HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3238<br /><br />PERIOD COVERED: DOY 310<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 />GTO/ACS 9290<br /><br />The Nature of Galaxies at z > 4.<br /><br />The Morphological, Photometric, and Spectroscopic Properties of Intermediate<br />Redshift Cluster. New and fundamental constraints on the evolutionary state of<br />high redshift clusters will be made by obtaining deep, multiband images {SDSS g,<br />r, i, z} over the central 1.5 Mpc regions of seven distant clusters in the range<br />0.76 < z < 1.27. In addition, slitless spectroscopy, using the WFC GRISM, will<br />be performed over the central 750 kpc region of each system galaxy.<br /><br />ACS/WFPC2 9481<br /><br />Pure Parallel Near-UV Observations with WFPC2 within High-Latitude ACS Survey<br />Fields<br /><br />In anticipation of the allocation of ACS high-latitude imaging survey{s}, we<br />request a modification of the default pure parallel program for those WFPC2<br />parallels that fall within the ACS survey field. Rather than duplicate the red<br />bands which will be done much better with ACS, we propose to observe in the<br />near-ultraviolet F300W filter. These data will enable study of the rest-frame<br />ultraviolet morphology of galaxies at 0<z<1. We will determine the morphological<br />k-correction, and the location of star formation within galaxies, using a sample<br />that is likely to be nearly complete with multi-wavelength photometry and<br />spectroscopic redshifts. The results can be used to interpret observations of<br />higher redshift galaxies by ACS.<br /><br />ACS 9500<br /><br />The Evolution of Galaxy Structure from 10, 000 Galaxies with 0.1HST Proposal<br />9500<br /><br />We propose to determine the evolution of galaxy structure over the last half of<br />cosmic history from galaxy images in the redshift range 0.1<z<1.2. Our sample of<br />10^4 galaxies is contained within a 30'* 30' field centered on the Chandra Deep<br />Field South and is complete to m_r~ 24. The redshift of each galaxy is known to<br />Delta z ~ 0.02 from low-resolution spectra using 17 medium band filters, which<br />also provide SED's complete from 3500Angstrom to 9250Angstrom for the whole<br />sample. A mosaic of 9* 9 ACS pointings in F555W and F850LP will provide < 0.1"<br />{<500 pc} rest-frame 4500Angstrom images for the entire sample of distant<br />galaxies with known redshifts, a 30-fold improvement by number over published<br />surveys. This unique data set will let us to resolve some of the most important<br />issues in galaxy evolution. We will see why star formation activity has declined<br />dramatically since z ~ 1: it could be changes in the interaction and merger<br />rate, waning fuel supply, or simply a shift of star-formation to progressively<br />less massive systems. By resolving the galaxies in rest-frame B, we can separate<br />the bulges, bars, and disks to determine if the bulges simply dim, while disks<br />grow radially with time. The growing disk surface mass density might increase<br />the incidence of large-scale bars. Using the >100 AGNs identified in the field,<br />we will investigate whether the population of host galaxies evolved in the last<br />10^10 years.<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 9598<br /><br />Earth Flats<br /><br />This proposal monitors flatfield stability. This proposal obtains sequences of<br />Earth streak flats to construct high quality flat fields for the WFPC2 filter<br />set. These flat fields will allow mapping of the OTA illumination pattern and<br />will be used in conjuction with previous internal and external flats to generate<br />new pipeline superflats. These Earth flats will complement the Earth flat data<br />obtained during cycles 4-10.<br /><br />WFPC2 9599<br /><br />WFPC2 Cycle 11 UV Earth Flats<br /><br />Monitor flat field stability. This proposal obtains sequences of earth streak<br />flats to improve the quality of pipeline flat fields for the WFPC2 UV filter<br />set. These Earth flats will complement the UV earth flat data obtained during<br />cycles 8-10.<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 />ACS 9647<br /><br />CCD Daily Monitor Part I<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 />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 />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 />NICMOS 9702<br /><br />NICMOS Parallel Thermal Background<br /><br />NICMOS Camera 2 pure parallel exposures in the F222M and F237M filters to<br />establish the stability of the HST+NCS+Instrument thermal emission. This data<br />will be compared against the already available Camera 3 measurements in F222M<br />which show an increased thermal background.<br /><br />FLIGHT OPERATIONS SUMMARY:<br /><br />Significant Spacecraft Anomalies: [The following are preliminary reports of<br />potential non-nominal performance that will be investigated.] None<br /><br />COMPLETED OPS REQs: None<br /><br />OPS NOTES EXECUTED: None<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 5 5<br />FGS REacq 11 11<br />FHST Update 9 9<br />LOSS of LOCK<br /><br />SIGNIFICANT EVENTS: None