HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3160<br /><br />PERIOD COVERED: DOY 199<br /><br />OBSERVATIONS SCHEDULED [see HSTARS below for possible observation problems]<br /><br />WFPC2 8183<br /><br />Morphology of the most massive galaxies in the early universe<br /><br />High redshift radio galaxies {HzRGs} are fundamentally important probes of<br />galaxy and cluster formation. They are amongst the most massive galaxies in the<br />early Universe and located in dense cluster environments. Our previous WFPC2<br />data have revealed that HzRGs are remarkably clumpy on a sub-kiloparsec scale,<br />reminiscent of simulations of forming massive ellipticals. Surprisingly our<br />NICMOS images often show clumpy aligned morphologies unlike those expected from<br />an old elliptical population. There is a wide diversity in HST morphologies and<br />colour distributions for the 9 objects for which we have both WFPC and NICMOS<br />images. We propose to observe obtain WFPC2 images of 10 additional z ~ 2 radio<br />galaxies for which we have NICMOS but no WFPC2 images. The new data will be used<br />to {i} determine the range of clumps colour distributions, thereby constraining<br />the formation history and the nature of the radio/optical alignment effect {ii}<br />compare them with the colours of Lyman--bre ak galaxies {iii} compare them with<br />dust properties and the surmised axis of the jet orientation {iv} confirm<br />relationships between clumpiness and other HzRG properties indicated by our<br />present small sample. These observations will comprise part of a multiwavelength<br />study of HzRGs, involving SCUBA on the JCMT as well as Keck and the VLT.<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 />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 />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 />ACS 9025<br /><br />Scattered Light in Coronographic Observations<br /><br />The scattered-light suppression of the HRC coronagraph will be examined by<br />obtaining several exposures of an occulted star through F435W, F606W, and F814W,<br />as a function of position behind each coronagraphic mask.<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 />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/HRC 9379<br /><br />Near Ultraviolet Imaging of Seyfert Galaxies: Understanding the Starburst-AGN<br />Connection<br /><br />We propose a near-UV snapshot survey of 101 Seyfert galaxies using ACS/HRC and<br />the filter F330W, a configuration which is optimal to detect faint star forming<br />regions around their nuclei. These images will complement optical and near-IR<br />images available in the HST archive, thus providing a panchromatic atlas of the<br />inner regions of active galaxies, which we will use to study the starburst-AGN<br />connection. The main goals of this proposal are: {1} Determine the frequency of<br />circumnuclear starbursts in Seyferts, down to levels which cannot be observed<br />from the ground; {2} characterize the observational {fluxes, colors, structure,<br />sizes} and intrinsic {luminosities, masses, ages, global star-formation rate}<br />properties of these clusters; {3} derive the luminosity functions of young star<br />clusters around the nucleus of Seyferts and compare these results with those<br />from normal and starburst galaxies to determine their survival rate close to the<br />AGN; {4} address questions about the relation between AGNs and starbursts, like<br />the possible connection between the masses and luminosities of black holes and<br />starbursts, and the implications for the evolution of the black holes and their<br />host galaxy bulges. By adding UV images to the existing optical and near-IR<br />ones, this project will create an extremely valuable database for astronomers<br />with a broad range of scientific interests, from the properties of the AGN to<br />the properties of their host galaxies.<br /><br />SNAP/STIS 9434<br /><br />A SNAPSHOT Survey of the Hot Interstellar Medium<br /><br />We propose to obtain SNAPSHOT STIS echelle observations of key tracers of hot<br />interstellar gas {CIV, NV and SiIV} for selected FUSE Team OVI survey targets<br />with known UV fluxes. By taking advantage of the SNAPSHOT observing mode we will<br />efficiently obtain a large number of spectra suitable for the study of the<br />highly ionized hot component of the interstellar medium {ISM}. Our goals are to<br />explore the physical conditions in and distribution of such gas, as well as to<br />explore the nature of the interfaces between the hot ISM and the other<br />interstellar gas phases. Using inter--comparisons of the various ionic ratios<br />for CIV, NV, OVI and SiIV, we will be able to discriminate between the various<br />models for the production of the highly ionized gas in the Galactic ISM. The<br />survey will also enable detailed studies of regions already known to contain hot<br />gas through X-ray emission measurements {e.g., SNRs and radio loops}. The<br />proposed SNAPSHOT observations will extend our previous Cycle 9 survey {which<br />was compromised by the STIS side 1 failure}, and should roughly double the<br />number of stars for which high quality STIS observations of the important hot<br />gas tracers are available, enabling us to derive a truly global view of the hot<br />ISM.<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 />STIS/ACS 9498<br /><br />The Nature of the Close Binary Quasar LBQS 0103-2753<br /><br />We propose STIS spectroscopic and ACS imaging observations of the<br />small--separation quasar pair LBQS 0103-2753 A/B {= CT 344}. This quasar pair<br />with z = 0.85, has a projected separation of only 0.3 arcsec or 2.3 kpc. The<br />brighter member of the pair {V = 18.2} is a BAL quasar while the fainter {V =<br />19.4} is a quasar at a similar redshift without BALs. It is very likely that the<br />two quasars are a binary quasar, and not a chance superposition along the line<br />of sight or a gravitational lens {Junkkarinen et al. 2001}. The goals of the<br />STIS spectroscopic observations are to accurately measure the systemic redshifts<br />and redshift difference, to search for variability, and to quantify the emission<br />line differences between the two quasars. Deep ACS WFC images, in the F606W and<br />F814W filters, will be used to provide information on the host galaxy<br />morphologies, to look for the signatures of a merger/interaction -- in<br />particular disturbed isophotes and tidal tails, and to study any cluster of<br />galaxies around this quasar pair. These observations will test the lensing<br />versus binary hypothesis and help differentiate between merging and a high<br />relative velocity galaxy--galaxy interaction. Studies of binary quasars with<br />such close separations will put constraints on merger timescales and duty cycles<br />for AGN fueling at these separations.<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 />FLIGHT OPERATIONS SUMMARY:<br /><br />HSTARS: [For details see ]http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf]<br /><br />8739 - Magnetic Torquers Flag Prior tp Predicted SAA Entry @200/0124z.<br /> OOL which are usually routine during an SAA event, began toggling<br /> in-and-out of limits six minutes prior to predicted SAA entry.<br /> At 200/01:24:18Z, Magnetic Torquer Magnetic Moment Command [GMT2AMM]<br /> began toggling in-and-out of limits high with a value of 2822.4.<br /> Limit is 2822. Highest value reached was 2908.8. Magnetic Torquer<br /> Current [GMT2AMC] toggle between high limit of 0.7056 and 0.7308.<br /> Predicted SAA entry was 200/01:30:22Z. MSS 1 Magnitude Squared [SMS1MSQ]<br /> also toggle in-and-out of limits beginning at 200/01:39:23Z. Guiding on<br /> FGSs during this time. FHST Map @ 200/01:25Z showed errors of<br /> 66.395, -0.228, and 7.769. At 200/01:57Z, showed 63.345, -2.127, and<br /> 3.797. These mnemonics will occasionally break limits due to SAA 1 events<br /> or when the solar flux is very low causing the torquer bars to use more<br /> current to provide more torque against a weaker magnetic field. Under<br /> investigation.<br /><br />COMPLETED OPS REQs: None<br /><br />OPS NOTES EXECUTED: None<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 11 11<br />FGS REacq 8 8<br />FHST Update 14 14<br />LOSS of LOCK None<br /><br />Operations Notes: None<br /><br />SIGNIFICANT EVENTS:<br />HST CCS 4.0 Operational Readiness for Load Uplink, Dump, and Compare<br />and 486 Ephemeris Generation Uplink testing scheduled 200/11:00Z - 20:00Z<br />with GDOC, SOC HITT, DMS, and CCS using CCS "G" String with CCS<br />Release 4.0.1 and PRD D06100R2.