HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3163<br /><br />PERIOD COVERED: DOY 204<br /><br />OBSERVATIONS SCHEDULED [see HSTARS below for possible observation problems]<br /><br />STIS 8564<br /><br />Measuring the Evolution of the UV Upturn<br /><br />We propose far-ultraviolet observations of CL1358+62, a rich, well-studied<br />cluster of galaxies at z =0.33. These observations will provide the first<br />completely unambiguous measurement of far-UV emission in quiescent ellipticals<br />at moderate redshift. Theoretically, the strength of far-UV emission {relative<br />to flux at longer wavelengths} is the most rapidly evolving feature in<br />elliptical galaxies. Models suggest that this ``UV upturn'' can change by a<br />factor of 25 over a few Gyr, and it is expected to fade rapidly with increasing<br />redshift. Surprisingly, the Faint Object Camera {FOC} found strong far-UV<br />emission in four elliptical galaxies at z=0.375, suggesting no evolution in this<br />diagnostic between our own epoch and one 4 Gyr earlier. However, the FOC<br />measurement was particularly susceptible to systematic errors, and it was<br />limited to a small number of galaxies in just one cluster. In contrast to the<br />FOC results, recent Space Telescope Imaging Spectrograph {STIS} observations at<br />z=0.55 obtained very weak detections of ellipticals at higher redshift, as<br />expected for ellipticals much younger than those in our own epoch. Observations<br />with the STIS far-UV camera are not subject to the uncertainties of the FOC<br />measurements, because the STIS camera is blind to flux at longer wavelengths.<br />Our observations of CL1358+62 will unambiguously test the apparent lack of<br />evolution in the UV upturn over the past 4 Gyr.<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 />ACS/WFC/HRC 9075<br /><br />Cosmological Parameters from Type Ia Supernovae at High Redshift.<br /><br />The Advanced Camera for Surveys [WFC and HRC] was used to obtain a Hubble<br />diagram of Type Ia supernovae {SNe Ia} that will be of long lasting value as a<br />record of the expansion history of the universe.<br /><br />STIS/CCD/MA1/MA2 9113<br /><br />Solar UV Radiation and the Origin of Life on Earth.<br /><br />The Space Telescope Imaging Spectrograph [CCD, MA1 and MA2] was used to observe<br />chromospheric models that will enable the proposers to predict the extreme-UV<br />emission of the early Sun and its consequences for the erosion of the early<br />Earth's atmosphere and the altered oxidation state of the planet, and<br />investigate the effect of metallicity on the UV emission and its consequences<br />for the photochemistry of Earth-like planets.<br /><br />STIS/CCD 9317<br /><br />Pure Parallel Imaging Program: Cycle 10.<br /><br />program for STIS during cycle 10.<br /><br />FGS/WFPC2 9334<br /><br />Dynamical Masses of White Dwarfs from Resolved Sirius-Like Binaries<br /><br />white-dwarf companions of cooler main-sequence stars. Out of 17 systems observed<br />to date, 8 have been resolved with WFPC2 by using UV filters. Two of the<br />resolved systems---56 Persei and Zeta Cygni---have predicted or known orbital<br />periods short enough that dynamical masses can be determined for the white<br />dwarfs within reasonable times. These would thus add to the extremely small<br />number of white dwarfs presently having accurately and directly measured masses.<br />We propose to image them annually in the UV with WFPC2. In addition, we will<br />observe Zeta Cyg with FGS in order to measure the absolute motion of the optical<br />component, needed for the mass solution. We also propose to observe Sirius<br />itself with WFPC2 over the next 3 Cycles. The resulting astrometric data will<br />not only greatly improve the precision of the binary orbit and the dynamical<br />mass measurements for both the main-sequence and white-dwarf components, but<br />will also test definitively for the claimed presence of a third body in this<br />famous system.<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 />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 />NICMOS 9484<br /><br />The NICMOS Parallel Observing Program<br /><br />We propose to manage the default set of pure parallels with NICMOS. Our<br />experience with both our GO NICMOS parallel program and the public parallel<br />NICMOS programs in cycle 7 prepared us to make optimal use of the parallel<br />opportunities. The NICMOS G141 grism remains the most powerful survey tool for<br />Halpha emission-line galaxies at cosmologically interesting redshifts. It is<br />particularly well suited to addressing two key uncertainties regarding the<br />global history of star formation: the peak rate of star formation in the<br />relatively unexplored but critical 1<= z <= 2 epoch, and the amount of star<br />formation missing from UV continuum-based estimates due to high extinction. Our<br />proposed deep G141 exposures will increase the sample of known HAlpha emission-<br />line objects at z ~ 1.3 by roughly an order of magnitude. We will also obtain a<br />mix of F110W and F160W images along random sight-lines to examine the space<br />density and morphologies of the reddest galaxies. The nature of the extremely<br />red galaxies remains unclear and our program of imaging and grism spectroscopy<br />provides unique information regarding both the incidence of obscured star bursts<br />and the build up of stellar mass at intermediate redshifts. In addition to<br />carrying out the parallel program we will populate a public database with<br />calibrated spectra and images, and provide limited ground- based optical and<br />near-IR data for the deepest parallel fields.<br /><br />SNAP 9485<br /><br />Completing A Near-Infrared Search for Very Low Mass Companions to Stars within<br />10 pc of the Sun<br /><br />Most stars are fainter and less massive than the Sun. Nevertheless, our<br />knowledge of very low mass {VLM} red dwarfs and their brown dwarf cousins is<br />quite limited. Unknown are the true luminosity function {LF}, multiplicity<br />fraction, mass function, and mass-luminosity relation for red and brown dwarfs,<br />though they dominate the Galaxy in both numbers and total mass. The best way to<br />constrain these relations is a search for faint companions to nearby stars. Such<br />a search has several advantages over field surveys, including greater<br />sensitivity to VLM objects and the availability of precise parallaxes from which<br />luminosities and masses can be derived. We propose to complete our four-filter<br />NICMOS snapshot search for companions to stars within 10 pc. With a 10 sigma<br />detection limit of M_J ~ 20 at 10 pc, we can detect companions between 10 and<br />100 AU that are at least 9 mag fainter than the empirical end of the main<br />sequence and at least 6.5 mag fainter than the brown dwarf Gl 229B. When<br />completed, our search will be the largest, most sensitive, volume-limited search<br />for VLM companions ever undertaken. Our four-filter search will permit<br />unambiguous identification of VLM-companion candidates for follow-up<br />observation. Together with IR speckle and deep imaging surveys, our program will<br />firmly establish the LF for VLM companions at separations of 1-1000 AU and the<br />multiplicity fraction of all stars within 10 pc.<br /><br />Note: These observations taken for proposal 9485 were lost because the NIC safed at<br />July 23, 2002 03:42 before the execution of your visit. See HSTAR 8744.<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 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 />WFPC2 9676<br /><br />POMS Test Proposal: WFII parallel archive proposal<br /><br />This is the generic target version of the WFPC2 Archival Pure Parallel program.<br />The program will be used to take parallel images of random areas of the sky,<br />following the recommendations of the 2002 Parallels Working Group.<br /><br />POMS 9677<br /><br />POMS Test Proposal: WFII backup parallel archive proposal<br /><br />This is a POMS test proposal designed to simulate scientific plans.<br /><br />FLIGHT OPERATIONS SUMMARY:<br /><br />HSTARS: [For details see ]http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf]<br /><br />8745 - Scan Step Limit Exceeded 3 times during Reacq @204/1733z.<br /> FGS 2 and 3 acquired fine lock during REACQ at 17:32:39<br /> but FGS 2 walkdown failed three times, causing loss of lock<br /> at 17:34:56, 17:35:34 and 17:36:12. In spite of these problems,<br /> REACQ was successful, no observations affected. Under investigation.<br /><br />8746 - Commanding problem on C-string @204/2200z.HSTAR 8746:FOT requested<br /> to move real-time NCC and Command to "C" String due to "A" String<br /> problem. NCC worked but not Command, refreshed the Command visn<br /> cd1 - port 3 crosspoint twice and still saw no clock and CD Manager<br /> didn't see commands leaving. Hard patched around HRS, still no clock,<br /> checked terminal timing connected to VEDA box, still saw nothing.<br /> Requested CD Manager re-boot CD visn cd1-port3, after re-boot, CD<br /> Manager saw clock and FOT was able to send out a good command.<br /> Under investigation.<br /><br />COMPLETED OPS REQs:<br />16802-0 - CCC/VIK K52 Level Change [level 4] @204/1436z<br />16803-0 - Recover NICMOS from Suspend @204/1459z<br /><br />OPS NOTES EXECUTED:<br />1025-1 - CCC K52 Level 3 limits @204/1949z<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 8 8<br />FGS REacq 3 3<br />FHST Update 17 17<br />LOSS of LOCK 3 lol-204/1734:56,1735:34,<br /> 1736:12z [HSTAR 8745]<br /><br />Operations Notes: NICMOS Suspended @204/0342z [HSTAR 8744]-<br />NICMOS Memory dump @204/0640z.[Rop NS-9].<br /><br />SIGNIFICANT EVENTS:<br /><br />Successfully changed CCC/VIK K52 to Level 4 @ 204/14:35:33Z<br />[OR 16802]. Battery 5 continues to operate at elevated temperatures<br />and exhibits higher load-share than the other batteries.<br />Elevated temperature drives the VTFE/TRSWCC to lower Voltage<br />cut-off levels, as a result, Batteries 1 - 4 are experiencing<br />a gradual capacity decline. OR 16801 adjusted K52 to Level<br />3 on Day 200.<br /><br />Successfully executed real-time commanding to recovery NICMOS<br />from Suspend to Operate @ 204/14:59:24Z [OR 16803] in time to<br />intercept SMS @ 204/15:39Z. Included command to position PAM<br />and FOM.<br /><br />HST Ground system with SOC/RFSOC/PSS and the SN testing<br />scheduled 205/16:10Z - 18:44Z with STGT, STOCC, NCC, NASCOM,<br />FDF, RFSOC/SOC, and PSS using CCS "B" and "G" Strings with CCS<br />Release 4.0.1 and PRD D06100R2. The objective of this testing<br />is to verify the IP and Serial telemetry and command interfaces<br />between CCS "B" and "G" Strings via the SN.