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Daily 3647
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT #3647 PERIOD COVERED: DOYs 184-187 OBSERVATIONS SCHEDULED S/C/NIC1/NIC3 9994 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. STIS/CCD/MA2 9900 Boron in stars of same O and Li, but different Be: testing cosmic-ray vs. neutrino spallation We propose to further investigate the origin of the light elements Li, Be, and B, by observing B in a group of galactic stars found to have similar O abundances but to differ significantly in their Be content. Contrary to Li, which is produced in the Big Bang and its abundance in halo stars constrains primordial nucleosynthesis and the baryonic density, Be and B are produced later by cosmic ray spallation as the galactic halo forms. Knowledge of their evolution is now being used along with that of [O/H] {and [Fe/H]} as a powerful discriminant between different models of the chemical and dynamical evolution of the galaxy. Light element abundances can be used to test these theories only if they have not been altered by destruction in stars. Recently we have identified a small number of stars characterized by the same O abundance but large differences in their Be content, which cannot be accounted for by stellar depletion {since their Li is undepleted}. As neutrino-spallation contributes only to the production of isotope 11 of B, and not to Be, Be and B abundanes in the same stars will allow us to see if B scales with Be {evidence for a CR spallation origin} or with O {evidence for contribution from neutrino spallation}. NIC/NIC3/STIS/CCD 9877 A test of the foreground proximity effect at z=1.2 The diffuse UV background flux J is a crucial component for cosmological evolution models, though few determinations have been made. The proximity effect, the thinning out of the Lyman alpha forest near a sight- line's background quasar and explained at least partly by the enhanced ionization from the quasar, is a key method to measure J. A foreground proximity effect {FPE} should exist from quasars close on the sky but at different z; it can constrain J and test the enhanced ionization model. Galaxy clustering around the quasar may modify the effect, but knowing the galaxy density around the Lya forest should allow for corrections. We propose to measure the FPE at z=1.2, which is advantageous because 1} the diffuse UV flux is lower, and thus contrast with the UV flux of neighboring quasars is higher, and 2} galaxies are easier to identify at z=1.2. We have good knowledge of the physical volume we wish to study through surveys for quasars, MgII absorbers and galaxies, to constrain the redshift-dependent galaxy density along the line of sight. We will analyze the results based on pixel opacities, which is more sensitive to fluctuations in J than traditional line counting, and will compare our results with cosmological simulations to derive estimates of the UV background in the context of available physical models. 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. STIS/CCD/MA1/MA2 9871 AALs in Quasars: Diagnostics of the Environment Associated absorption lines {AALs} in quasar spectra carry a wealth of information on the gas-phase kinematics, ionization states, column densities, outflow masses, and elemental abundances near the quasars. Most of the existing UV spectra have low spectral resolution, which hampers efforts to accurately determine these properties at low redshifts. We propose medium-resolution FUV and NUV STIS spectroscopy, more than an order of magnitude improvement in spectral resolution over previous studies, to observe a sample of AAL quasars at redshifts and luminosities intermediate between the nearby Seyferts and the bright, high-z quasars. Our aim is to determine basic physical parameters for the absorbers, measure the abundances, search for AAL variability, and constrain the location of the absorbers relative to the central quasars. A unique aspect of our z~0.2 sample is the ability to get both UV and X-ray diagnostics, thus allowing us to perform a joint analysis of our STIS data with X-ray observations to further constrain the full range of ionizations and column densities of the UV/X-ray absorbing gas. 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/MA1/MA2 9827 UV extinction by dust in unexplored LMC environments The ensemble of results from studies of the UV extinction in the Milky Way, Magellanic Clouds {MC}, M31 and M33, indicates a complex dependence of the dust properties with environment, where starburst activity and metallicity are relevant factors. Work in the LMC to date, based on IUE data, has several drawbacks: a} only supergiants could be used, b} they all have moderate extinction, c} the IUE S/N is limited, d} the large IUE slit may include light from other sources, such as scattered light from dust or faint companion stars, e} studies are confined to few {extreme} environments. We propose to obtain UV extinction curves more accurate than previous ones {from STIS spectra of main sequence stars with higher reddening}, sampling four environments in the LMC with different levels of star formation activity, including the general field, hitherto unexplored. The results will characterize the properties of dust in different conditions, at the LMC metallicity, which is useful to interpret integrated properties of distant galaxies, as well as GALEX upcoming UV surveys. A complementary study is under way with FUSE in the far-UV range. The combined results will provide insight on the properties of small grains. STIS/CCD/MA1 9818 Reverberation Mapping of the Least Luminous Seyfert 1 Galaxy NGC 4395 We propose to make a short UV and optical reverberation mapping monitoring of NGC~4395, by far the least luminous Seyfert 1 galaxy known {M_B~ -10}, where the Broad Line Region {BLR} is most likely between a fraction of a light hour to a few light hours across. This program will: 1. extend by a factor of ~100 the range of R_BLR probed by RM, 2. allow to test models for AGN continuum emission and BLR structure at very low L and M_BH. 3. provide significantly more reliable estimates of its M_BH than currently available, 4. allow to probe the M_BH-sigma_* relation in AGN at very low M_BH, which cannot be probed by other methods. Existing archival FOS observations indicate significant {up to 30-40%} line and continuum variations within one orbit, suggesting that the proposed RM is likely to succeed. The unusually small R_BLR in NGC 4395 implies that RM can be performed here at only a fraction of the cost required in typical AGN. 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/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/WFPC2 9774 Young Massive Clusters in Spiral Galaxies and the Connection with Open Clusters We propose to carry out a census of star clusters in the disks of the nearby spiral galaxies NGC 45, NGC 1313, NGC 4395, NGC 5236 and NGC 7793. Using ACS, we will identify much fainter and older star clusters than possible in previous ground-based surveys, or even in HST imaging of more distant galaxies. For the first time, we will directly explore the connection between young "massive'' {or "super''} star clusters {YMCs} and lower-mass "open'' clusters in different star forming environments. We will test the universality of the luminosity- and mass functions of stellar clusters and establish whether the presence of YMCs is a result of a top-heavy cluster luminosity function, or follows from generally richer cluster systems. Our target galaxies span a range of morphological properties, surface brightness and star formation rate. Some of them are known from ground-based studies to host large numbers of YMCs while others have more modest cluster populations. However, previous ground-based data were restricted to luminous clusters younger than about 500 Myr. Here we will extend the search to clusters formed throughout the entire lifetime of each galaxy and reach clusters with properties typical of the Milky Way open clusters. This will allow us to close the gap between studies of extragalactic and Galactic disk clusters. ACS/HRC/WFC 9770 Galaxy Evolution During Half the Age of the Universe: ACS imaging of rich galaxy clusters Detailed studies of nearby galaxies {z0.05} have shown that galaxies have very complex histories of formation and evolution involving mergers, bursts of star formation, and morphological changes. Even so, the global properties of the galaxies {radii, luminosities, rotation velocities, velocity dispersions, and absorption line strengths} follow a number of very tight {empirical} scaling relations, e.g. the Tully-Fisher relation and the Fundamental Plane. These relations place constraints on models for galaxy evolution. The results for nearby galaxies rely on high signal-to-noise spectroscopy and multi-color photometry. With the Gemini Telescopes and the Hubble Space Telescope {HST} it is possible to carry out similar detailed studies of galaxies at much larger redshifts, up to z~1.0, equivalent to half the age of the Universe. We have started a project using the scaling relations and aimed at studying the galaxy evolution over the last half of the age of the Universe. The project is based on a large database of spectroscopy and photometry of galaxies in 15 X-ray selected clusters of galaxies with redshifts between 0.15 and 1.0. Spectroscopic observations are being obtained using both Gemini Telescopes; we have observed 6 clusters so far, covering from z=0.18 to z=0.83. We propose to use HST/ACS to image the clusters and determine the morphologies and measure the sizes of the galaxies. At this time we ask for 26 orbits to image four of the clusters in our sample. ACS/WFC 9765 The Dusty ISM Substructure in Nearby Spiral Galaxies We propose an ACS V&I imaging snapshot survey of all nearby edge-on spiral galaxies in order to measure the small scale structures in their dust extinction down to the 10pc scale. Dust and molecular gas are tightly coupled and therefore HST high resolution reddening maps can reveal information about the cold ISM phase on a scale inaccessible from the groundby any other means. We have recently discovered a sudden change in dust lane properties using ground-based data; all galaxies with rotation speeds in access of 120km/s show dust lanes, but none of the slower rotators does. This transition may be caused by a sudden change in the state of the multiphase ISM, and HST resolution imaging is needed to fully quantify this effect. Analysis will consist of full radiative transfer modeling of dust extinction with realistic, fractal like substructure and power spectrum analysis of the structure from the global to the 10pc scale. By observing a sample of galaxies with a range in structural parameters we can quantify how the cold ISM structure changes as function of radius, rotation speed, local surface density, et cetera. This information is duly needed with SIRTF soon providing a wealth of information on dust absorption, but lacking the resolution to determine the small scale distribution of the dust. STIS/CCD/MA1 9736 Integrated Absorption- and Emission-Line Analysis of Nebulae Serious discrepancies have arisen in CNONe abundance determinations for galactic nebulae in the past ten years depending upon which type of emission lines are used in the analysis: forbidden vs. permitted lines. The cause of the discrepancies, which can exceed an order of magnitude for some PNe, has been studied intensively but is still unknown. Emission line abundances cannot be considered reliable until the nature of these contradictory results is understood. We have developed a technique for integrating absorption lines into emission analyses for diffuse nebulae that provides an independent check on the validity of emission-line analyses. It requires high resolution observations of UV resonance absorption produced by the nebular gas in imbedded or background stars together with optical spectra of the nebulae. We propose to obtain UV spectra of four PNe central stars with STIS that will provide data necessary to exploit the new technique of integrated abundance determination that combines both emission and absorption lines. 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. 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. S/C 10336 2-Gyro Reacquisition Test This proposal will test the software that will be used to perform target reacquisition when HST only has two working gyroscopes. ACS/HRC 10272 A Snapshot Survey of the Sites of Recent, Nearby Supernovae During the past few years, robotic {or nearly robotic} searches for supernovae {SNe}, most notably our Lick Observatory Supernova Search {LOSS}, have found hundreds of SNe, many of them in quite nearby galaxies {cz 4000 km/s}. Most of the objects were discovered before maximum brightness, and have follow-up photometry and spectroscopy; they include some of the best-studied SNe to date. We propose to conduct a snapshot imaging survey of the sites of some of these nearby objects, to obtain late-time photometry that {through the shape of the light and color curves} will help reveal the origin of their lingering energy. The images will also provide high-resolution information on the local environment of SNe that are far superior to what we can procure from the ground. For example, we will obtain color-color and color-magnitude diagrams of stars in these SN sites, to determine their progenitor masses and constraints on the reddening. Recovery of the SNe in the new HST images will also allow us to actually pinpoint their progenitor stars in cases where pre-explosion images exist in the HST archive. Use of ACS rather than WFPC2 will make our snapshot survey even more valuable than our Cycle 9 survey. This Proposal is complementary to our Cycle 13 archival proposal, in which we outline a plan for using existing HST images to glean information about SN environments. ACS/WFC 10260 The Most Massive Star Clusters: Supermassive Globular Clusters or Dwarf Galaxy Nuclei? Evidence is mounting that the most massive globular clusters, such as Omega Centauri and M31-G1, may be related to the recently discovered "Ultra-Compact Dwarfs" and the dense nuclei of dE, N galaxies. However, no systematic imaging investigation of these supermassive globular clusters -- at the level of Omega Cen and beyond -- has been done, and we do not know what fraction of them might bear the signatures {such as large effective radii or tidal tails} of having originated as dE nuclei. We propose to use the ACS/WFC to obtain deep images of 18 such clusters in NGC 5128 and M31, the two nearest rich globular cluster systems. These globulars are the richest star clusters that can be found in nature, the biggest of them reaching 10^7 Solar masses, and they are likely to represent the results of star formation under the densest and most extreme conditions known. Using the profiles of the clusters including their faint outer envelopes, we will carry out state-of-the-art dynamical modelling of their structures, and look for any clear evidence which would indicate that they are associated with stripped satellites. This study will build on our previous work with STIS and WFPC2 imaging designed to study the 'Fundamental Plane' of globular clusters. When our new work is combined with Archival WFPC2, STIS, and ACS material, we will also be able to construct the definitive mapping of the Fundamental Plane of globular clusters at its uppermost mass range, and confirm whether or not the UCD and dE, N objects occupy a different structural parameter space. NIC/NIC3 10226 The NICMOS Grism Parallel Survey 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. NIC2 10176 Coronagraphic Survey for Giant Planets Around Nearby Young Stars A systematic imaging search for extra-solar Jovian planets is now possible thanks to recent progress in identifying "young stars near Earth". For most of the proposed young {~ 30 Myrs} and nearby {~ 60 pc} targets, we can detect a few Jupiter-mass planets as close as a few tens of AUs from the primary stars. This represents the first time that potential analogs of our solar system - that is planetary systems with giant planets having semi-major axes comparable to those of the four giant planets of the Solar System - come within the grasp of existing instrumentation. Our proposed targets have not been observed for planets with the Hubble Space Telescope previously. Considering the very successful earlier NICMOS observations of low mass brown dwarfs and planetary disks among members of the TW Hydrae Association, a fair fraction of our targets should also turn out to posses low mass brown dwarfs, giant planets, or dusty planetary disks because our targets are similar to {or even better than} the TW Hydrae stars in terms of youth and proximity to Earth. Should HST time be awarded and planetary mass candidates be found, proper motion follow-up of candidate planets will be done with ground-based AOs. 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. ACS/HRC 10130 Systemic Proper Motions of the Magellanic Clouds from Astrometry with ACS: II. Second Epoch Images We request second epoch observations with ACS of Magellanic Cloud fields centered on the 40 quasars in the LMC and SMC for which we have first epoch Cycle 11 data. The new data will determine the systemic proper motion of the Clouds. An extensive astrometric analysis of the first epoch data shows that follow-up observations with a two year baseline will allow us to measure the proper motion of the clouds to within 0.022 mas/year in each of the two orthogonal directions {assuming that we can image 25 quasars, i.e., with a realistic Snapshot Program completion rate}. The best weighted combination of all previous measurements has a seven times larger error than what we expect. We will determine the proper motion of the clouds with 2% accuracy. When combined with HI data for the Magellanic Stream this will constrain both the mass distribution in the Galactic Halo and theoretical models for the origin of the Magellanic Stream. Previous measurements are too crude for such constraints. Our data will provide by far the most accurate proper motion measurement for any Milky Way satellite. WFPC2 10072 WFPC2 CYCLE 12 INTERNAL MONITOR This calibration proposal is the Cycle 12 routine internal monitor for WFPC2, to be run weekly to monitor the health of the cameras. A variety of internal exposures are obtained in order to provide a monitor of the integrity of the CCD camera electronics in both bays {gain 7 and gain 15}, a test for quantum efficiency in the CCDs, and a monitor for possible buildup of contaminants on the CCD windows. 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. WFPC2 10068 WFPC2 CYCLE 12 Standard Darks This dark calibration program obtains dark frames every week in order to provide data for the ongoing calibration of the CCD dark current rate, and to monitor and characterize the evolution of hot pixels. Over an extended period these data will also provide a monitor of radiation damage to the CCDs. ACS/HRC/WFC 10061 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 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. STIS/MA1 10034 Cycle 12 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/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. NIC3 10014 Spectrophotometry of FAINT IR STANDARDS We propose to establish new IR faint standards in the 15-17 mag range. Appropriate spectral types for faint IR standards are solar analogs and hotter WDs. Many M type and cooler stars are variable, so that long term monitoring is required before committing HST time to such cool stars. A few G type and WD faint stars will provide a set of faint IR standards with minimal sky and color coverage. Existing HST images of any candidates can provide verification that there are no contaminating stars above the 1% level within 2-3arcsec. However, the ACS calibration field in 47 Tuc is too crowded for linking to ground based observations. If the other candidates are selected from SDSS or other ground based data, then the NICMOS and STIS acquisition images can provide this verification, as well as correction factors for arbitrary photometric size apertures. The SNAP team is providing the northern faint stars using unreleased SDSS data. In addition, the extreme coolest types such as L and T stars have proven essential to sorting out the long wavelength QE of ACS; both the ACS and eventually WFC3 calibrations could be improved with knowledge of L and T SEDs in the region beyond 0.95 microns. In addition to the primary purpose of ACS QE vs. wavelength and broad band F814W and F850LP calibrations, these three stars in C.} below are at the flux level required for WFC3 grism calibration. The brighter M, L, and T standard stars will each require a NICMOS orbit, while each faint standard requires two NICMOS orbits and one STIS orbit for complete wavelength coverage. The STIS spectra of the M and L stars are done as ACS calibrations in cycles 12 and 11, respectively. An additional faint WD has already been proposed for 2 NICMOS and 4 STIS orbits in their cycle 12 programs already. See Table 1 for a summary of the 18 orbit allocation for this program 10014. Bright stars in the V=0-6 mag range would be useful for direct comparisons to NIST calibrated lamps. This comparison would offer the opportunity to compare two fundamentally different realms of physics: pure hydrogen stellar models and laboratory black body physics. Unfortunately, the NICMOS bright limit is V=~8 for a solar analog and a 1s exposure without defocussing the OTA. The primary Sloan standard BD+17d4708 at V=9.9 is safely fainter than this NICMOS limit. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) HSTAR 9461: FHST Roll Delay Update (U2,3RD) @ 184/13:14:22Z failed with Error Box results indicating tracker "2FAILED" for mnemonics QEBSTFG0, QEBSTFG1, and QEBSTFG2. Prior FHST Map @ 184/12:57:30Z showed 3-axis (RSS) value ~ 9.00 arcsec. Subsequent GS Acquisition (2,1,1) @ 184/13:45:28Z was successful. Under investigation. HSTAR 9462: GS Acquisition (3,2,2) @ 184/15:04:40Z, during ZOE, resulted in FL backup using FGS 3 at AOS without FGS indicating flags. FGS Modes and flag bit changes could not be determined at this time pending future ETR dump. Prior FHST FM Updates @ 184/14:49:04Z and 14:51:49Z showed good attitude error correction. Subsequent GS Reacquisition (3,2,2) @ 184/16:40:49Z resulted in FL backup. Under investigation. HSTAR 9463: FHST Roll Delay Update (U2,3RD) @ 184/22:53:51Z failed with Error Box results indicating "2FAILED" for mnemonics QEBSTFG0, QEBSTFG1, and QEBSTFG2. Subsequent GS Acquisition (2,1,1) @ 184/23:10:42Z was successful. Under investigation. HSTAR 9466: FHST Full Maneuver Updates failed (Optimal FHST Pair 1,3), during ZOE @ 186/177:15:14Z and 186/17:53:59Z. Error Box results indicating "3FAILED" for mnemonics QEBSTFG0, QEBSTFG1, and QEBSTFG2 at AOS. Subsequent GS Acquisition (2,1,1) @ 186/17:56:44Z was successful. Extract of engineering telemetry following ETR dump showed BOTH of the Full Maneuver Updates failed. Under investigation. HSTAR 9467: FHST Full Maneuver Update (U1,2FM) @ 187/04:35:12Z failed with Error Box results indicating "2FAILED" for mnemonics QEBSTFG0, QEBSTFG1, and QEBSTFG2 @ 187/04:35:46Z. Second FHST FM Update @ 187/04:40:12Z was successful, as was GS Acquisition (3,2,2) @ 187/05:14:44Z. Under investigation. HSTAR 9468: GS Acquisition (3,2,2) @ 187/07:25:00Z failed to FL backup on FGS 3. Upon AOS, HST was operating in FL backup on FGS 3 only. Further information after engineering recorder dump. No FGS flags were set at AOS. Extracted engineering data showed SSLE @ 187/07:05:19Z, GS Reacquisition (3,2,2) @ 187/08:38:28Z also failed to FL backup on FGS 3. HSTAR 9469: GS Acquisition (3,2,2) @ 187/11:51:10Z resulted in FL backup, guiding on FGS 3 due to SSLE on FGS 2. FHST Map @ 187/12:30Z showed vehicle axis errors of 4.756, -4.453, and 3.257 arcsec. GS Reacquisition (3,2,2) @ 187/13:36:11Z also failed to FL backup. Under investigation. COMPLETED OPS REQs: 17201-0 Battery 5 Capacity Test @ 184/1440z 17207-0 Set up ACS memory monitor @ 184/1612z OPS NOTES EXECUTED: 1248-0 RTCS 26 Inhibited in SMS 187 @ 187/0047z 1249-0 Verify ACS FW2 Fourier Correction Alogrithm Update @ 187/0047z 0916-0 Tabulation of Slew Attitude Error (Miss-distance) @ 187/0138z SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 35 35 FGS REacq 24 24 FHST Update 55 50 184/13:14:22z, 184/22:53:51z 186/17:51:14z, 186/17:53:59z 187/04:35:46z SIGNIFICANT EVENTS: Battery 5 discharge at the high rate continued until 181/20:17Z where the Battery 5 Voltage dropped to 26.63 Volts and the FSW ACR autonomously switched to the low rate, as planned. The measure capacity was 54.5 Ah. Based on discharge through the 5.1 Ohm resistor. When Battery 5 was last tested in July 2003, the capacity was measured to be 61.2 Ah. The discharge continued until Battery 5 dropped below 5 Volts @ 183/14:30Z. The battery was placed back on charge with one SPA online for one orbit and OCA disabled. The other two SPAs were autonomously brought online the second orbit. OCA was enabled @ 183/23:54Z. Battery 5 returned to FSW 6-battery system @ 184/14:29Z. An update to the NCS Temperature setpoint was last routinely reset on Day 100 to its current seasonal setting. The seasonal setpoint setting was lowered by 0.05 degrees @ 187/00:10Z, executed entirely from the SMS. Setup ACS Memory Monitor to capture SMS commanding to update a constant term in the ACS Filter Wheel 2 Resolver Fourier Correction algorithm and the mechanism raw resolver counts @ 184/16:12Z (OR 17207). Updated the constant term in the ACS Filter Wheel 2 Resolver Fourier Correction algorithm (EDAC RAM) @ 187/00:31Z; executed entirely from the SMS. This change was done to correct a bias subsequently observed in the resolver readings and should prevent the reoccurrence of Filter Wheel positioning errors, see HSTAR 9455. Update also added to the Boot-to-Operate reconfiguration instruction. Repeated the Two-Gyro Target Reacquisition test @ 187/03:29Z, special command Proposal 10336, executed entirely from the SMS. Gyro Scale Factor was modified for this calendar; modified value is: rga_scale_error = 1.4"/degree. SSA Transmitter 1 was placed back in service starting SMS 187. PCS and SAC rescheduled a routine update to the RGA Scale Factor/Alignment Table and Bias Offset Calibration. These changes involve relatively minor corrections to the Gyro Scale Factor and High Mode Bias Offset tables. Two uplink opportunities are identified: 188/16:02:11Z - 188/16:27:42Z and 188/19:34:22Z - 20:17:00Z. Vehicle will be RGA Hold during the uplink, with the FGSs in default. As before there is a concurrent ACS observation during the identified window, but this internal CCD monitoring Proposal 10061 "CCD Daily Monitor" should remain unaffected by these activities. |
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