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Daily 3698
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3698 PERIOD COVERED: DOYs 261-263 OBSERVATIONS SCHEDULED ACS/HRC/WFC 10061 CCD Daily Monitor This program consists of basic tests to monitor, the read noise, the development of hot pixels and test for any source of noise in ACS CCD detectors. This programme will be executed once a day for the entire lifetime of ACS. ACS/WFC 10121 The Core Dynamics of the Dense Globular Cluster NGC 6752 NGC 6752 is one of the best-studied dense globular clusters, and a wide variety of intriguing and anomalous results have been obtained. We propose ACS imaging of the core of this cluster. This will increase the accuracy of our previous internal proper motion measurements by almost an order of magnitude, providing an unprecedented probe of the central potential. The data will also greatly increase the radial extent of previous work on the binary frequency and luminosity function of this cluster. Together, the data will provide a new level of constraints on the dynamics of a dense globular cluster. ACS/WFC/NIC3/WFPC2 10134 The Evolution and Assembly of Galactic Disks: Integrated studies of mass, stars and gas in the Extended Groth Strip This project is a 126-orbit imaging survey in F606W/F814W ACS to measure the evolution of galaxy disks from redshift z = 1.4 to the present. By combining HST imaging with existing observations in the Extended Groth Strip, we can for the first time simultaneously determine the mass in dark matter that underlies disks, the mass in stars within those disks, and the rate of formation of new stars from gas in the disks, for samples of 1, 000 objects. ACS observations are critical for this work, both for reliable identifications of disks and for determining their sizes and inclinations. Combining these data with the kinematics measured from high-resolution Keck DEIMOS spectra will give dynamical masses that include dark matter. Stellar masses can be measured separately using ground-based BRIK and Spitzer IRAC GTO data, while cross-calibrated star formation rates will come from DEEP2 spectra, GALEX, and Spitzer/MIPS. The field chosen is the only one where all multiwavelength data needed will be available in the near term. These data will show how the fundamental properties of disks {luminosity, rotation speed, scale length} and their scaling relations have evolved since z~1, and also will measure the build-up of stellar disks directly, providing fundamental tests of disk formation and evolution. In addition to the above study of disk galaxies, the data will also be used to measure the evolution of red-sequence galaxies and their associated stellar populations. ACS images will yield the number of red-sequence galaxies versus time, together with their total associated stellar mass. ACS images are crucial to classify red-sequence galaxies into normal E/S0s versus peculiar types and to measure radii, which will complete the suite of fundamental structural parameters needed to study evolution. We will measure the zeropoints of major scaling laws {Fundamental Plane, radius versus sigma}, as well as evolution in characteristic quantities such as L*, v*, and r*. Stellar population ages will be estimated from high-resolution Keck DEIMOS spectra and compared to SED evolution measured from GALEX, HST, Spitzer, and ground-based colors. Important for both disk and red-galaxy programs are parallel exposures to be taken with both NIC3 {J and H} and WFPC2 {B}. These are arranged so that ACS, WFPC2, and NIC3 all overlap where possible , providing a rich data set of galaxies imaged with all three HST cameras from B to H. These data will be used to measure restframe visible morphologies and UV star-formation rates for galaxies near the edge of the survey, to discover and count EROs below the Keck spectroscopic limit of R = 24, and to provide an improved database of photometric redshifts for galaxies in the overlap regions. ACS/WFC/WFPC2 10227 Globular Cluster Systems of Giant, Post-Starburst Shell Ellipticals Mergers seem to have played a major role in determining the shapes and dynamics of elliptical galaxies. A few galactic mergers still occur and offer valuable clues to past evolutionary processes. Young globular clusters formed during mergers hold strong promise for age-dating such events, besides helping shed light on the cluster-formation process itself. With young globulars in ongoing mergers and ~0.5 Gyr old remnants now well studied {NGC 4038/39, 3256, 7252, and 3921}, we propose to observe 4 bona fide ellipticals featuring ripples, tidal tails as well as post-starburst spectra {E+A galaxies: strong Balmer absorption}, which are obvious candidates for having undergone a dissipated merger 1-4 Gyr ago. If the globulars formed during mergers are formed with a normal IMF, they should still be around in large numbers in intermediate-age systems. If that is indeed the case, it would constitute strong evidence in favor of the scenario in which metal-rich globulars in 'normal' ellipticals are formed in merging events. We plan to use these ACS observations to {1} measure high-accuracy {g-I error of 0.1 mag} colors for clusters as faint as the peak of the luminosity function {LF} of old globulars, {2} use these colors to separate first- and second-generation clusters, and {3} determine the LFs of the two kinds of clusters down to 1.5 mag past the LF peak for old globulars. Deep dithered g&I-band images form a crucial part of our observing strategy. When combined with previous HST studies of globulars in mergers, this study will yield about a dozen globular cluster systems with age estimates, enough to make meaningful statements about the influence of mergers in creating "red'', metal-rich globulars in giant E's and the evolution of the specific frequency of globular clusters during galactic mergers. NIC/NIC3 10226 The NICMOS Grism Parallel Survey We propose to continue managing the NICMOS pure parallel program. Based on our experience, we are well prepared to make optimal use of the parallel opportunities. The improved sensitivity and efficiency of our observations will substantially increase the number of line-emitting galaxies detected. As our previous work has demonstrated, the most frequently detected line is Halpha at 0.7z1.9, which provides an excellent measure of current star formation rate. We will also detect star-forming and active galaxies in other redshift ranges using other emission lines. The grism observations will produce by far the best available Halpha luminosity functions over the crucial--but poorly observed--redshift range where galaxies appear to have assembled most of their stellar mass. This key process of galaxy evolution needs to be studied with IR data; we found that observations at shorter wavelengths appear to have missed a large fraction of the star-formation in galaxies, due to dust reddening. We will also obtain deep F110W and F160W images, to examine the space densities and morphologies of faint red galaxies. In addition to carrying out the public parallels, we will make the fully reduced and calibrated images and spectra available on-line, with some ground-based data for the deepest parallel fields included. NIC1/NIC2/NIC3 8793 NICMOS Post-SAA calibration - CR Persistence Part 4 A new procedure proposed to alleviate the CR-persistence problem of NICMOS. Dark frames will be obtained immediately upon exiting the SAA contour 23, and every time a NICMOS exposure is scheduled within 50 minutes of coming out of the SAA. The darks will be obtained in parallel in all three NICMOS Cameras. The POST-SAA darks will be non-standard reference files available to users with a USEAFTER date/time mark. The keyword 'USEAFTER=date/time' will also be added to the header of each POST-SAA DARK frame. The keyword must be populated with the time, in addition to the date, because HST crosses the SAA ~8 times per day so each POST-SAA DARK will need to have the appropriate time specified, for users to identify the ones they need. Both the raw and processed images will be archived as POST-SAA DARKSs. Generally we expect that all NICMOS science/calibration observations started within 50 minutes of leaving an SAA will need such maps to remove the CR persistence from the science images. Each observation will need its own CRMAP, as different SAA passages leave different imprints on the NICMOS detectors. NIC2 10176 Coronagraphic Survey for Giant Planets Around Nearby Young Stars A systematic imaging search for extra-solar Jovian planets is now possible thanks to recent progress in identifying "young stars near Earth". For most of the proposed young {~ 30 Myrs} and nearby {~ 60 pc} targets, we can detect a few Jupiter-mass planets as close as a few tens of AUs from the primary stars. This represents the first time that potential analogs of our solar system - that is planetary systems with giant planets having semi-major axes comparable to those of the four giant planets of the Solar System - come within the grasp of existing instrumentation. Our proposed targets have not been observed for planets with the Hubble Space Telescope previously. Considering the very successful earlier NICMOS observations of low mass brown dwarfs and planetary disks among members of the TW Hydrae Association, a fair fraction of our targets should also turn out to posses low mass brown dwarfs, giant planets, or dusty planetary disks because our targets are similar to {or even better than} the TW Hydrae stars in terms of youth and proximity to Earth. Should HST time be awarded and planetary mass candidates be found, proper motion follow-up of candidate planets will be done with ground-based AOs. WFPC2 10071 WFPC2 CYCLE 12 Supplemental Darks Part 3/3 This dark calibration program obtains 3 dark frames every day to provide data for monitoring and characterizing the evolution of hot pixels. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) HSTAR 9534: GS Acquisition (1,3,1) @ 261/21:45:29Z resulted in FL backup (3,0,3) due to SSLE on FGS 1. Previous FHST Roll Delay Update was successful with small axis errors. There was no FHST Map scheduled after the GS Acquisition. The following GS acquisition passed with no problem. Under investigation. HSTAR 9535: GS Acquisition (3,1,3) @ 261/23:45:26Z failed to RGA control due to SRLE on FGS 1 and FGS 3. Two FHST FM Updates scheduled prior to the GS acquisition both succeeded and had a very low vehicle error observed. Search Radius for GS acquisition was 55 arcsec. Following GS acquisition was successful. FHST Map @ 261/23:53:14Z showed errors of -12.874, -3.777 and -5.104 arcsec. Under investigation. HSTAR 9536: GS Acquisition (3,1,3) @ 262/04:43:34Z succeeded after failing multiple attempts at FL walkdown for SRLE on FGS 1. Subsequent FHST Map @ 262/04:56:16Z had 3-axis (RSS) value approximately 12.00 arcsec. Reference HSTAR 9535, had GS ID: Primary FGS 0848300909, Secondary 0848300233. Under investigation. HSTAR 9537: GS Acquisition (2,1,2) @ 262/11:13:11Z resulted in FL backup (2,0,2)due to SSLE on FGS 1. GS Reacquisition (2,1,2) @ 262/12:27:49Z will also result in FL backup (2,0,2). Under investigation. COMPLETED OPS REQs: None OPS NOTES EXECUTED: 1259-0 Battery 3 Capacity test ground limits @ 262/21:59z SCHEDULED SUCCESSFUL FAILURE TIMES FGS Gsacq 35 34 See Hstar # 9535 FGS Reacq 19 19 FHST Update 41 41 LOSS of LOCK SIGNIFICANT EVENTS: None |
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