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Daily 3382
HUBBLE SPACE TELESCOPE DAILY REPORT******* # 3382 PERIOD COVERED: DOY 162 OBSERVATIONS SCHEDULED 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. ACS 9401 The ACS Virgo Cluster Survey We propose the most comprehensive imaging survey to date of low-redshift, early-type galaxies. Our goal is to exploit the exceptional imaging capabilities of the ACS by acquiring deep images --- in the SDSS g^ and z^ bandpasses --- for 163 E, S0, dE, dE, N and dS0 galaxies in Virgo, the nearest rich cluster. This extraordinary dataset would likely constitute one of the principal legacies of HST, and would have widespread applications for many diverse areas of astrophysics. Our immediate scientific objectives are threefold: {1} measure metallicities, ages and radii for the many thousands of globular clusters {GCs} in these galaxies, and use this information to derive the protogalactic mass spectrum of each galaxy; {2} measure the central luminosity and color profile of each galaxy, and use this information to carry out a completely independent test of the merging hierarchy inferred from the GCs, with the aid of N-body codes that simulate the merger of galaxies containing massive black holes; and {3} calibrate the z^ -band SBF method, measure Virgo's 3-D structure, and carry out the definitive study of the GC luminosity function's precision as a standard candle. Our proposed Virgo Cluster Survey will yield a database of unprecedented depth, precision and uniformity, and will enable us to study the record of galaxy and cluster formation in a level of detail which will never be possible with more distant systems. NICMOS 9423 NICMOS Observations of Transient Infrared Jets in the Galactic Microquasar GRS1915+105 We propose to use HST/NICMOS to make Target of Opportunity observations of the galactic microquasar GRS1915+105. This source possesses transient radio jets which exhibit apparent superluminal motions, and resolved infrared emission from these jets has been observed in GRS1915+105 {Sams, Eckart, and Sunyaev, 1996; Eikenberry and Fazio, 1996}. Because the jet ejection events are correlated with X-ray outbursts, we will use observations of X-ray flares with the Rossi X-Ray Timing Explorer to trigger the HST observations. We will then monitor GRS1915+105 periodically with NICMOS, obtaining relative astrometry, photometry, polarimetry, and grism spectroscopy of the jets and the parent object. These observations will allow us to greatly increase our understanding of the jets' radiative mechanisms and physical conditions, and their evolution with time. We require the capabilities of HST and NICMOS due to the small angular separations between the jets and the parent object {increasing from ~ 0.1 to ~ 0.8 arcsec over the span of the TOO observations} and the high reddening towards GRS1915+105 {A_V ~ 30 mag}. WFPC2 9458 Probing the Formation & Evolution of M31's Outer Disk and Halo The fossil record of galaxy formation and evolution is imprinted on the spatial distribution, ages and metallicities of galactic stellar populations. The observations proposed here build significantly upon our extensive ground-based and archival WFPC2 programs and aim to constrain the formation and evolution of our nearest large neighbour, M31. We propose deep imaging of 8 fields in the outer disk and halo, several of which have been identified from our panoramic ground-based CCD survey {covering ~ 26 square degrees} to possess significant stellar density and/or potential metallicity variations. Deep colour-magnitude diagrams reaching ~2-3 magnitudes below the horizontal branch will be constructed, allowing detailed characterization of the luminous evolved stellar populations via the red giant metallicity distribution, the luminous asymptotic giant branch, the horizontal branch morphology and the red clump, as well as the detection of a main-sequence that may be present from any younger component. Our primary goals are to: {i} quantify the stellar population variations associated with M31 halo substructure, including the newly- discovered giant stellar stream, and {ii} derive stringent constraints on the age and metallicity of stars in the far outer disk. These observations will directly address two key predictions of cold dark matter hierarchical galaxy formation models. ACS 9480 Cosmic Shear With ACS Pure Parallels Small distortions in the shapes of background galaxies by foreground mass provide a powerful method of directly measuring the amount and distribution of dark matter. Several groups have recently detected this weak lensing by large-scale structure, also called cosmic shear. The high resolution and sensitivity of HST/ACS provide a unique opportunity to measure cosmic shear accurately on small scales. Using 260 parallel orbits in Sloan textiti {F775W} we will measure for the first time: beginlistosetlength sep0cm setlengthemsep0cm setlength opsep0cm em the cosmic shear variance on scales 0.7 arcmin, em the skewness of the shear distribution, and em the magnification effect. endlist Our measurements will determine the amplitude of the mass power spectrum sigma_8Omega_m^0.5, with signal-to-noise {s/n} ~ 20, and the mass density Omega_m with s/n=4. They will be done at small angular scales where non-linear effects dominate the power spectrum, providing a test of the gravitational instability paradigm for structure formation. Measurements on these scales are not possible from the ground, because of the systematic effects induced by PSF smearing from seeing. Having many independent lines of sight reduces the uncertainty due to cosmic variance, making parallel observations ideal. ACS/WFPC2 9481 Pure Parallel Near-UV Observations with WFPC2 within High-Latitude ACS Survey Fields In anticipation of the allocation of ACS high-latitude imaging survey{s}, we request a modification of the default pure parallel program for those WFPC2 parallels that fall within the ACS survey field. Rather than duplicate the red bands which will be done much better with ACS, we propose to observe in the near-ultraviolet F300W filter. These data will enable study of the rest-frame ultraviolet morphology of galaxies at 0z1. We will determine the morphological k-correction, and the location of star formation within galaxies, using a sample that is likely to be nearly complete with multi-wavelength photometry and spectroscopic redshifts. The results can be used to interpret observations of higher redshift galaxies by ACS. NICMOS 9484 The NICMOS Parallel Observing Program We propose to manage the default set of pure parallels with NICMOS. Our experience with both our GO NICMOS parallel program and the public parallel NICMOS programs in cycle 7 prepared us to make optimal use of the parallel opportunities. The NICMOS G141 grism remains the most powerful survey tool for HAlpha emission-line galaxies at cosmologically interesting redshifts. It is particularly well suited to addressing two key uncertainties regarding the global history of star formation: the peak rate of star formation in the relatively unexplored but critical 1= z = 2 epoch, and the amount of star formation missing from UV continuum-based estimates due to high extinction. Our proposed deep G141 exposures will increase the sample of known HAlpha emission- line objects at z ~ 1.3 by roughly an order of magnitude. We will also obtain a mix of F110W and F160W images along random sight-lines to examine the space density and morphologies of the reddest galaxies. The nature of the extremely red galaxies remains unclear and our program of imaging and grism spectroscopy provides unique information regarding both the incidence of obscured star bursts and the build up of stellar mass at intermediate redshifts. In addition to carrying out the parallel program we will populate a public database with calibrated spectra and images, and provide limited ground- based optical and near-IR data for the deepest parallel fields. STIS 9506 A SNAPSHOT SURVEY OF HIGH COLUMN DENSITY, LOW-Z LyAlpha ABSORBERS We propose a STIS G140L spectroscopic Snapshot program of bright {V=16.5} AGN not previously observed in the UV to discover new high-column density {N_H = 10^15 cm^-2} LyAlpha absorbers in the local Universe {z = 0.45}. Many more of these high column density systems are needed because: {1} They contribute most of the baryons to the local IGM; {2} They include systems for which valuable metallicity and D/H measurements can be made with the Cosmic Origins Spectrograph {COS}; {3} They include many of the ``warm-hot'' absorbers, thought to be a large baryon reservoir in the local Universe; and {4} They are most likely to be ``associated'' with galaxy halos. Because of their low-z, many of these absorbers can be located relative to galaxies of known redshifts, allowing an immediate scientific return from these snapshots. Perhaps the most important, lasting results of this survey require higher resolution reobservations with COS by our GTO team. Using these snapshots to select the best targets, we will obtain COS R~22, 000 spectra to determine the D/H and metallicity of absorbers in galaxy halos, groups, and voids. We will use pairs and ``constellations'' of AGN to determine absorber sizes, shapes, and covering factors. Candidate ``warm-hot'' absorbers will be reobserved with COS to determine their numbers accurately and to assess their metallicity, sizes, and relationships to galaxies and galaxy groups. WFPC2 9595 WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt3/3 This dark calibration program obtains 3 dark frames every day to provide data for monitoring and characterizing the evolution of hot pixels. STIS 9606 CCD Dark Monitor-Part 2 Monitor the darks for the STIS CCD. STIS 9608 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 9615 Cycle 11 MAMA Dark Monitor This test performs the routine monitoring of the MAMA detector dark noise. This proposal will provide the primary means of checking on health of the MAMA detectors systems through frequent monitoring of the background count rate. The purpose is to look for evidence of change in dark indicative of detector problem developing. 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. NICMOS 9637 NICMOS Focus Stability The purpose of this activity is to determine if the best focus determined in SMOV is stable. This program will execute in approximately one month intervals starting about 1 month after the last execution of proposal 8980. ACS 9658 ACS Earth Flats This program will obtain sequences of flat field images by observing the bright Earth. Several UV filters from the interim calibration program {9564} require additional exposures to obtain the required illumination. A few UV filters from this program will be repeated to monitor for changes in the flat fields and to verify the interim results. Since no streaks are observed in the UV, the wavelength coverage is extended to longer wavelengths in order to explore the severity of streaks in the flats from clouds in the FOV. We have added exposures for the HRC in the visible filters to verify the results derived from the L-flat campaign and to explore the severity of streaks. We have also added exposures on WFC using the minimum exposure time and using filters which will not saturate the brightest WFC pixel by more than 10 times the full well. ACS 9674 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. STIS 9708 STIS Pure Parallel Imaging Program: Cycle 11 This is the default archival pure parallel program for STIS during cycle 11. WFPC2 9709 POMS Test Proposal: 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. ACS/HRC/WFC 9728 Tracing the History of Cosmic Expansion to z~2 with Type Ia Supernovae Type Ia supernovae {SNe Ia} provide the only direct evidence for an accelerating universe, an extraordinary result that needs the most rigorous test. The case for cosmic acceleration rests on the observation that SNe Ia at z = 0.5 are about 0.25 mag fainter than they would be in a universe without acceleration. A powerful and straightforward way to assess the reliability of the SN Ia measurement and the conceptual framework of its interpretation is to look for cosmic deceleration at z 1. This would be a clear signature of a mixed dark-matter and dark-energy universe. Systematic errors in the SNe Ia result attributed to grey dust or cosmic evolution of the SN Ia peak luminosity would not show this change of sign. We have obtained a toehold on this putative ``epoch of deceleration'' with SN 1997ff at z = 1.7, and 3 more at z 1 from our Cycle 11 program, all found and followed by HST. However, this is too important a test to rest on just a few objects, anyone of which could be subject to a lensed line-of-sight or misidentification. Here we propose to extend our measurement with observations of twelve SNe Ia in the range 1.0 z 1.5 or 6 such SNe Ia and 1 ultradistant SN Ia at z = 2, that will be discovered as a byproduct from proposed Treasury and DD programs. These objects will provide a much firmer foundation for a conclusion that touches on important questions of fundamental physics. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) None COMPLETED OPS REQs: 16991-0 - FSW 2.3C EEPROM Installation @ 162/1243z OPS NOTES EXECUTED: None ************************** SCHEDULED**** SUCCESSFUL*** FAILURE TIMES FGS GSacq**************** 10*********************** 10 FGS REacq**************** 7************************** 7 FHST Update************** 20************************ 20 LOSS of LOCK SIGNIFICANT EVENTS: On 162/11:49:27:00 commanding commenced for the installation of FSW2.3C EEPROM installation (OR 16991-0) on the first opportunity.* EEPROM load was completed at 162/11:55:13 and the memory dump and comparison completed at 162/12:35:30 with FSW's concurrence.* BMIC enable (last step) was performed at 162/12:43:05.* All operations associated with the EEPROM installation proceeded nominally.* This concludes a successful FSW2.3C Installation. |
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