HUBBLE SPACE TELESCOPE<br /><br /><br />DAILY REPORT # 3528<br /><br /><br />PERIOD COVERED: DOYs 9-11/2004<br /><br /><br />OBSERVATIONS SCHEDULED<br /><br /><br />ACS 9984<br /><br /><br />Cosmic Shear With ACS Pure Parallels<br /><br /><br />Small distortions in the shapes of background galaxies by foreground mass<br />provide a powerful method of directly measuring the amount and distribution of<br />dark matter. Several groups have recently detected this weak lensing by<br />large-scale structure, also called cosmic shear. The high resolution and<br />sensitivity of HST/ACS provide a unique opportunity to measure cosmic shear<br />accurately on small scales. Using 260 parallel orbits in Sloan textiti {F775W}<br />we will measure for the first time: beginlistosetlength sep0cm setlengthemsep0cm<br />setlength opsep0cm em the cosmic shear variance on scales <0.7 arcmin, em the<br />skewness of the shear distribution, and em the magnification effect. endlist Our<br />measurements will determine the amplitude of the mass power spectrum<br />sigma_8Omega_m^0.5, with signal-to-noise {s/n} ~ 20, and the mass density<br />Omega_m with s/n=4. They will be done at small angular scales where non-linear<br />effects dominate the power spectrum, providing a test of the gravitational<br />instability paradigm for structure formation. Measurements on these scales are<br />not possible from the ground, because of the systematic effects induced by PSF<br />smearing from seeing. Having many independent lines of sight reduces the<br />uncertainty due to cosmic variance, making parallel observations ideal.<br /><br /><br />STIS/CCD 9981<br /><br /><br />The Ultra Deep Field - STIS parallels<br /><br /><br />We propose to obtain slitless spectroscopy of objects in the GEMS and GOODS area<br />around the UDF.<br /><br /><br />WFPC2 9980<br /><br /><br />The Ultra Deep Field - WFPC2 Parallels<br /><br /><br />The ACS Ultra Deep Field {UDF} is a survey carried out by using Director's<br />Discretionary time. The main science drivers are galaxy evolution and cosmology.<br />The primary instrument is the Advanced Camera for Surveys but WFPC2, NICMOS, and<br />STIS will also be used in pure parallel mode. The data will be made public. The<br />UDF consists of a single ultra-deep field {410 orbits in total} within the CDF-S<br />GOODS area. We request a modification of the default pure parallel programs.<br />Rather than duplicate the redder bands which will be done much better with ACS,<br />we propose to observe in the near-ultraviolet F300W filter. These data will<br />enable study of the rest-frame ultraviolet morphology of galaxies at 0<z<1,<br />allowing determination of the morphological k-correction and the location of<br />star formation within galaxies, using a sample that is likely to be nearly<br />complete with multi-wavelength photometry and spectroscopic redshifts. The<br />results can be used to interpret observations of higher redshift galaxies by<br />ACS.<br /><br /><br />NIC3 9979<br /><br /><br />The Ultra Deep Field - NICMOS Parallels<br /><br /><br />This is a plan to manage the NICMOS pure parallels of the ACS Ultra Deep Survey.<br />We will obtain a mix of F110W and F160W images along sight-lines within the<br />mosaiced ACS fields of the CDF-S GOODS and GEMS surveys, with these sight-lines<br />enabling an examination of the space density and morphologies of the reddest<br />galaxies.<br /><br /><br />ACS/CCD/WFC 9978<br /><br /><br />The Ultra Deep Field with ACS<br /><br /><br />The ACS Ultra Deep Field {UDF} is a survey carried out by using Director's<br />Discretionary time. The main science driver are galaxy evolution and cosmology.<br />The primary instrument is the Advanced Camera for Surveys but WFPC2 and NICMOS<br />will also be used in parallel. The data will be made public. The UDF consists of<br />a single ultra-deep field {410 orbits in total} within the CDF-S GOODS area. The<br />survey will use four filters: F435W {55 orbits}, F606W {55 orbits}, F775W {150<br />orbits}, and F850LP {150 orbits}. The F435W {B} and F606W {V} exposures will be<br />one magnitude deeper than the equivalent HDF filters. The F775W {I} exposure<br />will be 1.5 magnitude deeper than the equivalent HDF exposure. The depth in<br />F775W and F850LP is optimized for searching very red objects - like z=6 galaxies<br />- at the detection limit of the F850LP image. The pointing will be RA{J2000}=3<br />32 40.0 and Decl.{J2000}=-27 48 00. These coordinates may change slightly due to<br />guide star availability and implementation issues. We will attempt to include in<br />the field both a spectroscopically confirmed z=5.8 galaxy and a<br />spectroscopically confirmed type Ia SN at z=1.3. The pointing avoids the gaps<br />with the lowest effective exposure on the Chandra ACIS image of CDFS. This basic<br />structure of the survey represents a consensus recommendation of a Scientific<br />Advisory Committee to the STScI Director Steven Beckwith. A local Working Group<br />is looking in detail at the implementation of the survey.<br /><br /><br />FGS 9969<br /><br /><br />FGS Astrometry of the Extrasolar Planet of Epsilon Eridani<br /><br /><br />We propose observations with HST/FGS in Position Mode to determine the<br />astrometric elements {perturbation orbit semimajor axis and inclination} of the<br />candidate extra-solar planet around the K2 V star Epsilon Eridani that has been<br />detected by Doppler spectroscopy. These observations will also permit us to<br />determine the actual mass of the planet by providing the sin{i} factor which can<br />not be determined with the radial velocity method. High precision radial<br />velocity {RV} measurements spanning the years 1980.8--2000.0 for the nearby<br />{3.22 pc} star Epsilon Eri show convincing variations with a period of ~ 7 yrs.<br />These data represent a combination of six independent data sets taken with four<br />different telescopes. A least squares orbital solution using robust estimation<br />yields orbital parameters of period, P = 6.9 yrs, velocity K- amplitude = 19<br />m/s, eccentricity e = 0.6, projected companion mass M_B sin{i} = 0.83 M_Jupiter.<br />An estimate of the inclination yields a perturbation semi-major axis, Alpha =<br />0arcs0022, easily within the reach of HST/FGS astrometry.<br /><br /><br />ACS/HRC/WFC 9919<br /><br /><br />The Morphological, Photometric, and Spectroscopic Properties of Intermediate<br />Redshift Cluster Galaxies:<br /><br /><br />New and fundamental constraints on the evolutionary state of high redshift<br />clusters will be made by obtaining deep, multiband images {SDSS r, i, z} over<br />the central 1.5 Mpc regions of seven distant clusters in the range 0.76 < z <<br />1.27. The ACS data will allow us to {1} definitively establish the morphological<br />composition and star formation rates as functions of clustercentric radius,<br />local density, x-ray luminosity {obtained from accompanying Chandra, and XMM<br />data}, {2} explore the relationship between substructure, kinematics, and<br />morphology, {3} strongly constrain the galaxy merger frequency and the origins<br />of elliptical and S0 galaxies, {4} measure the mass distribution independently<br />from the light {via gravitational lensing} enabling comparisons with<br />kinematically derived masses, and {5} study the evolution of the structure of<br />the brightest cluster members. The clusters selected for this program already<br />have extensive spectroscopic observations and NIR imaging is either in hand or<br />underway from approved ground based programs. To date, the lower part of this<br />redshift range has only been marginally studied with HST. Our sample includes<br />the two most distant, spectroscopically confirmed superclusters and will<br />significantly increase the baseline over which evolutionary effects can be<br />studied. The data will also be used to identify very high-z galaxies via their<br />unique spectral properties.<br /><br /><br />FGS 9882<br /><br /><br />The Distance and Mass of the Neutrino-Luminous White Dwarf PG 0122+200<br /><br /><br />PG 0122+200 is a pulsating hot white dwarf that is believed to radiate more<br />energy as neutrinos than it does as photons. We propose to measure with FGS the<br />trigonometric parallax of PG 0122+200 and thereby determine its distance,<br />luminosity, and mass. Ongoing investigations from the ground will infer the<br />neutrino luminosity through its effect on the pulsation periods, thus testing<br />standard and non-standard lepton theory, but the stellar mass must first be<br />known. The pulsation spectrum of PG 0122+200 admits two alternative<br />seismological interpretations, each implying a different mass, luminosity, and<br />distance. Measurement of an accurate distance will resolve the matter once and<br />for all and precisely determine the stellar mass. This project represents the<br />first test of lepton physics in dense {log rho = 6} plasma and is relevant to<br />the many areas of stellar physics in which neutrino interactions are important,<br />including recent theories intended to solve the solar-neutrino problem.<br /><br /><br />NIC/NIC3 9865<br /><br /><br />The NICMOS Parallel Observing Program<br /><br /><br />We propose to continue managing the NICMOS pure parallel program. Based on our<br />experience, we are well prepared to make optimal use of the parallel<br />opportunities. The improved sensitivity and efficiency of our observations will<br />substantially increase the number of line-emitting galaxies detected. As our<br />previous work has demonstrated, the most frequently detected line is Halpha at<br />0.7<z<1.9, which provides an excellent measure of current star formation rate.<br />We will also detect star-forming and active galaxies in other redshift ranges<br />using other emission lines. The grism observations will produce by far the best<br />available Halpha luminosity functions over the crucial--but poorly<br />observed--redshift range where galaxies appear to have assembled most of their<br />stellar mass. This key process of galaxy evolution needs to be studied with IR<br />data; we found that observations at shorter wavelengths appear to have missed a<br />large fraction of the star-formation in galaxies, due to dust reddening. We will<br />also obtain deep F110W and F160W images, to examine the space densities and<br />morphologies of faint red galaxies. In addition to carrying out the public<br />parallels, we will make the fully reduced and calibrated images and spectra<br />available on-line, with some ground-based data for the deepest parallel fields<br />included.<br /><br /><br />ACS/WFC 9860<br /><br /><br />ESSENCE: Measuring the Dark Energy Equation of State<br /><br /><br />The accelerating universe appears to be dominated by a dark energy with a<br />significant negative pressure. The ratio of the pressure to density of this<br />mysterious energy {its equation of state} is an observable which can<br />differentiate between the proliferating candidate theories. We propose to<br />estimate the dark energy equation of state by observing Type Ia supernovae at<br />redshifts near z=0.7 with HST in concert with the on-going ESSENCE NOAO Survey<br />program that is discovering and studying supernovae between 0.3<z<0.8. We show<br />that an interesting constraint on the equation of state can be made with<br />supernovae observed at modest redshifts given the current knowledge of the<br />matter density. We will follow 10 Type Ia supernovae discovered from the ground<br />and passed to HST without disrupting its schedule. The full data set will<br />constrain the equation of state to 10% and strictly limit the range of possible<br />dark energy models. In keeping with the ESSENCE policy, these observations will<br />available to the community immediately.<br /><br /><br />ACS/WFC/WFPC2 9825<br /><br /><br />An ACS/WFC H-alpha Survey of the Orion Nebula<br /><br /><br />We propose to survey nearly 500 square arcminutes of the Orion Nebula in H-alpha<br />using the ACS/WFC, increasing the sky coverage by an order of magnitude over the<br />sum of all previous HST observations. This survey will, for the first time,<br />sample the majority of young stars and circumstellar environments in the<br />extended Trapezium cluster of 2, 000 low-mass stars. Our primary goal is to<br />determine the survival rate and statistical properties of protoplanetary disks<br />in the type of radiation field and dynamical environment in which most stars are<br />born. The survey will be used to search for new silhouette disks, bright<br />proplyds, microjets, large-scale outflows, and to characterize the properties of<br />these objects as a function of location in the nebula. We will determine<br />accurate proper motions in regions where previous HST data exist. However, 90%<br />of our fields will be observed with HST for the first time. This survey will<br />provide the first complete census of pre-main sequence objects and outflows in<br />an HII region and will constrain the extent of hazards to planet formation in<br />such environments. The images will also provide a legacy for future stellar and<br />nebular variability studies and proper motion measurements by providing a first<br />epoch data base.<br /><br /><br />STIS 9786<br /><br /><br />The Next Generation Spectral Library<br /><br /><br />We propose to continue the Cycle 10 snapshot program to produce a Next<br />Generation Spectral Library of 600 stars for use in modeling the integrated<br />light of galaxies and clusters. This program is using the low dispersion UV and<br />optical gratings of STIS. The library will be roughly equally divided among four<br />metallicities, very low {[Fe/H] lt -1.5}, low {[Fe/H] -1.5 to -0.5}, near-solar<br />{[Fe/H] -0.3 to 0.1}, and super-solar {[Fe/H] gt 0.2}, well-sampling the entire<br />HR-diagram in each bin. Such a library will surpass all extant compilations and<br />have lasting archival value, well into the Next Generation Space Telescope era.<br />Because of the universal utility and community-broad nature of this venture, we<br />waive the entire proprietary period.<br /><br /><br />STIS 9783<br /><br /><br />The Ages of Nuclear Star Clusters in Early-type Spiral Galaxies<br /><br /><br />We propose to obtain STIS G430L spectra of the previously identified nuclear<br />star cluster in a sample of 16 spiral galaxies of early to intermediate Hubble<br />type. HST's spatial resolution is required to separate the nuclear cluster from<br />the underlying galaxy bulge. Analysis of the spectra with population synthesis<br />methods will reveal the cluster ages. We will use the age distribution to<br />constrain the duty cycle of nuclear cluster formation. Comparison of the results<br />to those for a larger sample of nuclear clusters in late-type, bulgeless<br />galaxies will allow us to investigate possible differences between the formation<br />mechanisms of nuclear clusters in early and late Hubble types. Such differences<br />might be expected because galaxy bulges show a dichotomy: in late Hubble types,<br />the surface brightness profiles are best described by an exponential, while they<br />follow a de Vaucouleurs law in earlier types. Although the reason for this<br />dichotomy is still unknown, it is plausible that galaxy bulges have different<br />formation mechanisms at the two ends of the Hubble sequence. We know that {1}<br />nuclear cluster formation is linked to the funneling of gas towards the nucleus<br />via gravitational torques from stellar bars, {2} a nuclear mass concentration<br />can make bars unstable, and {3} unstable bars can form bulges. Therefore, the<br />age distribution of nuclear star clusters contains important clues to the<br />evolution of galaxy centers and promises new insight into the origin of the<br />Hubble sequence.<br /><br /><br />ACS/WFC/HRC 9771<br /><br /><br />The local Hubble flow and the density field within 6 Mpc<br /><br /><br />Great progress has been made recently in accurate distance measurements of<br />nearby galaxies beyond the Local Group based on the luminosity of the tip of the<br />red giant branch {TRGB}. Over the last three years, snapshot surveys with HST<br />have provided us with the TRGB distances for more than a hundred nearby galaxies<br />obtained with an accuracy of about 10%. The local velocity field within 5 Mpc<br />exhibits a significant anisotropy which disagrees with a spherical Virgo-centric<br />flow. The local Hubble flow is very cold, with 1-D rms deviations of ~30 km/s.<br />Cosmological simulations with Cold Dark Matter can only realize such low<br />dispersions with a combination of a low mean density of matter and a substantial<br />component with negative pressure. There may be a constraint on the equation of<br />state w=-p/rho. Our observations will concentrate on 116 galaxies whose expected<br />distances lie within 4 - 6 Mpc, allowing us to trace a Dark Matter distribution<br />in the Local Volume with twice the information currently available. The program<br />is a good one for SNAP mode because the order and rate that the observations are<br />made are not very important, as long as there is good completion over several<br />years.<br /><br /><br />STIS/CCD/MA1 9759<br /><br /><br />Confirmation of New Candidates for the Study of Intergalactic Helium<br /><br /><br />The reionization of intergalactic helium is believed to take place between<br />redshift 3 and 4. The study of HeII Lyman-alpha absorption in four quasars at<br />2.7<z<3.3 demonstrates the great potential of such an intergalactic-medium {IGM}<br />probe and suggests that the reionization epoch is at higher redshifts. Clean<br />quasar sightlines may be found only from massive pre-selection processes in the<br />optical and UV, because of random, severe absorption by intervening Lyman-limit<br />systems. The SDSS has discovered approximately 36000 quasars, and we propose to<br />verify the UV detectability in 70 top candidates for helium studies extending to<br />even higher redshift. Our proposed approach has already proven successful, and<br />additional positive confirmations will allow follow-up observations, with STIS<br />or COS, to pinpoint the epoch of reionization of the IGM, and the evolution of<br />its properties near that period.<br /><br /><br />ACS/HRC 9747<br /><br /><br />An Imaging Survey of the Statistical Frequency of Binaries Among<br />Exceptionally-Young Dynamical Families in the Main Asteroid Belt<br /><br /><br />We propose an ambitious SNAPSHOT program to determine the frequency of binaries<br />among two very young asteroid families in the Main Belt, with potentially<br />profound implications. These families {of C- and S-type} have recently been<br />discovered {Nesvorny et al. 2002, Nature 417, 720}, through dynamical modeling,<br />to have been formed at 5.8 MY and 8.3 MY ago in catastrophic impact events. This<br />is the first time such precise and young ages have been assigned to a family.<br />Main-belt binaries are almost certainly produced by collisions, and we would<br />expect a young family to have a significantly higher frequency of binaries than<br />the background, because they may not yet have been destroyed by impact or<br />longer-term gravitational instabilities. In fact, one of the prime observables<br />from such an event should be the propensity for satellites. This is the best way<br />that new numerical models for binary production by collisions {motivated largely<br />by our ground-based discoveries of satellites among larger asteroids}, can be<br />validated and calibrated. HST is the only facility that can be used to search<br />for binaries among such faint objects {V>17.5}. We will also measure two control<br />clusters, one being an "old" family, and the other a collection of background<br />asteroids that do not have a family association, and further compare with our<br />determined value for the frequency of large main-belt binaries {2%}. We request<br />visits to 180 targets, using ACS/HRC.<br /><br /><br />ACS/WFC 9744<br /><br /><br />HST Imaging of Gravitational Lenses<br /><br /><br />Gravitational lenses offer unique opportunities to study cosmology, dark matter,<br />galactic structure, galaxy evolution and quasar host galaxies. They are also the<br />only sample of galaxies selected based on their mass rather than their<br />luminosity or surface brightness. While gravitational lenses can be discovered<br />with ground-based optical and radio observations, converting them into<br />astrophysical tools requires HST. HST has demonstrated that it is the only<br />telescope that can in each case precisely locate the lens galaxy, measure its<br />luminosity, color and structure, and search for lensed images of the source host<br />galaxy given the typical image separations of ~1''. We will obtain ACS/WFC V and<br />I images and NICMOS H images of 21 new lenses never observed by HST and NICMOS H<br />images of 16 lenses never observed by HST in the IR. As in previous cycles, we<br />request that the data be made public immediately.<br /><br /><br />NIC2 9726<br /><br /><br />A NICMOS search for obscured supernovae in starburst galaxies<br /><br /><br />Recent near-IR monitoring campaigns were successful in detecting obscured<br />supernovae {SNe} in starburst galaxies. The inferred SN rate is much higher than<br />that obtained in previous optical campaigns, but it is still significantly lower<br />than expected by the high level star formation of these systems. One possible<br />explanation for the shortage of SNe is that most of them occur in the nuclear<br />region, where the limited angular resolution of groundbased observations<br />prevents their detection. We propose NICMOS SNAP observations of a sample of<br />starburst galaxies already observed once by NICMOS, with the goal of exploiting<br />its sensitivity and angular resolution to detect nuclear obscured SNe which<br />might have been missed by groundbased surveys. These observation will allow to<br />assess the real SN rate in starbust galaxies and deliver a sample of SN<br />occurring in the extreme environment of galactic nuclei. We expect to detect<br />more than 55 SNe {if the whole sample is observed}. If the number of SNe<br />detected in the program is much lower than expected it would prompt for a<br />revision of our understanding of the relation between the star formation rate<br />and the SN rate.<br /><br /><br />WFPC2 9709<br /><br /><br />POMS Test Proposal: WFII parallel archive proposal<br /><br /><br />This is the generic target version of the WFPC2 Archival Pure Parallel program.<br />The program will be used to take parallel images of random areas of the sky,<br />following the recommendations of the 2002 Parallels Working Group.<br /><br /><br />STIS 9633<br /><br /><br />STIS parallel archive proposal - Nearby Galaxies - Imaging and Spectroscopy<br /><br /><br />Using parallel opportunities with STIS which were not allocated by the TAC, we<br />propose to obtain deep STIS imagery with both the Clear {50CCD} and Long-Pass<br />{F28X50LP} filters in order to make color-magnitude diagrams and luminosity<br />functions for nearby galaxies. For local group galaxies, we also include G750L<br />slitless spectroscopy to search for e.g., Carbon stars, late M giants and S-type<br />stars. This survey will be useful to study the star formation histories,<br />chemical evolution, and distances to these galaxies. These data will be placed<br />immediately into the Hubble Data Archive.<br /><br /><br />ACS/STIS 9451<br /><br /><br />ACS Imaging and STIS Spectroscopy of Binary Brown Dwarfs<br /><br /><br />We have compiled a sample of 9 spatially resolved binary brown dwarfs {18<br />objects}, and now propose ACS imaging and STIS spectroscopic follow-up<br />observations. While theoretical models on the interplay of chemical and physical<br />processes governing brown dwarf atmospheres have reached a high level of<br />sophistication, interpretation of observational data remains difficult. As brown<br />dwarfs never stabilize themselves on the hydrogen main sequence, there is always<br />an ambiguity between the temperature or luminosity of any brown dwarf and its<br />mass or age. The individual components of brown dwarf binaries, however, are<br />expected to be coeval and have the same underlying chemical composition. This<br />provides crucial constraints on any model, thus greatly reducing the number of<br />the free parameters. The aim is to obtain photometric and spectroscopic data to<br />probe the physical and chemical properties of the brown dwarf atmospheres, as<br />well as second epoch astrometric data to characterize th e orbital motion. The<br />study will provide important feedback on theoretical model atmospheres and<br />evolutionary tracks for brown dwarfs. As such, it will be an important step<br />towards a better understanding of objects with spectral properties intermediate<br />between those of giant planets and late-type stars.<br /><br /><br />NICMOS 8791<br /><br /><br />NICMOS Post-SAA calibration - CR Persistence Part 2<br /><br /><br />A new procedure proposed to alleviate the CR-persistence problem of NICMOS. Dark<br />frames will be obtained immediately upon exiting the SAA contour 23, and every<br />time a NICMOS exposure is scheduled within 50 minutes of coming out of the SAA.<br />The darks will be obtained in parallel in all three NICMOS Cameras. The POST-SAA<br />darks will be non-standard reference files available to users with a USEAFTER<br />date/time mark. The keyword 'USEAFTER=date/time' will also be added to the<br />header of each POST-SAA DARK frame. The keyword must be populated with the time,<br />in addition to the date, because HST crosses the SAA ~8 times per day so each<br />POST-SAA DARK will need to have the appropriate time specified, for users to<br />identify the ones they need. Both the raw and processed images will be archived<br />as POST-SAA DARKSs. Generally we expect that all NICMOS science/calibration<br />observations started within 50 minutes of leaving an SAA will need such maps to<br />remove the CR persistence from the science images. Each observation will need<br />its own CRMAP, as different SAA passages leave different imprints on the NICMOS<br />detectors.<br /><br /><br />STIS/CCD 10085<br /><br /><br />STIS Pure Parallel Imaging Program: Cycle 12<br /><br /><br />This is the default archival pure parallel program for STIS during cycle 12.<br /><br /><br />STIS/MA1 10083<br /><br /><br />HST UV Images of Saturn's Aurora Coordinated with Cassini Solar Wind<br />Measurements<br /><br /><br />A key measurement goal of the Cassini mission to Saturn is to obtain<br />simultaneous solar wind and auroral imaging measurements in a campaign scheduled<br />for Jan. 2004. Cassini will measure the solar wind approaching Saturn<br />continuously from 9 Jan. - 6 Feb., but not closer to Saturn due to competing<br />spacecraft orientation constraints. The only system capable of imaging Saturn's<br />aurora in early 2004 will be HST. In this community DD proposal we request the<br />minimum HST time needed to support the Cassini mission during the solar wind<br />campaign with UV images of Saturn's aurora. Saturn's magnetosphere is<br />intermediate between the "closed" Jovian case with large internal sources of<br />plasma and the Earth's magnetosphere which is open to solar wind interactions.<br />Saturn's aurora has been shown to exhibit large temporal variations in<br />brightness and morphology from Voyager and HST observations. Changes of auroral<br />emitted power exceeding one order of magnitude, dawn brightenings, and<br />latitudinal motions of the main oval have all been observed. Lacking knowledge<br />of solar wind conditions near Saturn, it has not been possible to determine its<br />role in Saturn's auroral processes, nor the mechanisms controlling the auroral<br />precipitation. During Cassini's upcoming approach to Saturn there will be a<br />unique opportunity to answer these questions. We propose to image one complete<br />rotation of Saturn to determine the corotational and longitudinal dependences of<br />the auroral activity. We will then image the active sector of Saturn once every<br />two days for a total coverage of 26 days during the Cassini campaign to measure<br />the upstream solar wind parameters. This is the minimum coverage needed to<br />ensure observations of the aurora under solar wind pressure variations of more<br />than a factor of two, based on the solar wind pressure variations measured by<br />Voyager 2 near Saturn on the declining phase of solar activity. The team of<br />proposers has carried out a similar coordinated observing campaign of Jupiter<br />during the Cassini flyby, resulting in a set of papers and HST images on the<br />cover of Nature on 28 February 2002.<br /><br /><br />WFPC2 10082<br /><br /><br />POMS Test Proposal: WFII backup parallel archive proposal<br /><br /><br />This is a POMS test proposal designed to simulate scientific plans<br /><br /><br />WFPC2 10076<br /><br /><br />WFPC2 Cycle 12 CTE Monitor<br /><br /><br />Monitor CTE changes during Cycle 12, including 2X2 binning characterization.<br /><br /><br />WFPC2 10069<br /><br /><br />WFPC2 CYCLE 12 Supplemental Darks, Part 1/3<br /><br /><br />This dark calibration program obtains 3 dark frames every day to provide data<br />for monitoring and characterizing the evolution of hot pixels.<br /><br /><br />ACS/HRC/WFC 10059<br /><br /><br />CCD Daily Monitor<br /><br /><br />This program consists of basic tests to monitor, the read noise, the development<br />of hot pixels and test for any source of noise in ACS CCD detectors. This<br />programme will be executed once a day for the entire lifetime of ACS.<br /><br /><br />STIS/CCD 10019<br /><br /><br />CCD Bias Monitor - Part 1<br /><br /><br />Monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1<br />at gain = 4, to build up high-S/N superbiases and track the evolution of hot<br />columns.<br /><br /><br />STIS/CCD 10017<br /><br /><br />CCD Dark Monitor-Part 1<br /><br /><br />Monitor the darks for the STIS CCD.<br /><br /><br />NIC3 10014<br /><br /><br />Spectrophotometry of FAINT IR STANDARDS<br /><br /><br />Faint spectrophotometric standard stars required for COS and the SBC channel on<br />ACS have been established via the STIS FASTEX program that has executed over the<br />last three cycles. Cycle 12 is an especially opportune time to establish<br />companion faint IR standards for WFC3, because the NICMOS proposal 9998 includes<br />observations in cycle 12 of all 6 of the primary standard stars in order to<br />establish the absolute flux calibration of the three grism modes to 1%. In<br />addition to WFC3, these new faint secondary IR standards will be a significant<br />step towards establishing flux standards for JWST, as well as for SNAP, SIRTF,<br />and SOFIA. The 6 primary standards included in Propid=9998 are in the range of<br />V=11-13 and include three hot pure hydrogen WDs and 3 solar analogs. We propose<br />to establish new IR faint standards in the 15-17 mag range. Appropriate spectral<br />types for faint IR standards are solar analogs and hotter WDs. Many M type and<br />cooler stars are variable, so that long term monitoring is required before<br />committing HST time to such cool stars. A few G type and WD faint stars will<br />provide a set of faint IR standards with minimal sky and color coverage.<br />Existing HST images of any candidates can provide verification that there are no<br />contaminating stars above the 1% level within 2-3arcsec. However, the ACS<br />calibration field in 47 Tuc is too crowded for linking to ground based<br />observations. If the other candidates are selected from SDSS or other ground<br />based data, then the NICMOS and STIS acquisition images can provide this<br />verification, as well as correction factors for arbitrary photometric size<br />apertures. The SNAP team is providing the northern faint stars using unreleased<br />SDSS data. In addition, the extreme coolest types such as L and T stars have<br />proven essential to sorting out the long wavelength QE of ACS; both the ACS and<br />eventually WFC3 calibrations could be improved with knowledge of L and T SEDs in<br />the region beyond 0.95 microns. In addition to the primary purpose of ACS QE vs.<br />wavelength and broad band F814W and F850LP calibrations, these three stars in<br />C.} below are at the flux level required for WFC3 grism calibration. The<br />brighter M, L, and T standard stars will each require a NICMOS orbit, while each<br />faint standard requires two Nicmos orbits and one STIS orbit for complete<br />wavelength coverage. The STIS spectra of the M and L stars are done as ACS<br />calibrations in cycles 12 and 11, respectively. An additional faint WD has<br />already been proposed for 2 Nicmos and 4 STIS orbits in their cycle 12 programs<br />already. See Table 1 for a summary of the 18 orbit allocation for this program<br />10014. Bright stars in the V=0-6 mag range would be useful for direct<br />comparisons to NIST calibrated lamps. This comparison would offer the<br />opportunity to compare two fundamentally different realms of physics: pure<br />hydrogen stellar models and laboratory black body physics. Unfortunately, the<br />Nicmos bright limit is V=~8 for a solar analog and a 1s exposure without<br />defocussing the OTA. The primary Sloan standard BD+17d4708 at V=9.9 is safely<br />fainter than this Nicmos limit.<br /><br /><br />WFPC2/ACS/HRC/WFC 10013<br /><br /><br />Focus Monitor<br /><br /><br />The focus of HST is measured from WFPC2/PC and ACS/HRC images of stars. Multiple<br />exposures are taken in parallel over an orbit to determine the influence of<br />breathing on the derived mean focus. Observations are taken of clusters with<br />suitable orientations to ensure stars appear in all fields.<br /><br /><br />FLIGHT OPERATIONS SUMMARY:<br /><br /><br />Significant Spacecraft Anomalies: [The following are preliminary reports of<br />potential non-nominal performance that will be investigated.)<br /><br /><br />HSTAR 9274: GS Re-acquisition [2,3,2) @ 009/20:23:56Z [during LOS) resulted in FL<br /> backup FGS2 due to SSLEX on FGS 3. Following FHST Map scheduled for<br /> the time 009/21:22Z showed attitude error of 1.104, 0.632, and 1.595<br /> arcsec. Following GS re-acquisition @ 009/22:03:43Z passed with FL.<br /> Under investigation.<br /><br /><br />HSTAR 9275: GS Acquisition [1,2,2) @ 010/04:13:51Z resulted in FL backup FGS 1 due<br /> to SSLE on FGS 2. Prior FM Updates @ 010/03:56Z and 03:59Z showed good<br /> attitude error vector. Under investigation.<br /><br /><br />HSTAR 9276: GS Acquisition [1,2,2) @ 010/15:24:57Z resulted in FL backup using FGS<br /> 1 due to SSLE on FGS 2. Under investigation.<br /><br /><br />HSTAR 9277: FHST FM Update and GS Acquisition Failure @ 011/20:25:43Z and 20:28:28Z<br /> failed with Error Box results showing "3 FAILED" for mnemonics QEBSTFG0,<br /> QEBSTFG1, and QEBSTFG2. GS Acquisition [1,3,1) failed due to radius<br /> limit exceeded on FGS 1. Under investigation.<br /><br /><br />HSTAR 9278: FHST Roll Delay Update failure @ 011/21:59:10Z. Error Box results QEBSTF0,<br /> QEBSTFG1, and QEBSTFG2 showed "3 FAILED". Under investigation.<br /><br /><br />COMPLETED OPS REQs: NONE<br /><br /><br />OPS NOTES EXECUTED: NONE<br /><br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 28 27 See HSTAR # 9277<br />FGS REacq 17 17<br />FHST Update 72 69 See HSTAR # 9277 & 9278<br />LOSS of LOCK<br /><br /><br />SIGNIFICANT EVENTS: None