#1
|
|||
|
|||
Daily 3641
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3641 PERIOD COVERED: DOY 176 OBSERVATIONS SCHEDULED ACS/HRC 10050 ACS Earth Flats High signal sky flats will be obtained by observing the bright Earth with the HRC and WFC. These observations will be used to verify the accuracy of the flats currently used by the pipeline and will provide a comparison with flats derived via other techniques: L-flats from stellar observations, sky flats from stacked GO observations, and internal flats using the calibration lamps. Weekly coronagraphic monitoring is required to assess the changing position of the spots. 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. 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. 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. ACS/WFC 9777 The environment of QSOs at the reionization epoch Our goal is to elucidate the role of QSOs and galaxies at the tail end of reionization by identifying z~6 galaxies near SDSS z6 QSOs through their red i-z colors. A similar technique was used by the SDSS to identify the QSOs themselves. Based on our understanding of the growth of structure in the Universe and on observations at z ~= 4, we expect z~6 QSOs to be associated to the high peaks in the matter density distribution. Therefore, they should be surrounded by an excess of objects - as compared to random fields - unless the ionizing radiation from the QSOs themselves is inhibiting star formation. We will concentrate on 5 QSOs discovered by the SDSS at z~6 and spend 7 orbits with ACS on each of the QSO fields {2.5 in F775W - i - and 4.5 in F850LP - z}, for a total of 35 orbits. The exposures are optimized for the detection of objects with i-z 2. The reference properties of the field population will be provided by GOODS which is reaching the same depth. The proposed observations will be capable of revealing the dominant effect between galaxy suppression by the QSO ionizing flux and number density excess due to clustering. We will test whether the balance between suppression and enhancement evolves with redshift. We will also be able to estimate for these fields the ionizing continuum contribution by galaxies and compare it with that of the QSOs. If galaxies are found to be comparably important to QSOs in these selected fields, the idea that hydrogen reionization is primarily due to stellar radiation would be significantly strengthened. ACS/WFC/NIC3/WFPC2 10134 The Evolution and Assembly of Galactic Disks: Integrated studies of mass, stars and gas in the Extended Groth Strip This project is a 126-orbit imaging survey in F606W/F814W ACS to measure the evolution of galaxy disks from redshift z = 1.4 to the present. By combining HST imaging with existing observations in the Extended Groth Strip, we can for the first time simultaneously determine the mass in dark matter that underlies disks, the mass in stars within those disks, and the rate of formation of new stars from gas in the disks, for samples of 1, 000 objects. ACS observations are critical for this work, both for reliable identifications of disks and for determining their sizes and inclinations. Combining these data with the kinematics measured from high-resolution Keck DEIMOS spectra will give dynamical masses that include dark matter. Stellar masses can be measured separately using ground-based BRIK and Spitzer IRAC GTO data, while cross-calibrated star formation rates will come from DEEP2 spectra, GALEX, and Spitzer/MIPS. The field chosen is the only one where all multiwavelength data needed will be available in the near term. These data will show how the fundamental properties of disks {luminosity, rotation speed, scale length} and their scaling relations have evolved since z~1, and also will measure the build-up of stellar disks directly, providing fundamental tests of disk formation and evolution. In addition to the above study of disk galaxies, the data will also be used to measure the evolution of red-sequence galaxies and their associated stellar populations. ACS images will yield the number of red-sequence galaxies versus time, together with their total associated stellar mass. ACS images are crucial to classify red-sequence galaxies into normal E/S0s versus peculiar types and to measure radii, which will complete the suite of fundamental structural parameters needed to study evolution. We will measure the zeropoints of major scaling laws {Fundamental Plane, radius versus sigma}, as well as evolution in characteristic quantities such as L*, v*, and r*. Stellar population ages will be estimated from high-resolution Keck DEIMOS spectra and compared to SED evolution measured from GALEX, HST, Spitzer, and ground-based colors. Important for both disk and red-galaxy programs are parallel exposures to be taken with both NIC3 {J and H} and WFPC2 {B}. These are arranged so that ACS, WFPC2, and NIC3 all overlap where possible , providing a rich data set of galaxies imaged with all three HST cameras from B to H. These data will be used to measure restframe visible morphologies and UV star-formation rates for galaxies near the edge of the survey, to discover and count EROs below the Keck spectroscopic limit of R = 24, and to provide an improved database of photometric redshifts for galaxies in the overlap regions. 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. NIC1/NIC2/NIC3 8793 NICMOS Post-SAA calibration - CR Persistence Part 4 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. NIC2 9875 The Fundamental Plane of Massive Gas-Rich Mergers We propose deep NICMOS H-band imaging of a carefully selected sample of 33 luminous, late-stage galactic mergers. This program is part of a comprehensive investigation of the most luminous mergers in the nearby universe, the ultraluminous infrared galaxies {ULIGs}. The high-resolution HST images will complement an extensive set of ground-based data that include long-slit NIR spectra from a recently approved Large VLT Programme. This unique dataset will allow us to derive with unprecedented precision structural -and- kinematic parameters for a large unbiased sample of objects spanning the entire ULIG luminosity function. These data will refine the fundamental plane of massive gas-rich mergers and enable us to answer the following questions: {1} Do ultraluminous mergers form elliptical galaxies, and in particular, giant ellipticals? {2} Do ULIGs evolve into optically bright QSOs? The results from this detailed study of massive mergers in the local universe will be relevant to understanding galaxy formation and evolution at earlier epochs, and in particular, the dusty sub-mm population that accounts for more than half of the star formation at z 1. NIC3 9998 NICMOS Cycle 12 Grism Calibration and Standard Stars to 2.5microns This is the grism calibration proposal. 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 10018 CCD Dark Monitor-Part 2 Monitor the darks for the STIS CCD. 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/MA1 9758 Iron deficiency in hot hydrogen-deficient post-AGB stars The first attempt to measure the iron abundance in hot hydrogen-deficient post-AGB stars arrived at a surprising result. From the non-detection of iron lines in FUSE spectra of three extremely hot {Teff100, 000K} PG1159-type central stars of the planetary nebulae, we found that iron is deficient by at least one order of magnitude. We propose HST/STIS observations of three hydrogen-deficient post-AGB stars, each representing the UV-brightest member of a spectroscopic subclass. High-resolution UV spectroscopy will reveal the origin of the iron deficiency. The determination of the Fe/Ni abundance ratio can decide if dust fractionation in the former AGB star atmosphere or s-process neutron-capture in the interior helium-buffer layer is responsible for the iron depletion. In the latter case we can verify our understanding of the "born-again'' star phenomenon and of the s-process synthesis of trans-iron elements in low-mass AGB stars. WFPC2 10071 WFPC2 CYCLE 12 Supplemental Darks Part 3/3 This dark calibration program obtains 3 dark frames every day to provide data for monitoring and characterizing the evolution of hot pixels. 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 06 06 FGS REacq 10 10 FHST Update 09 09 LOSS of LOCK SIGNIFICANT EVENTS: PSS Serial testing scheduled 177/13:30Z - 18:30Z with GDOC, SOC, HITT using CCS "H" String with CCS Release 5.0.3.1 and PRD xx (intentionally removed). The purpose of this testing is to verify PSS CR 7992 and successful telemetry transmission and command response functionality via serial link from Building xx (intentionally removed). |
Thread Tools | |
Display Modes | |
|
|
Similar Threads | ||||
Thread | Thread Starter | Forum | Replies | Last Post |
Monitoring NASA Daily ISS Report | JimO | Space Station | 2 | June 1st 04 10:33 PM |
JimO Speaks on 'Daily Planet' re Hubble | JimO | Policy | 0 | February 11th 04 10:53 PM |
Spirit's daily activities schedule? | Matti Anttila | Policy | 0 | January 15th 04 08:39 AM |
best site for daily schedule of rover activity? | bob | History | 2 | January 5th 04 12:16 PM |
Investor's Business Daily: Rethinking NASA | dougk | Policy | 1 | August 28th 03 12:07 AM |