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Daily 3445
HUBBLE SPACE TELESCOPE DAILY REPORT******* # 3445 PERIOD COVERED: DOY 253 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 9760 ACS Imaging of the Gemini Deep Deep Survey Fields: Galaxy Assembly at z = 1.5 We are presently carrying out the deepest redshift survey ever undertaken {the Gemini Deep Deep Survey}. Spectra of extraordinary quality have been taken in order to obtain redshifts in the so-called "redshift desert" at 1z2. This redshift range corresponds to the epoch of peak galaxy formation. In this proposal we request 40 orbits of ACS imaging to determine the morphologies of 100-120 candidate early-type galaxies with known redshifts in our survey fields. We seek to determine if these systems are indeed elliptical galaxies and to link their morphological states to their spectroscopically determined ages, recent star-formation histories, and to the evolving global stellar mass function at the peak epoch of galaxy assembly. ACS/HRC 9719 Metallicity Spreads in M31 Globular Clusters Our recent deep HST photometry of the M31 halo globular cluster {GC} Mayall~II, also called G1, has revealed a red-giant branch with a clear spread that we attribute to an intrinsic metallicity dispersion of at least 0.4 dex in [Fe/H]. The only other GC exhibiting such a metallicity dispersion is Omega Centauri, the brightest and most massive Galactic GC, whose range in [Fe/H] is about 0.5 dex. These observations are obviously linked to the fact that both G1 and Omega Cen are bright and massive GC, with potential wells deep enough to keep part of their gas, which might have been recycled, producing a metallicity scatter among cluster stars. These observations dramatically challenge the notion of chemical homogeneity as a defining characteristic of GCs. It is critically important to find out how common this phenomenon is and how it can constrain scenarios/models of GC formation. The obvious targets are other bright and massive GCs, which exist in M31 but not in our Galaxy where Omega Cen is an isolated giant. We propose to acquire, with ACS/HRC, deep imaging of 3 of the brightest M31 GCs for which we have observed velocity dispersion values similar to those observed in G1 and Omega Cen. A sample of GCs with chemical abundance dispersions will provide essential information about their formation mechanism. This would represent a major step for the studies of the origin and evolution of stellar populations. ACS/WFC 9744 HST Imaging of Gravitational Lenses Gravitational lenses offer unique opportunities to study cosmology, dark matter, galactic structure, galaxy evolution and quasar host galaxies. They are also the only sample of galaxies selected based on their mass rather than their luminosity or surface brightness. While gravitational lenses can be discovered with ground-based optical and radio observations, converting them into astrophysical tools requires HST. HST has demonstrated that it is the only telescope that can in each case precisely locate the lens galaxy, measure its luminosity, color and structure, and search for lensed images of the source host galaxy given the typical image separations of ~1''. We will obtain ACS/WFC V and I images and NICMOS H images of 21 new lenses never observed by HST and NICMOS H images of 16 lenses never observed by HST in the IR. As in previous cycles, we request that the data be made public immediately. NIC3/ACS/HRC/WFC 9803 Deep NICMOS Images of the UDF The ACS Ultra Deep Field {UDF} images will greatly enhance the rich suite of deep multi-wavelength images in the Chandra Deep Field South {CDF--S}. We propose to complete the image set with deep near-IR NICMOS images at 1.1 and 1.6 microns over a significant fraction of the UDF, providing a critical link between the HST ACS and SIRTF observations. The timely addition of the near-IR images ensures that investigators will have images that span the spectrum from X-ray to far IR. In recognition of the value of the near IR images this proposal is submitted as a Treasury proposal with no proprietary period. The proposal team will deliver science quality images, mosaiced images covering 4.9 sq arc min, and a photometric catalog complete to an AB mag of 28.2 in both the F110W and F160W filters. The program also delivers a parallel extremely deep ACS field, 8' away, that reaches to within 0.6 mag of the UDF in the same filters as the UDF. The scientific program of the proposal team focuses on the star formation history of the universe, evolved galaxies at high redshift, galaxies at the epoch of reionization, and the redshift evolution of AGNs and ULIRGs. The HDF-N is currently the only field with spatially-coincident deep HST imaging in both the optical and near-IR. The small size of the HDF-N means that large scale structure is the dominant error in the results from the HDF-N. Providing observations in a field that is spatially uncorrelated is critically important. The UDF/CDF-S fulfills that goal. The depth of the UDF ACS imaging, and the wealth of Great Observatory and ground based observations in the CDF-S, make these NICMOS observations uniquely valuable. An extraordinarily rich array of science opportunities await the community from the NICMOS UDF data. 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 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 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 9712 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. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) None Executed Ops Note 1156:* Change Limits MAMA 1 Threshold Voltage @ 254/03:00Z. ****************************** Scheduled********** Successful FGS Aquisitions************ 5************************* 5 FGS ReAcqs**************** 9************************* 9 FHST Updates************* 13*********************** 13 LOL SIGNIFICANT EVENTS: Completed FSW 2.4a RAM Installation/Backout and EEPROM Installation OAT 252/10:11Z 253/01:55Z.* Both FSW 2.4a RAM Installation and Backout (IP-42) and EEPROM Installation (IP-43) were completed successfully.* In addition, IP-45 Enable/Disable/Preview Onboard Magnetic Field Model Procedure was exercised in Preview Mode for 1 plus orbit.* At the end of the test, updated DMS,. TCLs: XSUBCWPF, XSUBCWPN, QTABCHEK, and QTABCRD were run against the VEST using an argument of 340, the new table value addition to the procedures.* This completes Level 3 validation of these procedures. Completed SUN Transition B Side Command testing 253/11:00Z 18:00Z.* The SUN F String and SGI B String platforms compared nominally through a series of command functions.* The test was run completely on the B-side with Q, I, and S channel data being ingested.* No errors were seen in telemetry. Completed SDH/HSTPS Account Verification testing 252/11:02Z 19:55Z. Testing was partially successful.* Compared D and F String results against the B String.* Although, eventually got a Non-PN (RS) encoded science SSR dump to work, it took 5 attempts to see success on all strings.* Saw missing and incomplete packets first on D String, then on F String, then Dand F and finally all three strings.* All strings were on INTA, all objectives were eventually met. |
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