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Daily 3578
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3578 PERIOD COVERED: DOY 85 OBSERVATIONS SCHEDULED ACS 9475 ACS coronagraphic survey for debris disks around nearby stars We propose a comprehensive imaging survey of nearby stars that will realize the full potential of the ACS coronagraph to map debris disks, the extrasolar analogs of our Kuiper Belt. Most debris disks are detected only by excess thermal emission at far-infrared wavelengths. Because they have a factor of 100 less dust cross section than the young debris disks around HR 4796A and beta Pic, they are undetectable by present techniques. In simulations of disk detectability, Kalas and Jewitt {1996} determined that detecting the scattered light from the disk requires at least two orders of magnitude of suppression of the central PSF than is attainable from the ground. The ACS coronagraph finally provides this increase in sensitivity, surpassing the WFPC2 sensitivity to faint nebulosity near bright stars by at least three orders of magnitude. Mapping the debris around stars is particularly important for the indirect detection of planet-mass objects. Dynamical models have shown that unseen perturbers dynamically modify the radial, azimuthal and vertical structure of debris disks. These data will provide the critical high-resolution mapping of debris disks. ACS/HRC/WFC 10059 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/HRC/WFC 9796 Observations of Intermediate Mass Black Hole Candidate Ultra-Luminous X-ray Sources Ultra-luminous X-ray {ULX} sources are off-nuclear point sources in nearby normal galaxies. Variability observed on the timescale of days, weeks, and years signals that ULXS are accreting sources, likely harboring black holes. However, the observed X-ray luminosity of these systems far exceeds the Eddington limit for a 10 Msun black hole; some ULXs may be intermediate mass black holes. The identification and study of optical counterparts with HST will be central to better understanding these objects. We propose to obtain deep U-B-V-I exposures of 4 extremely bright ULXs in nearby spirals: NGC 1313 X-1 and X-2, M81 X-9 {Holmberg II X-1}, and M74 X-1. Each has a 0.5'' Chandra position, and X-ray luminosity and spectral characteristics consistent with expectations for intermediate mass black holes. We will use the colors we obtain, the magnitudes we measure, and any source variability {also, correlated optical-X-ray variability from simultaneous Chandra snapshots} to constrain the nature of the donor stars and the black holes {10 Msun or 100-1000 Msun}, and the formation and evolution scenarios for each system. ACS/WFPC2 9488 Cosmic Shear - with ACS Pure Parallel Observations The ACS, with greater sensitivity and sky coverage, will extend our ability to measure the weak gravitational lensing of galaxy images caused by the large scale distribution of dark matter. We propose to use the ACS in pure parallel {non- proprietary} mode, following the guidelines of the ACS Default Pure Parallel Program. Using the HST Medium Deep Survey WFPC2 database we have measured cosmic shear at arc-min angular scales. The MDS image parameters, in particular the galaxy orientations and axis ratios, are such that any residual corrections due to errors in the PSF or jitter are much smaller than the measured signal. This situation is in stark contrast with ground-based observations. We have also developed a statistical analysis procedure to derive unbiased estimates of cosmic shear from a large number of fields, each of which has a very small number of galaxies. We have therefore set the stage for measurements with the ACS at fainter apparent magnitudes and smaller, 10 arc-second scales corresponding to larger cosmological distances. We will adapt existing MDS WFPC2 maximum likelihood galaxy image analysis algorithms to work with the ACS. The analysis would also yield an online database similar to that in archive.stsci.edu/mds/ NIC/NIC3 9865 The NICMOS Parallel Observing Program 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 8792 NICMOS Post-SAA calibration - CR Persistence Part 3 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. STIS 9633 STIS parallel archive proposal - Nearby Galaxies - Imaging and Spectroscopy Using parallel opportunities with STIS which were not allocated by the TAC, we propose to obtain deep STIS imagery with both the Clear {50CCD} and Long-Pass {F28X50LP} filters in order to make color-magnitude diagrams and luminosity functions for nearby galaxies. For local group galaxies, we also include G750L slitless spectroscopy to search for e.g., Carbon stars, late M giants and S-type stars. This survey will be useful to study the star formation histories, chemical evolution, and distances to these galaxies. These data will be placed immediately into the Hubble Data Archive. STIS/CCD 10018 CCD Dark Monitor-Part 2 Monitor the darks for the STIS CCD. STIS/CCD 10020 CCD Bias Monitor - Part 2 Monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4, to build up high-S/N superbiases and track the evolution of hot columns. STIS/CCD 10085 STIS Pure Parallel Imaging Program: Cycle 12 This is the default archival pure parallel program for STIS during cycle 12. WFPC2 10070 WFPC2 CYCLE 12 Supplemental Darks Part 2/3 This dark calibration program obtains 3 dark frames every day to provide data for monitoring and characterizing the evolution of hot pixels. WFPC2 10084 WFII parallel archive proposal This is the generic target version of the WFPC2 Archival Pure Parallel program. The program will be used to take parallel images of random areas of the sky, following the recommendations of the 2002 Parallels Working Group. WFPC2 10090 WFII backup parallel archive proposal This is a POMS test proposal designed to simulate scientific plans. WFPC2/ACS 9601 WFPC2-ACS Photometric Cross-Calibration This proposal is aimed at providing photometric zeropoint cross-calibration between the commonly used WFPC2 photometric filter sets and those that will be used for ACS programs. The proposal includes observations of globular clusters spanning a wide range in metallicity, including NGC 2419 and 47 Tuc. In addition, we will obtain WFPC2 observations of the primary ACS standard star. This program will produce a valuable tie-in between the WFPC2, ACS and Sloan filter photometric systems. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) None COMPLETED OPS REQs: None OPS NOTES EXECUTED: None SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 9 9 FGS REacq 6 6 FHST Update 20 20 LOSS of LOCK SIGNIFICANT EVENTS: Battery Reconditioning Macro Ops Acceptance Test scheduled 086/11:00Z - 087/05:00Z with GDOC, HITT, SE, and VEST using CCS "D" String (prime) with CCS Release 5.0.3.1 and PRD O06300ST and CCS "C" String (secondary) with CCS Release 4.0.3.1 and PRD O06300T. The purpose of this testing is to verify installation and backout procedures for the Battery Reconditioning macro work in an operational scenario. Command Timing test scheduled 086/12:00Z - 22:00Z with GDOC, SOC, HITT, and CCS using CCS "H" String with CCS Release 5.0.3.1 and PRD O06300ST. The purpose of this testing is to check the command timing for CCS Release 5.0.3.1 with historical, baselined numbers for standard configuration with S-Channel data and other loads. |
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