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Daily 3528
HUBBLE SPACE TELESCOPE
DAILY REPORT # 3528 PERIOD COVERED: DOYs 9-11/2004 OBSERVATIONS SCHEDULED ACS 9984 Cosmic Shear With ACS Pure Parallels Small distortions in the shapes of background galaxies by foreground mass provide a powerful method of directly measuring the amount and distribution of dark matter. Several groups have recently detected this weak lensing by large-scale structure, also called cosmic shear. The high resolution and sensitivity of HST/ACS provide a unique opportunity to measure cosmic shear accurately on small scales. Using 260 parallel orbits in Sloan textiti {F775W} we will measure for the first time: beginlistosetlength sep0cm setlengthemsep0cm setlength opsep0cm em the cosmic shear variance on scales 0.7 arcmin, em the skewness of the shear distribution, and em the magnification effect. endlist Our measurements will determine the amplitude of the mass power spectrum sigma_8Omega_m^0.5, with signal-to-noise {s/n} ~ 20, and the mass density Omega_m with s/n=4. They will be done at small angular scales where non-linear effects dominate the power spectrum, providing a test of the gravitational instability paradigm for structure formation. Measurements on these scales are not possible from the ground, because of the systematic effects induced by PSF smearing from seeing. Having many independent lines of sight reduces the uncertainty due to cosmic variance, making parallel observations ideal. STIS/CCD 9981 The Ultra Deep Field - STIS parallels We propose to obtain slitless spectroscopy of objects in the GEMS and GOODS area around the UDF. WFPC2 9980 The Ultra Deep Field - WFPC2 Parallels The ACS Ultra Deep Field {UDF} is a survey carried out by using Director's Discretionary time. The main science drivers are galaxy evolution and cosmology. The primary instrument is the Advanced Camera for Surveys but WFPC2, NICMOS, and STIS will also be used in pure parallel mode. The data will be made public. The UDF consists of a single ultra-deep field {410 orbits in total} within the CDF-S GOODS area. We request a modification of the default pure parallel programs. Rather than duplicate the redder 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, allowing determination of 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. NIC3 9979 The Ultra Deep Field - NICMOS Parallels This is a plan to manage the NICMOS pure parallels of the ACS Ultra Deep Survey. We will obtain a mix of F110W and F160W images along sight-lines within the mosaiced ACS fields of the CDF-S GOODS and GEMS surveys, with these sight-lines enabling an examination of the space density and morphologies of the reddest galaxies. ACS/CCD/WFC 9978 The Ultra Deep Field with ACS The ACS Ultra Deep Field {UDF} is a survey carried out by using Director's Discretionary time. The main science driver are galaxy evolution and cosmology. The primary instrument is the Advanced Camera for Surveys but WFPC2 and NICMOS will also be used in parallel. The data will be made public. The UDF consists of a single ultra-deep field {410 orbits in total} within the CDF-S GOODS area. The survey will use four filters: F435W {55 orbits}, F606W {55 orbits}, F775W {150 orbits}, and F850LP {150 orbits}. The F435W {B} and F606W {V} exposures will be one magnitude deeper than the equivalent HDF filters. The F775W {I} exposure will be 1.5 magnitude deeper than the equivalent HDF exposure. The depth in F775W and F850LP is optimized for searching very red objects - like z=6 galaxies - at the detection limit of the F850LP image. The pointing will be RA{J2000}=3 32 40.0 and Decl.{J2000}=-27 48 00. These coordinates may change slightly due to guide star availability and implementation issues. We will attempt to include in the field both a spectroscopically confirmed z=5.8 galaxy and a spectroscopically confirmed type Ia SN at z=1.3. The pointing avoids the gaps with the lowest effective exposure on the Chandra ACIS image of CDFS. This basic structure of the survey represents a consensus recommendation of a Scientific Advisory Committee to the STScI Director Steven Beckwith. A local Working Group is looking in detail at the implementation of the survey. FGS 9969 FGS Astrometry of the Extrasolar Planet of Epsilon Eridani We propose observations with HST/FGS in Position Mode to determine the astrometric elements {perturbation orbit semimajor axis and inclination} of the candidate extra-solar planet around the K2 V star Epsilon Eridani that has been detected by Doppler spectroscopy. These observations will also permit us to determine the actual mass of the planet by providing the sin{i} factor which can not be determined with the radial velocity method. High precision radial velocity {RV} measurements spanning the years 1980.8--2000.0 for the nearby {3.22 pc} star Epsilon Eri show convincing variations with a period of ~ 7 yrs. These data represent a combination of six independent data sets taken with four different telescopes. A least squares orbital solution using robust estimation yields orbital parameters of period, P = 6.9 yrs, velocity K- amplitude = 19 m/s, eccentricity e = 0.6, projected companion mass M_B sin{i} = 0.83 M_Jupiter. An estimate of the inclination yields a perturbation semi-major axis, Alpha = 0arcs0022, easily within the reach of HST/FGS astrometry. ACS/HRC/WFC 9919 The Morphological, Photometric, and Spectroscopic Properties of Intermediate Redshift Cluster Galaxies: New and fundamental constraints on the evolutionary state of high redshift clusters will be made by obtaining deep, multiband images {SDSS r, i, z} over the central 1.5 Mpc regions of seven distant clusters in the range 0.76 z 1.27. The ACS data will allow us to {1} definitively establish the morphological composition and star formation rates as functions of clustercentric radius, local density, x-ray luminosity {obtained from accompanying Chandra, and XMM data}, {2} explore the relationship between substructure, kinematics, and morphology, {3} strongly constrain the galaxy merger frequency and the origins of elliptical and S0 galaxies, {4} measure the mass distribution independently from the light {via gravitational lensing} enabling comparisons with kinematically derived masses, and {5} study the evolution of the structure of the brightest cluster members. The clusters selected for this program already have extensive spectroscopic observations and NIR imaging is either in hand or underway from approved ground based programs. To date, the lower part of this redshift range has only been marginally studied with HST. Our sample includes the two most distant, spectroscopically confirmed superclusters and will significantly increase the baseline over which evolutionary effects can be studied. The data will also be used to identify very high-z galaxies via their unique spectral properties. FGS 9882 The Distance and Mass of the Neutrino-Luminous White Dwarf PG 0122+200 PG 0122+200 is a pulsating hot white dwarf that is believed to radiate more energy as neutrinos than it does as photons. We propose to measure with FGS the trigonometric parallax of PG 0122+200 and thereby determine its distance, luminosity, and mass. Ongoing investigations from the ground will infer the neutrino luminosity through its effect on the pulsation periods, thus testing standard and non-standard lepton theory, but the stellar mass must first be known. The pulsation spectrum of PG 0122+200 admits two alternative seismological interpretations, each implying a different mass, luminosity, and distance. Measurement of an accurate distance will resolve the matter once and for all and precisely determine the stellar mass. This project represents the first test of lepton physics in dense {log rho = 6} plasma and is relevant to the many areas of stellar physics in which neutrino interactions are important, including recent theories intended to solve the solar-neutrino problem. 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. ACS/WFC 9860 ESSENCE: Measuring the Dark Energy Equation of State The accelerating universe appears to be dominated by a dark energy with a significant negative pressure. The ratio of the pressure to density of this mysterious energy {its equation of state} is an observable which can differentiate between the proliferating candidate theories. We propose to estimate the dark energy equation of state by observing Type Ia supernovae at redshifts near z=0.7 with HST in concert with the on-going ESSENCE NOAO Survey program that is discovering and studying supernovae between 0.3z0.8. We show that an interesting constraint on the equation of state can be made with supernovae observed at modest redshifts given the current knowledge of the matter density. We will follow 10 Type Ia supernovae discovered from the ground and passed to HST without disrupting its schedule. The full data set will constrain the equation of state to 10% and strictly limit the range of possible dark energy models. In keeping with the ESSENCE policy, these observations will available to the community immediately. ACS/WFC/WFPC2 9825 An ACS/WFC H-alpha Survey of the Orion Nebula We propose to survey nearly 500 square arcminutes of the Orion Nebula in H-alpha using the ACS/WFC, increasing the sky coverage by an order of magnitude over the sum of all previous HST observations. This survey will, for the first time, sample the majority of young stars and circumstellar environments in the extended Trapezium cluster of 2, 000 low-mass stars. Our primary goal is to determine the survival rate and statistical properties of protoplanetary disks in the type of radiation field and dynamical environment in which most stars are born. The survey will be used to search for new silhouette disks, bright proplyds, microjets, large-scale outflows, and to characterize the properties of these objects as a function of location in the nebula. We will determine accurate proper motions in regions where previous HST data exist. However, 90% of our fields will be observed with HST for the first time. This survey will provide the first complete census of pre-main sequence objects and outflows in an HII region and will constrain the extent of hazards to planet formation in such environments. The images will also provide a legacy for future stellar and nebular variability studies and proper motion measurements by providing a first epoch data base. 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 9783 The Ages of Nuclear Star Clusters in Early-type Spiral Galaxies We propose to obtain STIS G430L spectra of the previously identified nuclear star cluster in a sample of 16 spiral galaxies of early to intermediate Hubble type. HST's spatial resolution is required to separate the nuclear cluster from the underlying galaxy bulge. Analysis of the spectra with population synthesis methods will reveal the cluster ages. We will use the age distribution to constrain the duty cycle of nuclear cluster formation. Comparison of the results to those for a larger sample of nuclear clusters in late-type, bulgeless galaxies will allow us to investigate possible differences between the formation mechanisms of nuclear clusters in early and late Hubble types. Such differences might be expected because galaxy bulges show a dichotomy: in late Hubble types, the surface brightness profiles are best described by an exponential, while they follow a de Vaucouleurs law in earlier types. Although the reason for this dichotomy is still unknown, it is plausible that galaxy bulges have different formation mechanisms at the two ends of the Hubble sequence. We know that {1} nuclear cluster formation is linked to the funneling of gas towards the nucleus via gravitational torques from stellar bars, {2} a nuclear mass concentration can make bars unstable, and {3} unstable bars can form bulges. Therefore, the age distribution of nuclear star clusters contains important clues to the evolution of galaxy centers and promises new insight into the origin of the Hubble sequence. ACS/WFC/HRC 9771 The local Hubble flow and the density field within 6 Mpc Great progress has been made recently in accurate distance measurements of nearby galaxies beyond the Local Group based on the luminosity of the tip of the red giant branch {TRGB}. Over the last three years, snapshot surveys with HST have provided us with the TRGB distances for more than a hundred nearby galaxies obtained with an accuracy of about 10%. The local velocity field within 5 Mpc exhibits a significant anisotropy which disagrees with a spherical Virgo-centric flow. The local Hubble flow is very cold, with 1-D rms deviations of ~30 km/s. Cosmological simulations with Cold Dark Matter can only realize such low dispersions with a combination of a low mean density of matter and a substantial component with negative pressure. There may be a constraint on the equation of state w=-p/rho. Our observations will concentrate on 116 galaxies whose expected distances lie within 4 - 6 Mpc, allowing us to trace a Dark Matter distribution in the Local Volume with twice the information currently available. The program is a good one for SNAP mode because the order and rate that the observations are made are not very important, as long as there is good completion over several years. STIS/CCD/MA1 9759 Confirmation of New Candidates for the Study of Intergalactic Helium The reionization of intergalactic helium is believed to take place between redshift 3 and 4. The study of HeII Lyman-alpha absorption in four quasars at 2.7z3.3 demonstrates the great potential of such an intergalactic-medium {IGM} probe and suggests that the reionization epoch is at higher redshifts. Clean quasar sightlines may be found only from massive pre-selection processes in the optical and UV, because of random, severe bsorption by intervening Lyman-limit systems. The SDSS has discovered approximately 36000 quasars, and we propose to verify the UV detectability in 70 top candidates for helium studies extending to even higher redshift. Our proposed approach has already proven successful, and additional positive confirmations will allow follow-up observations, with STIS or COS, to pinpoint the epoch of reionization of the IGM, and the evolution of its properties near that period. ACS/HRC 9747 An Imaging Survey of the Statistical Frequency of Binaries Among Exceptionally-Young Dynamical Families in the Main Asteroid Belt We propose an ambitious SNAPSHOT program to determine the frequency of binaries among two very young asteroid families in the Main Belt, with potentially profound implications. These families {of C- and S-type} have recently been discovered {Nesvorny et al. 2002, Nature 417, 720}, through dynamical modeling, to have been formed at 5.8 MY and 8.3 MY ago in catastrophic impact events. This is the first time such precise and young ages have been assigned to a family. Main-belt binaries are almost certainly produced by collisions, and we would expect a young family to have a significantly higher frequency of binaries than the background, because they may not yet have been destroyed by impact or longer-term gravitational instabilities. In fact, one of the prime observables from such an event should be the propensity for satellites. This is the best way that new numerical models for binary production by collisions {motivated largely by our ground-based discoveries of satellites among larger asteroids}, can be validated and calibrated. HST is the only facility that can be used to search for binaries among such faint objects {V17.5}. We will also measure two control clusters, one being an "old" family, and the other a collection of background asteroids that do not have a family association, and further compare with our determined value for the frequency of large main-belt binaries {2%}. We request visits to 180 targets, using ACS/HRC. 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. NIC2 9726 A NICMOS search for obscured supernovae in starburst galaxies Recent near-IR monitoring campaigns were successful in detecting obscured supernovae {SNe} in starburst galaxies. The inferred SN rate is much higher than that obtained in previous optical campaigns, but it is still significantly lower than expected by the high level star formation of these systems. One possible explanation for the shortage of SNe is that most of them occur in the nuclear region, where the limited angular resolution of groundbased observations prevents their detection. We propose NICMOS SNAP observations of a sample of starburst galaxies already observed once by NICMOS, with the goal of exploiting its sensitivity and angular resolution to detect nuclear obscured SNe which might have been missed by groundbased surveys. These observation will allow to assess the real SN rate in starbust galaxies and deliver a sample of SN occurring in the extreme environment of galactic nuclei. We expect to detect more than 55 SNe {if the whole sample is observed}. If the number of SNe detected in the program is much lower than expected it would prompt for a revision of our understanding of the relation between the star formation rate and the SN rate. 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. 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. ACS/STIS 9451 ACS Imaging and STIS Spectroscopy of Binary Brown Dwarfs We have compiled a sample of 9 spatially resolved binary brown dwarfs {18 objects}, and now propose ACS imaging and STIS spectroscopic follow-up observations. While theoretical models on the interplay of chemical and physical processes governing brown dwarf atmospheres have reached a high level of sophistication, interpretation of observational data remains difficult. As brown dwarfs never stabilize themselves on the hydrogen main sequence, there is always an ambiguity between the temperature or luminosity of any brown dwarf and its mass or age. The individual components of brown dwarf binaries, however, are expected to be coeval and have the same underlying chemical composition. This provides crucial constraints on any model, thus greatly reducing the number of the free parameters. The aim is to obtain photometric and spectroscopic data to probe the physical and chemical properties of the brown dwarf atmospheres, as well as second epoch astrometric data to characterize th e orbital motion. The study will provide important feedback on theoretical model atmospheres and evolutionary tracks for brown dwarfs. As such, it will be an important step towards a better understanding of objects with spectral properties intermediate between those of giant planets and late-type stars. 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/CCD 10085 STIS Pure Parallel Imaging Program: Cycle 12 This is the default archival pure parallel program for STIS during cycle 12. STIS/MA1 10083 HST UV Images of Saturn's Aurora Coordinated with Cassini Solar Wind Measurements A key measurement goal of the Cassini mission to Saturn is to obtain simultaneous solar wind and auroral imaging measurements in a campaign scheduled for Jan. 2004. Cassini will measure the solar wind approaching Saturn continuously from 9 Jan. - 6 Feb., but not closer to Saturn due to competing spacecraft orientation constraints. The only system capable of imaging Saturn's aurora in early 2004 will be HST. In this community DD proposal we request the minimum HST time needed to support the Cassini mission during the solar wind campaign with UV images of Saturn's aurora. Saturn's magnetosphere is intermediate between the "closed" Jovian case with large internal sources of plasma and the Earth's magnetosphere which is open to solar wind interactions. Saturn's aurora has been shown to exhibit large temporal variations in brightness and morphology from Voyager and HST observations. Changes of auroral emitted power exceeding one order of magnitude, dawn brightenings, and latitudinal motions of the main oval have all been observed. Lacking knowledge of solar wind conditions near Saturn, it has not been possible to determine its role in Saturn's auroral processes, nor the mechanisms controlling the auroral precipitation. During Cassini's upcoming approach to Saturn there will be a unique opportunity to answer these questions. We propose to image one complete rotation of Saturn to determine the corotational and longitudinal dependences of the auroral activity. We will then image the active sector of Saturn once every two days for a total coverage of 26 days during the Cassini campaign to measure the upstream solar wind parameters. This is the minimum coverage needed to ensure observations of the aurora under solar wind pressure variations of more than a factor of two, based on the solar wind pressure variations measured by Voyager 2 near Saturn on the declining phase of solar activity. The team of proposers has carried out a similar coordinated observing campaign of Jupiter during the Cassini flyby, resulting in a set of papers and HST images on the cover of Nature on 28 February 2002. WFPC2 10082 POMS Test Proposal: WFII backup parallel archive proposal This is a POMS test proposal designed to simulate scientific plans WFPC2 10076 WFPC2 Cycle 12 CTE Monitor Monitor CTE changes during Cycle 12, including 2X2 binning characterization. WFPC2 10069 WFPC2 CYCLE 12 Supplemental Darks, Part 1/3 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 10059 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 10019 CCD Bias Monitor - Part 1 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 10017 CCD Dark Monitor-Part 1 Monitor the darks for the STIS CCD. NIC3 10014 Spectrophotometry of FAINT IR STANDARDS Faint spectrophotometric standard stars required for COS and the SBC channel on ACS have been established via the STIS FASTEX program that has executed over the last three cycles. Cycle 12 is an especially opportune time to establish companion faint IR standards for WFC3, because the NICMOS proposal 9998 includes observations in cycle 12 of all 6 of the primary standard stars in order to establish the absolute flux calibration of the three grism modes to 1%. In addition to WFC3, these new faint secondary IR standards will be a significant step towards establishing flux standards for JWST, as well as for SNAP, SIRTF, and SOFIA. The 6 primary standards included in Propid=9998 are in the range of V=11-13 and include three hot pure hydrogen WDs and 3 solar analogs. 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. WFPC2/ACS/HRC/WFC 10013 Focus Monitor The focus of HST is measured from WFPC2/PC and ACS/HRC images of stars. Multiple exposures are taken in parallel over an orbit to determine the influence of breathing on the derived mean focus. Observations are taken of clusters with suitable orientations to ensure stars appear in all fields. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) HSTAR 9274: GS Re-acquisition (2,3,2) @ 009/20:23:56Z (during LOS) resulted in FL backup FGS2 due to SSLEX on FGS 3. Following FHST Map scheduled for the time 009/21:22Z showed attitude error of 1.104, 0.632, and 1.595 arcsec. Following GS re-acquisition @ 009/22:03:43Z passed with FL. Under investigation. HSTAR 9275: GS Acquisition (1,2,2) @ 010/04:13:51Z resulted in FL backup FGS 1 due to SSLE on FGS 2. Prior FM Updates @ 010/03:56Z and 03:59Z showed good attitude error vector. Under investigation. HSTAR 9276: GS Acquisition (1,2,2) @ 010/15:24:57Z resulted in FL backup using FGS 1 due to SSLE on FGS 2. Under investigation. HSTAR 9277: FHST FM Update and GS Acquisition Failure @ 011/20:25:43Z and 20:28:28Z failed with Error Box results showing "3 FAILED" for mnemonics QEBSTFG0, QEBSTFG1, and QEBSTFG2. GS Acquisition (1,3,1) failed due to radius limit exceeded on FGS 1. Under investigation. HSTAR 9278: FHST Roll Delay Update failure @ 011/21:59:10Z. Error Box results QEBSTF0, QEBSTFG1, and QEBSTFG2 showed "3 FAILED". Under investigation. COMPLETED OPS REQs: NONE OPS NOTES EXECUTED: NONE SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 28 27 See HSTAR # 9277 FGS REacq 17 17 FHST Update 72 69 See HSTAR # 9277 & 9278 LOSS of LOCK SIGNIFICANT EVENTS: None |
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