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Daily 3432
HUBBLE SPACE TELESCOPE DAILY REPORT******* # 3432 PERIOD COVERED: DOY 233 OBSERVATIONS SCHEDULED ACS 9675 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 9764 Elliptical galaxies in z~1.5 clusters Giant elliptical galaxies offer can some of the tightest constraints on models of galaxy formation. Recent observations have shown significant inconsistencies between their properties and the predictions of the currently popular hierarchical clustering models. Many outstanding questions about the nature and evolution of these objects can best {or only} be addressed by extending studies of cluster ellipticals out to z1. Recently we have identified large overdensities of red galaxies, strongly clustered around powerful radio sources at z~1.5. We propose to image our two richest fields, of Abell Class 0-1 richness, using the F814W and F606W filters on the ACS/WFC. Our goals are to investigate: {1} Galaxy morphologies: we will determine the bulge fractions of the red cluster galaxies, to confirm that they are early-types, and measure their characteristic radii to investigate their evolutionary status. {2} Colour gradients: we will search for colour gradients indicative of recent star formation {particularly blue cores}, or inhomogeneities in the internal colours which might be indicative of recent assembly. {3} Cluster membership: with two additional colours we will obtain accurate photometric redshift estimates for all galaxies. Combined with studies of nearby clusters and of field ellipticals, our results will place very tight constraints on the formation of the most massive galaxies. ACS/WFC 9892 H-alpha Snapshots of Nearby Galaxies observed in F300W: Quantifying Star Formation in a Dusty Universe Previous studies of nearby galaxies show large discrepancies between different star formation {SF} indicators on large {100 pc, or even global} scales: the strikingly complex interplay of young stars, dust and ionized gas are the primary cause of this variance. The few galaxies in the HST Archive with both WFPC2 H-alpha and mid-UV {F255W or F300W} imaging show this complex geometry extending down to 10 pc scales. We propose a SNAPshot survey in the ACS/WFC H-alpha filter of 48 galaxies of all Hubble types, that are nearby but beyond the Local Group, and that were previously imaged with WFPC2 in the mid-UV and in F814W. We aim to provide a benchmark for understanding the SF processes in both normal and star-bursting galaxies, at spatial resolutions unattainable from the ground for a large and varied galaxy sample. These data can be applied to a wide range of astrophysical problems and will, therefore, be made public immediately. Our science goals are to: {1} spatially resolve the dust clouds and filaments which strongly affect mid-UV and H-alpha derived SF rates, {2} test how the large-scale correlation between H-alpha and mid-UV flux breaks down on pc scales, and {3} model the propagation of star formation by comparing the SF over time scales of ~100 Myr {via mid-UV} and ~5 Myr {via H-alpha}. This will {4} significantly improve our insight into, and calibration of SF in UV-bright galaxies at high z, and into the cosmic SF history. NIC1/NIC2/STIS/CCD/WFPC2 9738 Spectroscopy and Polarimetry of Mars at Closest Approach We plan a coordinated program of spectroscopy, imaging, and spectropolarimetry of Mars during the August 2003 opposition to study the composition and physical state of surface materials and airborne aerosols. The observations include {a} Moderate spectral resolution 290 to 570 nm STIS long-slit push-broom imaging spectroscopy of Mars, to constrain the properties of airborne aerosol particles and to search for and globally map iron-bearing minerals that are diagnostic of specific past climatic conditions; {b} WFPC2 UV-VIS images designed primarily to quantify the effects of ice and dust aerosols on our STIS spectra; {c} NICMOS near-IR images to search for and globally map the presence of hydrated surface minerals; and {d} ACS multispectral polarizer images to provide critical phase function measurements needed to constrain the physical properties of the Martian surface layer. The observations are timed to take advantage of the closest approach of Mars to Earth for the next several hundred years. Images and spectra will be acquired at a spatial scale comparable to existing spacecraft orbital spectroscopy data {~10 km/pixel} and in wavelength regions not sampled by past or current Mars spacecraft instrumentation. These observations also provide complementary scientific and calibration measurements in support of current and future NASA and ESA Mars exploration missions. NIC3/NIC2/NIC3 10064 Mini-SMOV NICMOS dark current, shading profile, and read noise program The purpose of this proposal is to study the dark current, read noise, and shading profile for all three NICMOS detectors after the NICMOS starts operating due to safing. This proposal is a version of the NICMOS monitoring program. 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 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 9786 The Next Generation Spectral Library We propose to continue the Cycle 10 snapshot program to produce a Next Generation Spectral Library of 600 stars for use in modeling the integrated light of galaxies and clusters. This program is using the low dispersion UV and optical gratings of STIS. The library will be roughly equally divided among four metallicities, very low {[Fe/H] lt -1.5}, low {[Fe/H] -1.5 to -0.5}, near-solar {[Fe/H] -0.3 to 0.1}, and super-solar {[Fe/H] gt 0.2}, well-sampling the entire HR-diagram in each bin. Such a library will surpass all extant compilations and have lasting archival value, well into the Next Generation Space Telescope era. Because of the universal utility and community-broad nature of this venture, we waive the entire proprietary period. STIS/CCD 10000 STIS Pure Parallel Imaging Program: Cycle 12 This is the default archival pure parallel program for STIS during cycle 12. 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. 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. WFPC2 9710 POMS Test Proposal: WFII backup parallel archive proposal This is a POMS test proposal designed to simulate scientific plans. WFPC2 9816 Proper motion kinematics in Galactic bulge/bar fields With this proposal we continue a successful programme to measure proper motions in fields in the galactic bulge. We are able to reach accuracies of ca 10km/s in transverse motion at a distance of 8kpc, for thousands of stars per WFPC2 field. In combination with VLT spectroscopic radial velocities and metallicity indices, we will be able to construct a full dynamical and stellar-population model for our Bulge. Previous fields in this programme were on the minor axis; the fields proposed here {using first epoch observations from 1995-1998 from the archive} lie in the first quadrant, on the near side of the Galactic bar. We also wish to establish first-epoch observations in the 4th quadrant, where no suitable data exist so far. 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*********** 10********************** 10 FGS REacq*********** 07*********************** 07 FHST Update********* 18********************** 18 LOSS of LOCK SIGNIFICANT EVENTS: Successfully completed Command Timing Comparison testing on SUN/SGI platform using the CCS "D" and "C" Strings 232/11:00Z - 19:30Z.* Results indicate the SUN (D String) performance is significantly faster.* While command FIVEBLCKs in a "NoVerify" mode a 15% - 30% increase was seen and in "Countcheck" mode a 10% - 20% increase was see in some FIVEBLCKs.* A 10% - 15% increase was seen in only one command load in TDRSS 32 kbps NoVerify.* Another test is scheduled for Day 240 with Sys Admin to monitor the "D" String while commanding.*** |
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