HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3159<br /><br />PERIOD COVERED: DOY 198<br /><br />OBSERVATIONS SCHEDULED [see HSTARS below for possible observation problems]<br /><br />WF/PC-2/STIS/CCD 8624<br /><br />Imaging and Spectroscopy of Dusty Circumstellar Disks.<br /><br />The WF/PC-2 and the Space Telescope Imaging Spectrograph [CCD] were used to<br />further understanding of the properties and evolution of dusty disks in the<br />circumstellar environments of young stars which is a key element in furthering<br />our concepts of the formation mechanisms of extra-solar planetary systems.<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 />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 9317<br /><br />Pure Parallel Imaging Program: Cycle 10.<br /><br />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/HRC 9391<br /><br />High-Resolution Imaging of Pluto's Surface<br /><br />We will collect a series of observations with the ACS/HRC from which we will<br />derive a two-color global map of Pluto's surface. We will image Pluto at F435W<br />and F555W, wavelengths that have been extensively studied from the ground over<br />the past 50 years. The maps will provide albedos with accurate error<br />determinations down to 52 degrees South latitude. These observations will<br />provide a second epoch of HST mapping of the active surface of Pluto as it<br />continues to recede from the Sun and will provide an important context for other<br />detailed studies of Pluto.<br /><br />ACS 9427<br /><br />Globular Cluster Systems in Supergiant E Galaxies<br /><br />clusters {Brightest Cluster Galaxies}. It is among this BCG class that the<br />characteristics of globular cluster systems display their widest range in<br />metallicity distribution and specific frequency and thus confront galaxy<br />formation models with their most varied challenges. Were these systems built<br />primarily by early in situ conversion of gas clouds, by later mergers, or by<br />ongoing accretions of dwarfs? Their extensive halo cluster systems contain many<br />clues to these relic events. BCGs are the biggest and rarest type of galaxy, and<br />to date the globular clusters in only two BCGs {M87, NGC 1399} are well studied.<br />The ACS camera now brings many more such systems within reach. We propose to<br />image the globular cluster systems in 13 BCGs in the distance regime cz ~eq 2000<br />- 5000 km s^-1. With deep {B, I} exposures we will measure the globular cluster<br />metallicity distribution functions, specific frequency, radial distributions,<br />and luminosity distributions, as well as correlations among these quantities.<br />This work will be the first comprehensive, homogeneous deep survey of globular<br />clusters in BCGs. The superior area and sensitivity of ACS will yield a gain of<br />a factor of eight over previous WFPC2 studies for sample size and metallicity<br />discrimination.<br /><br />GO 9461<br /><br />HST / Chandra Monitoring of the M87 Jet<br /><br />We propose to correlate the X-ray variability of the M87 jet against<br />morphological changes and variability seen in high resolution HST optical/UV<br />observations. We have already been granted Chandra bi-monthly monitoring between<br />Nov. 2001 and Aug. 2002, as well as HST observations in Nov. 2001. Here we<br />propose for a second HST epoch in Aug. 2002 which will allow measurement of<br />optical/UV variability and morphological changes during the Chandra run. These<br />observations will elucidate the X-ray emission mechanism for the jet.<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 9472<br /><br />A Snapshot Survey for Gravitational Lenses among z >= 4.0 Quasars<br /><br />Over the last few years, the Sloan Digital Sky Survey has revolutionized the<br />study of high-redshift quasars by discovering over 200 objects with redshift<br />greater than 4.0, more than doubling the number known in this redshift interval.<br />The sample includes eight of the ten highest redshift quasars known. We propose<br />a snapshot imaging survey of a well-defined sample of 250 z > 4.0 quasars in<br />order to find objects which are gravitationally lensed. Lensing models including<br />magnification bias predict that at least 4% of quasars in a flux-limited sample<br />at z > 4 will be multiply lensed. Therefore this survey should find of order 10<br />lensed quasars at high redshift; only one gravitationally lensed quasar is<br />currently known at z > 4. This survey will provide by far the best sample to<br />date of high-redshift gravitational lenses. The observed fraction of lenses can<br />put strong constraints on cosmological models, in particular on the cosmological<br />constant Lambda. In addition, magnification bias can significantly bias<br />estimates of the luminosity function of quasars and the evolution thereof; this<br />work will constrain how important an effect this is, and thereby give us a<br />better understanding of the evolution of quasars and black holes at early<br />epochs, as well as constrain models for black hole formation.<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/WFC 9492<br /><br />Extragalactic Distances: the Need for Accurate Photometry of Blue Supergiants<br />and Cepheids<br /><br />The investigation of the Wind Momentum-Luminosity Relationship {WLR} of blue<br />supergiant stars as an independent extragalactic distance indicator has reached<br />a critical phase. Following our recent discovery and spectroscopic follow-up of<br />several tens of stars outside of the Local Group in NGC 300 and NGC 3621, we can<br />now calibrate the WLR in terms of spectral subtype and metallicity with a higher<br />accuracy than hithertho possible with the statistically limited samples<br />available in the nearby galaxies studied so far. This, however, requires<br />high-resolution imaging to obtain accurate BVI photometry of a significant<br />fraction of those stars for which we have spectroscopic information. This can be<br />effectively accomplished with eight ACS/WFC fields in these two galaxies. As a<br />further step, we can use the calibrated WLR to measure the first independent<br />extragalactic distance. We then propose additional imaging of six ACS/WFC fields<br />in M101 to select blue supergiant candidates for spectroscopic follow-up. Having<br />recently discovered more than a hundred new Cepheids in NGC 300, the<br />high-resolution imaging proposed for the photometry of blue supergiants can also<br />be used, with no additional observing effort, to verify the effects of blending<br />on the Cepheid distance to this galaxy, an important calibrator of secondary<br />distance indicators.<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 9566<br /><br />CCD Hot Pixel Annealing.<br /><br />The Advanced Camera for Surveys [WFC and HRC] was used to perform hot pixel<br />annealing that will be performed once per month. The CCD TECs will be turned off<br />and heaters will be activated to bring the WFC detector temperature to about<br />+10C. The HRC temperature will reach about 30C. This state will be held for<br />approximately 24 hours, after which the heaters are turned off, the TECs turned<br />on, and the CCDs returned to normal operating condition.<br /><br />STIS 9618<br /><br />STIS MAMA Dispersion Solutions<br /><br />Obtain wavecals just deep enough to constrain wavelength and spatial distortion<br />maps without overusing the calibration lamp. For the first time on orbit, data<br />will be obtained at all available central wavelengths. This information will<br />help constrain global models of STIS optical performance being developed at ECF<br />and STScI. During the observations, MSM monthly offsets will be set to zero to<br />complement observations over the past couple of cycles, which occurred at extreme<br />monthly offsets. The echelle observations at zero offset will yield dispersion<br />solutions that are directly applicable to all echelle science data obtained<br />after monthly offsets are disabled.<br /><br />ACS 9665<br /><br />Extreme Red Stars<br /><br />ACS provides unprecedented sensitivity in the far red, this coupled with recent<br />astronomical pushes to ever cooler objects {e.g. new classifications for L and T<br />stellar dwarfs, and extremely high redshift galaxies} increases the need for<br />extending the photometric calibration to include such objects. We propose<br />observations of 4 stellar objects for which excellent ground based optical and<br />near-IR data exist that span V-I colors of 4.5 at M7 to > 6.0 at L5.<br /><br />FLIGHT OPERATIONS SUMMARY:<br /><br />HSTARS: [For details see ]http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf]<br />HSTARS: None<br /><br />COMPLETED OPS REQs: None<br /><br />OPS NOTES EXECUTED: None<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 7 7<br />FGS REacq 8 8<br />FHST Update 19 19<br />LOSS of LOCK None<br /><br />Operations Notes: None<br /><br />SIGNIFICANT EVENTS:<br />Successfully completed CCS Release 4.0.1 Ops Readiness 486 Ephemeris Generation/Uplink<br />testing on Day 198. Objectives of test were to verify routine operational procedures<br />and CCS capabilities to support HST 486 ephemeris file transmittal from STScI via PNMs,<br />SAC table load generation QA checks/signoff, uplink and transfer of post ephemeris<br />information to STScI via PNMs. SAC personnel delivered a 486 ephemeris TCL to Core for<br />use in HST 486 ephemeris uplink on Day 200.<br /><br />PASS Release 31.65 was successfully placed into formal operations 7/17/02 on the SOGS<br />cluster. Aliveness testing of the new software was successfully performed. The look-alike<br />areas on STOSC for operational images [OP, OP_NEW, and OP_OLD on DISK$SPST_MS] were not<br />affected by this release. The new image, LCHK.EXE and the updated error message file,<br />ERROR.ERM were unloaded into the OP area. For details of this release see<br />URL: http://pasbye.hst.nasa.gov/ sepg/release/reltable.htm.