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Daily 3613
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3613 PERIOD COVERED: DOYs 135-137 OBSERVATIONS SCHEDULED 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. STIS/CCD 9839 Recombination Lines and Temperature Structure in Planetary Nebulae A high-spatial resolution study of recombination lines {RLs} in bright compact planetary nebulae {PNs} is proposed. Many PNs show a large discrepancy between abundances derived from O II RLs and those derived from [O III]. Others show little or no discrepancy. The PNs with small discrepancies are more compact and high surface brightness. This program seeks to understand why PNs show such differences by studying the RLs at high spatial resolution in the compact PNs NGC 6572 and NGC 6790, which show no discrepancy between O II and [O III], to compare with ground-based studies of the larger PNs NGC 6153 and NGC 6720. The goal is to determine if the distribution of RL emission in NGC 6572 and NGC 6790 is more consistent with radiative recombination than in NGC 6720, where the RL emission is more centrally peaked than [O III]. This will allow us to demonstrate whether or not it is the RLs that are preferentially enhanced in the nebulae with large discrepancies. The Cat's Eye nebula NGC 6543 will also be observed, to determine if the enhanced RL emission is connected to the presence of X-ray emitting gas, as might be expected if the enhanced RLs are a result of high temperature dielectronic recombination. 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. ACS/HRC 9746 Binary systems in the Kuiper Belt The properties of the orbits of Kuiper belt object {KBO} satellites hold keys to fundamental insight into masses and densities of KBOs, the interaction history of the early solar system, the internal structure of distant ice-rock bodies, and even the genesis of the Pluto-Charon binary. Within the past 18 months, 9 KBO satellite systems have been discovered, allowing for the first time the possibility of characterizing a sample of KBO satellite orbital properties. We propose HRC observations to determine satellite orbits in the 6 best cases. We have carefully devised a strategy for each of these 6 systems to make maximum use of ground-based observations, previous HST observations, and the smallest possible number of new HST observations. Our proposed observations will efficiently provide highly reliable orbital solutions which are critical to achieving the scientific promise available from the study of these systems. Our strategy relies heavily on extensive Monte Carlo simulations to define optimal times of observing such that each new point obtained gives maximum leverage for refining the orbital solution. We find that with this strategy we can provide mass solutions for all 6 systems to an accuracy of better than 10% using only 25 new HST observations. This highly efficient program provides extreme scientific output with optimal use of scarce resources. 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. NIC3 10337 The COSMOS 2-Degree ACS Survey NICMOS Parallels The COSMOS 2-Degree ACS Survey NICMOS Parallels. This program is a companion to program 10092. ACS/WFC/WFPC2 10092 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. 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. ACS/HRC/WFC 10060 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/CCD 10022 STIS CCD Hot Pixel Annealing Cycle 12 The effectiveness of the CCD hot pixel annealing process is assessed by measuring the dark current behavior before and after annealing and by searching for any window contamination effects. In addition CTE performance is examined by looking for traps in a low signal level flat. Follows on from proposal 9612. 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 10018 CCD Dark Monitor-Part 2 Monitor the darks for the STIS CCD. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) HSTAR 9417: GS Acquisition (2,1,2) @ 136/15:18:58Z ended in FL backup on FGS 2 due to SSLE on FGS 2 @ 136/15:22:27Z. Under investigation. HSTAR 9418: Saved FGS Error Null Bias (QSFGENB0), during successful GS Acquisition (2,1,2) @ 137/16:09:20Z, flagged OOL with a value of -1770.975 arcsec. Under investigation. COMPLETED OPS REQs: None OPS NOTES EXECUTED: 1234-0 - TDW Cross-support tracking (T77 CODE) @ 135/1756z, 136/0040z, 136/0403z, 136/1938z, 136/2125z, 137/0223z, 137/0415z, 137/1806z, 137/1940z, 137/2110z, 138/0044z, 138/0222z 1235-0 - Change Limits MAMA2 Threshold Voltage @ 136/2308z, 138/0838z SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 31 31 FGS REacq 22 22 FHST Update 28 28 LOSS of LOCK SIGNIFICANT EVENTS: SMS138O00 begins the use of reduced FGS Earth avoidance angles: Bright Earth avoidance angle went from 15.5 to 13.5 degrees. Dark Earth avoidance angle went from 7.6 to 6.0 degrees. |
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