC2 9596<br /><br />WFPC2 CYCLE 11 INTERNAL MONITOR<br /><br />This calibration proposal is the Cycle 11 routine internal monitor for WFPC2, to<br />be run weekly to monitor the health of the cameras. A variety of internal<br />exposures are obtained in order to provide a monitor of the integrity of the CCD<br />camera electronics in both bays {gain 7 and gain 15}, a test for quantum<br />efficiency in the CCDs, and a monitor for possible buildup of contaminants on<br />the CCD windows.<br /><br />CAL/WF2 9597<br /><br />Intflat Sweep, Visflat Sweep, and Filter Anomaly Check<br /><br />No abstract available.<br /><br />STIS 9605<br /><br />CCD Dark Monitor-Part 1<br /><br />Monitor the darks for the STIS CCD<br /><br />STIS 9607<br /><br />CCD Bias Monitor - Part 1<br /><br />Monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1<br />at gain = 4, to build up high-S/N superbiases and track the evolution of hot<br />columns.<br /><br />STIS/CAL 9609<br /><br />CCD Read Noise Monitor<br /><br />This proposal measures the read noise of all the amplifiers {A, B, C, D} on the<br />STIS CCD using pairs of bias frames. Full frame and binned observations are made<br />in both Gain 1 and Gain 4, with binning factors of 1x1, 1x2, 2x1 and 2x2. All<br />exposures are internals. Pairs of visits are scheduled for monthly execution.<br /><br />STIS 9633<br /><br />STIS parallel archive proposal - Nearby Galaxies - Imaging and Spectroscopy<br /><br />Using parallel opportunities with STIS which were not allocated by the TAC, we<br />propose to obtain deep STIS imagery with both the Clear {50CCD} and Long-Pass<br />{F28X50LP} filters in order to make color-magnitude diagrams and luminosity<br />functions for nearby galaxies. For local group galaxies, we also include G750L<br />slitless spectroscopy to search for e.g., Carbon stars, late M giants and S-type<br />stars. This survey will be useful to study the star formation histories,<br />chemical evolution, and distances to these galaxies. These data will be placed<br />immediately into the Hubble Data Archive.<br /><br />WFPC2 9676<br /><br />POMS Test Proposal: WFII parallel archive proposal<br /><br />used to take parallel images of random areas of the sky, following the<br />recommendations of the 2002 Parallels Working Group.<br /><br />STIS 9692<br /><br />STIS Pure Parallel Imaging Program: Cycle 10<br /><br />This is the default archival pure parallel program for STIS during cycle 10.<br /><br />Spacecraft 9695<br /><br />Guide Star Test for program 9453<br /><br />Guide Star Test<br /><br />FLIGHT OPERATIONS SUMMARY:<br /><br />COMPLETED OPS REQs: None<br /><br />OPS NOTES EXECUTED: None<br /><br />Significant Spacecraft Anomalies: [The following are preliminary reports of<br />potential non-nominal performance that will be investigated.] None<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 13 13<br />FGS REacq 4 4<br />FHST Update 25 25<br />LOSS of LOCK<br /><br />SIGNIFICANT EVENTS:<br /><br />Completed CCS-O-0013 ESTR & SSR Operations Test for OPS Readiness 4.0.1 testing<br />273/11:00Z - 15:00Z. Verified in telemetry all science and engineering records and<br />playback occurred correctly. Verified on Events Page files were opened and the<br />playbacks were being processed correctly by the ground system. Modifications were<br />make to the script to better clarify SOC's file structure.<br /><br />HST Checkout of ANCC Interface Test from IP Packet Filter scheduled 274/12:30Z - 20:00Z<br />with WSC TC, GDOC, HITT, I&C, and CCS using CCS "C" String with CCS Release 4.0.1 and<br />PRD D06100R2. The purpose of this testing is to verify CCS Release 4.0.1 IP Mode is<br />capable of interfacing through the IP Packet Filters to the ANCC for ODMs and GCMRs.