HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3152<br /><br />PERIOD COVERED: DOY 189<br /><br />OBSERVATIONS SCHEDULED (see HSTARS below for possible observation problems)<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. <br />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 <br />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/CCD 8906<br /><br />Hot Pixel Annealing.<br /><br />pixel annealing process by measuring the dark current behavior before and after<br />annealing and by searching for any window contamination effects. In addition,<br />CTE performance is examined by looking for traps in a low signal level flat.<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/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 8934<br /><br />WFPC2 Decontaminations and Associated Observations Pt. 3/3<br /><br />photometric stability check, focus monitor, pre- and post-decon internals <br />{bias,<br />intflats, kspots, & darks}, UV throughput check, VISFLAT sweep, and internal UV<br />flat check.<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 8939<br /><br />Cycle 10 Internal Monitor.<br /><br />The WF/PC-2 was used to calibrate the internal monitor, to be run weekly to<br />monitor the health of the cameras.<br /><br />WF/PC-2 9087<br /><br />Black Hole X-ray Transients and X-ray Binaries in M31.<br /><br />The WF/PC-2 was used to search for M31 for x-ray transients which had <br />previously<br />been seen as part of the Chandra Guaranteed Time Observations {GTO} <br />program. The<br />x-ray properties of these transient sources {spectra, variability} allow us to<br />determine whether the accreting object is a black hole or a neutron star. It is<br />proposed to determine the nature of the mass-losing star. Massive stars will<br />show little {<2 mag} change in their UV luminosities during outbursts, while<br />low-mass stars will show large {>5 mag} changes in their UV luminosities. By<br />determining the nature of the primary {accreting} and secondary stars in these<br />x-ray transients, we will have the first data set that will allow the evolution<br />of black hole and neutron star binaries to be studied in an external galaxy.<br /><br />GO 9172<br /><br />Molecular Hydrogen in the Damped LyAlpha Absorber of Q1331+170<br /><br />We wish to search for the Lyman and Werner absorption lines of molecular<br />hydrogen {rest LambdaLambda = 1104 to 911 Angstrom} associated with the<br />well-studied damped LyAlpha and 21-cm absorber at z=1.776 in Q1331+170. The <br />rare<br />detection of C I absorption in this system make this a promising candidate <br />for a<br />search. After detecting H_2, we plan to measure the relative population in the<br />individual rotation states. The J = 0, 1, 2, 3 states will yield the kinetic<br />temperature of the gas, while the weak J = 4 and higher states will measure {or<br />limit} the local UV radiation field and hydrogen density. The detection of <br />C I^*<br />has been used to measure the cosmic microwave background temperature at <br />z=1.776,<br />and test the validity of the Big Bang model. The observed population of the <br />fine<br />structure levels of C I can be explained entirely by the expected CMB <br />radiation,<br />with surprisingly strong limits on local sources of excitation. The H_2 <br />spectrum<br />will enable us to check this result, by allowing us to make an independent<br />estimate of the rate of UV and collisional pumping of the C I^* levels.<br /><br />GTO/ACS 9291<br /><br />Formation of High Redshift Radio Galaxies<br /><br />This programme uses ACS observations of high redshift radio galaxies {HzRGs} to<br />investigate massive galaxy and cluster formation in the early Universe. By<br />carrying out deep observations of a few z > 3.8 targets the following four<br />questions will be studied: {1} Are HzRGs massive central-cluster galaxies <br />formed<br />through hierarchical assembly of Lyman break galaxies? Detailed brightness<br />distributions colors and morphologies of HzRG clumps will be measured and<br />compared with those of Lyman break galaxies. {2} Are HzRGs located in dense<br />{proto-} clusters and if so what are the properties of the associated<br />large-scale structures? Lyman alpha excesses, colors and morphologies of <br />objects<br />in field will be used to search for companion galaxies of HzRGs. {3} What are<br />the origin and fate of giant gas halos associated with HzRGs and what role do<br />they play in the formation of massive galaxies? The morphologies and locations<br />of Ly-alpha clumps will be compared with those of continuum clumps. {4} Is<br />nuclear activity a source of star formation in the early Universe? The<br />properties of continuum and Ly-alpha clumps along will be compared in relation<br />to the radio jet.<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 <br />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 <br />Group.<br /><br />NICMOS 9321<br /><br />Dark current, shading profile, and read noise monitoring program<br /><br />The purpose of this proposal is to monitor the detector dark current, read<br />noise, and shading profile for all three NICMOS cameras from the onset of <br />normal<br />NCS operations throughout the start of Cycle 11.<br /><br />ACS/WFC 9373<br /><br />Reaching the Horizontal Branch in NGC 5128: Deepest Probe of a Giant <br />Elliptical<br /><br />NGC 5128 is the nearest easily observable giant E galaxy, and is a unique<br />testing ground for stellar population models. Previous WFPC2 photometry of its<br />halo red-giant stars has shown that they are predominantly metal-rich<br />{<m/H>~-0.45}, but little is yet known about their spread in ages. With the<br />ACS/WFC camera, we propose to obtain deep {V, I} photometry down to the <br />level of<br />its horizontal-branch population, with the goal of refining the metallicity<br />distribution function and gaining quantitative information on its age<br />distribution. This will be unique data for any giant elliptical galaxy and will<br />provide major new input to population synthesis techniques for such 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 <br />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 <br />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/CAL 9558<br /><br />ACS weekly Test<br /><br />This program consists of basic tests to monitor, the read noise, the <br />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 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 />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 />HSTARS: None<br /><br />COMPLETED OPS REQs: None<br /><br />OPS NOTES EXECUTED:<br />0911-0 Limit Management During WFPC2 Decontamination (M001)<br />0911-0 Limit Management During WFPC2 Decontamination (M001)<br />1004-2 Update Pressure-Based Battery Capacity Equations<br /> Guide Star Acquisitions:<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 7 7<br />FGS REacq 8 8<br />FHST Update 13 13<br />LOSS of LOCK None<br /><br />Operations Notes: None<br /><br />SIGNIFICANT EVENTS: None