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Daily 3564
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3564 PERIOD COVERED: DOY 64 OBSERVATIONS SCHEDULED ACS/HRC 9747 An Imaging Survey of the Statistical Frequency of Binaries Among Exceptionally-Young Dynamical Families in the Main Asteroid Belt We propose an ambitious SNAPSHOT program to determine the frequency of binaries among two very young asteroid families in the Main Belt, with potentially profound implications. These families {of C- and S-type} have recently been discovered {Nesvorny et al. 2002, Nature 417, 720}, through dynamical modeling, to have been formed at 5.8 MY and 8.3 MY ago in catastrophic impact events. This is the first time such precise and young ages have been assigned to a family. Main-belt binaries are almost certainly produced by collisions, and we would expect a young family to have a significantly higher frequency of binaries than the background, because they may not yet have been destroyed by impact or longer-term gravitational instabilities. In fact, one of the prime observables from such an event should be the propensity for satellites. This is the best way that new numerical models for binary production by collisions {motivated largely by our ground-based discoveries of satellites among larger asteroids}, can be validated and calibrated. HST is the only facility that can be used to search for binaries among such faint objects {V17.5}. We will also measure two control clusters, one being an "old" family, and the other a collection of background asteroids that do not have a family association, and further compare with our determined value for the frequency of large main-belt binaries {2%}. We request visits to 180 targets, using ACS/HRC. 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/NIC3 9890 Probing the Dynamics and Shock Physics of the Cas A Supernova Remnant Cassiopeia A {Cas A; SN 1680} is the youngest known and closest example of an oxygen-rich, core-collapse supernova remnant. A two-year WFPC2 survey of part of the remnant yielded many new insights including realization of the stunning amount of fine-scale detail present in the ejecta, and the first precise location of the reverse shock front in the main shell via rapid emission and structural changes visible over 2 yrs. In addition, these data revealed over 100 new ejecta knots located out ahead of the forward blast wave in a small region where only a handful were known from ground-based images. We propose a follow-up survey program aimed at obtaining hi-res images of the entire remnant in the ejecta's four major emission lines. A separate set of ACS and NIC3 [Si VI] images of the NW reverse shock filaments will be taken 3-4 months following the main Cycle 12 survey images. These will allow us to the trace individual ejecta knot deceleration dynamics, excitation, and evolution during reverse shock passage. Analysis of the emission line fluxes will make use of custom shock models generated by us for Cas A. These data will also provide data on outer knot chemistry and expansion asymmetries particularly in regard to the collimation of the NE and SW jets of O, Si, Ca-rich ejecta. A major aim of this program is to acquire a superb two-year image database covering the entire remnant to allow a detailed shock physics and dynamics study. ACS/WFC 10046 CCD Hot Pixel Annealing Hot pixel annealing will be performed once every 4 weeks. The CCD TECs will be turned off and heaters will be activated to bring the detector temperatures to about +20C. This state will be held for approximately 12 hours, after which the heaters are turned off, the TECs turned on, and the CCDs returned to normal operating condition. To assess the effectiveness of this procedure, a bias and two dark images will be taken after the annealing procedure for both WFC and HRC. The HRC darks are taken in parallel with the WFC darks. ACS/WFC/WFPC2 9822 The COSMOS 2-Degree ACS Survey We will undertake a 2 square degree imaging survey {Cosmic Evolution Survey -- COSMOS} with ACS in the I {F814W} band of the VIMOS equatorial field. This wide field survey is essential to understand the interplay between Large Scale Structure {LSS} evolution and the formation of galaxies, dark matter and AGNs and is the one region of parameter space completely unexplored at present by HST. The equatorial field was selected for its accessibility to all ground-based telescopes and low IR background and because it will eventually contain ~100, 000 galaxy spectra from the VLT-VIMOS instrument. The imaging will detect over 2 million objects with I 27 mag {AB, 10 sigma}, over 35, 000 Lyman Break Galaxies {LBGs} and extremely red galaxies out to z ~ 5. COSMOS is the only HST project specifically designed to probe the formation and evolution of structures ranging from galaxies up to Coma-size clusters in the epoch of peak galaxy, AGN, star and cluster formation {z ~0.5 to 3}. The size of the largest structures necessitate the 2 degree field. Our team is committed to the assembly of several public ancillary datasets including the optical spectra, deep XMM and VLA imaging, ground-based optical/IR imaging, UV imaging from GALEX and IR data from SIRTF. Combining the full-spectrum multiwavelength imaging and spectroscopic coverage with ACS sub-kpc resolution, COSMOS will be Hubble's ultimate legacy for understanding the evolution of both the visible and dark universe. NIC3 9999 The COSMOS 2-Degree ACS Survey NICMOS Parallels The COSMOS 2-Degree ACS Survey NICMOS Parallels. This program is a companion to program 9822. NICMOS 8791 NICMOS Post-SAA calibration - CR Persistence Part 2 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/CCD 10017 CCD Dark Monitor-Part 1 Monitor the darks for the STIS CCD. STIS/CCD 10019 CCD Bias Monitor - Part 1 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. STIS/MA1/MA2 10032 MAMA Full Field Sensitivity Monitor & PSF Check The purpose of this program is to monitor the sensitivity of the MAMA detectors over the full field. This is achieved by observing globular cluster NGC6681 once during Cycle 12. The data can be directly compared with similar data obtained in Cycles 7, 8, 9, 10 and 11. 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. 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: 1115-0 CCC IPCONFIG Connections @ 064/17:31z SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 10 10 FGS REacq 03 03 FHST Update 12 12 LOSS of LOCK SIGNIFICANT EVENTS: CCS Release 5.0.3.1 - PACOR A PSS PF-13 Interface Test scheduled 065/12:00Z - 20:00Z with GDOC, HITT, PACOR A, OPUS, and SOC using CCS "C" with CCS Release 4.0.3.1 and "D" Strings with CCS Release 5.0.3.1 and PRD O06300ST. The purpose of this testing is to verify PACOR A can ingest various science data products from PF-13 and the PSS. |
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