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Daily 3627
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3627 PERIOD COVERED: DOYs 156-158 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. ACS/HRC 9987 Coronagraphic search for disks around nearby stars We will use the coronagraphic and imaging modes of the High Resolution camera to study of the role of circumstellar disks in planetary system formation over timescales of ~1-1000 Myr. Our targets comprise pre Main-Sequence {MS} and MS stars, selected by infrared excess, and targets selected from SIRTF surveys. Some targets, like Beta Pictoris have debris disks that have been detected at optical or near-IR wavelengths, while others have disks inferred from mid-IR or ISO observations. We will obtain multicolor images of each target's circumstellar environment for the purpose of {1} detecting and characterizing disk morphologies over all scales {including warps and regions of enhanced or depleted density}, and {2} seeking evidence of embedded planets. Direct and occulted images will be recorded for studying the disks within 2 arcseconds of these targets; the coronagraph will be used to image the outer regions of the disks. Together with existing infrared observations, we will provide constraints on the sizes, distribution, and composition of dust grains. STIS/CCD/MA1 9985 Comets: Gas in the Inner Coma Our target of opportunity program aims at understanding the nucleus-coma interface in comets. Imaging of the near-nucleus region, from both the in situ spacecraft missions to comet Halley in 1986, and more recently with the WFPC2 Planetary Camera, has revealed the structure and evolution of the dust jets associated with active areas on the surface of the nucleus. These dust jets are thought to be driven by the vaporization of the volatiles trapped in the cometary ice. However, the total source inventory of the gaseous component of the coma is not known as there has not been to date direct imaging of a "parent" molecule vaporized directly from the nucleus. In the spectral range of the SBC, the dominant emissions are the Fourth Positive band system of CO and the resonance transitions of its dissociation products carbon and oxygen {oxygen is also produced by the photodissociation of water}. The latter, as dissociation products, are rather extended but the CO emission is concentrated close to the nucleus {McPhate et al. 1999}. Thus, imaging with the SBC using the BaF_2 filter to remove the OI 1304 A will provide a measure of the gas flow leaving the comet's nucleus. In the event of outbursts {often associated with the rotation of active areas into the sunlit hemisphere}, sequential images can provide a direct measure of the gas outflow velocity. The possible presence of a distributed source of CO {such as the purported "CHON" grains invoked to explain the distribution recorded by the Giotto neutral mass spectrometer at Halley} will also be determined. We note that while CO can be detected spectroscopically from the ground at both infrared and millimeter wavelengths, both of these require very high spectral resolving power and the techniques are not suitable for direct imaging of the CO. FGS 9961 The Masses and Luminosities of Population II Stars Very little is currently known concerning the mass-luminosity relation {MLR} of Population II stars. However, with the advent of the Hipparcos Catalogue, improved distances to many spectroscopic binaries known to be Pop II systems are now available. After surveying the literature and making reasonable estimates of the secondary masses, we find 13 systems whose minimum separation should be larger than the resolution limit of FGS1. Because of the expected magnitude differences and separations, it is not possible to resolve the systems from the ground. We therefore propose FGS observations of the sample. In combination with the known spectroscopic orbits and Hipparcos distances, these observations will yield up to 26 precise stellar mass determinations of metal-poor stars, if all systems are resolved and the relative orbits are determined. A combination of FGS data and ground-based observations will lead to component luminosities and effective temperatures. This program will allow for a significantly better understanding of the Pop II main sequence, which in turn will lead to better ages and distances of the galactic globular clusters, and a Pop II MLR will be constructed for the first time. FGS 9879 An Astrometric Calibration of the Cepheid Period-Luminosity Relation We propose to measure the parallaxes of 10 Galactic Cepheid variables. When these parallaxes {with 1-sigma precisions of 10% or better} are added to our recent HST FGS parallax determination of delta Cep {Benedict et al 2002}, we anticipate determining the Period-Luminosity relation zero point with a 0.03 mag precision. In addition to permitting the test of assumptions that enter into other Cepheid distance determination techniques, this calibration will reintroduce Galactic Cepheids as a fundamental step in the extragalactic distance scale ladder. A Period-Luminosity relation derived from solar metallicity Cepheids can be applied directly to extragalactic solar metallicity Cepheids, removing the need to bridge with the Large Magellanic Cloud and its associated metallicity complications. NIC/NIC3 9865 The NICMOS Parallel Observing Program We propose to continue managing the NICMOS pure parallel program. Based on our experience, we are well prepared to make optimal use of the parallel opportunities. The improved sensitivity and efficiency of our observations will substantially increase the number of line-emitting galaxies detected. As our previous work has demonstrated, the most frequently detected line is Halpha at 0.7z1.9, which provides an excellent measure of current star formation rate. We will also detect star-forming and active galaxies in other redshift ranges using other emission lines. The grism observations will produce by far the best available Halpha luminosity functions over the crucial--but poorly observed--redshift range where galaxies appear to have assembled most of their stellar mass. This key process of galaxy evolution needs to be studied with IR data; we found that observations at shorter wavelengths appear to have missed a large fraction of the star-formation in galaxies, due to dust reddening. We will also obtain deep F110W and F160W images, to examine the space densities and morphologies of faint red galaxies. In addition to carrying out the public parallels, we will make the fully reduced and calibrated images and spectra available on-line, with some ground-based data for the deepest parallel fields included. NIC1/NIC2 9844 Brown dwarf atmospheric variability observations We propose to use NIC1 and NIC2 to study brown dwarfs for atmospheric variability. We will observe a sequence of early Ts, a detected variable T2, a T3 and a T4.5. Atmospheric variability, that is expected by some models for these objects, would constrain the physical parameters of cloud vertical distribution, horizontal homogeneity and the dynamics of the very cool atmospheres. The existence and amplitude of the variations would reveal the size and distribution of the cloud cover over the surface of the brown dwarf and test a model explaining the rapidity of the L to T type transition. The relative color changes would constrain the vertical extent of dynamical process and the depth in the atmosphere at which they take place. If a periodicity is measured, the rotational period of the dwarf could be estimated. HST provides the unique and crucial opportunity to observe beyond Earth atmospheric variable absorption, particularly in the important water bands ACS/HRC 9823 Rings of Uranus: Dynamics, Particle Properties and Shepherding Moons We propose to image the rings and small inner satellites of Uranus using the High Resolution Channel of the ACS. The revolutionary capabilities of the ACS will allow us to address a variety of important questions relating to ring properties and ring-moon interactions. Observations at a range of wavelengths and phase angles will reveal the opposition surges of these rings and moons, providing information on color and surface structure. Measurements of the ring in front of the planet will provide complementary information on optical depth; any variations of optical depth with wavelength will reveal the rings' poorly-constrained population of embedded dust. The rings of Uranus are closing rapidly as the planet approaches equinox in 2007, an event that takes place only every 42 years. Using this opportunity, our observations will be repeated at different solar and terrestrial tilt angles; this sequence of images will be particularly valuable for constraining the physical thickness and packing density of the rings. We will place particular emphasis on the rotational variations of the Epsilon Ring, whose radial width {and therefore its packing density} varies by a factor of five. In addition, a set of deep exposures targeted just off the planet will enable us to detect any 4-5 km moons embedded within the ring system. Dynamicists invoke numerous such moons to "shepherd" the many sharp ring boundaries, so this will serve as a definitive test of the theory. ACS/WFC 9788 A Narrow-band Snapshot Survey of Nearby Galaxies We propose to use ACS/WFC to conduct the first comprehensive HST narrow-band {H-alpha + [N II]} imaging survey of the central regions of nearby bulge-dominated disk {S0 to Sbc} galaxies. This survey will cover, at high angular resolution extending over a large field, an unprecedented number of galaxies representing many different environments. It will have important applications for many astrophysical problems of current interest, and it will be an invaluable addition to the HST legacy. The observations will be conducted in snapshot mode, drawing targets from a complete sample of 145 galaxies selected from the Palomar spectroscopic survey of nearby galaxies. Our group will use the data for two primary applications. First, we will search for nuclear emission-line disks suitable for future kinematic measurements with STIS, in order to better constrain the recently discovered relations between black hole mass and bulge properties. Preliminary imaging of the type proposed here must be done, sooner or later, if we are to make progress in this exciting new field. Second, we will investigate a number of issues related to extragalactic star formation. Specifically, we will systematically characterize the properties of H II regions and super star clusters on all galactic scales, from circumnuclear regions to the large-scale disk. 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/HRC/WFC 9781 Galaxy Evolution in Action : The Detailed Morphology of Post-Starburst Galaxy If galaxies evolve morphologically, then some should be in transition between late and early types. One proposed evolutionary mechanism is a galaxy-galaxy merger, but evolved merger products are difficult to find. Fortunately, spectroscopic surveys have now uncovered large numbers of E+A galaxies, a class of objects whose post-starburst spectra, current lack of HI gas, and pressure-supported kinematics suggest that they are the missing panel that connects the "Toomre sequence" of merging spirals with normal ellipticals and S0s. Our first HST observations of five of these galaxies are intriguing. We find a considerable range of tidally disturbed morphologies, an "E+A" fundamental plane, significant differences among the color gradients within 1 kpc {~0.8''}, and populations of bright, blue globular clusters. These initial results are difficult to interpret, however, because they are drawn from a small sample of galaxies whose very blue overall colors may have selected a particular evolutionary path of E+As. Here we propose for ACS imaging of the remaining 15 E+As from the Las Campanas Redshift Survey to probe the full range of E+A properties. The proposed observations will allow us to 1} determine what fraction of the interactions that lead to E+As destroy all disk-like structures {and therefore necessarily lead to elliptical formation}, 2} measure the inner color gradients and constrain the spatial distribution of stars produced as gas sinks to the center during a merger, and 3} determine whether these interactions produce globular clusters in the required numbers to account for the increased specific frequency of clusters in early-type galaxies. STIS/CCD/MA1 9778 Probing Outflowing Winds from the Galactic Center We propose to use two extragalactic sightlines to probe our own Galaxy's "starburst" wind emanating from the Galactic Center. While new infrared imaging and spectroscopy have detected massive stars and very recent {3x10^6 yrs} star formation in the Galactic Center region, only indirect evidence {e.g., radio loops and arcs, bi-conical cavity edges seen in the mid-IR} exists for a wind. However, these winds are routinely detected from starbursts in other galaxies. Far-UV STIS echelle spectroscopy {E140M} of two targets on either side of the Galactic Center at {l, b}={350,-33} and {349, 55} will allow us to map the kinematics of outflowing gas in high ionization species of N V, Si IV and C IV. Similar spectra of distant {1.5-5 kpc}, bright B stars in the same regions of the sky will allow us to remove foreground contaminating components due to the Sco-Cen OB associations. Lower resolution STIS first-order and FUSE spectra show highly redshifted gas in N V and O VI respectively along these sightlines; these new observations will provide three times better spectral resolution {7-10 km/s in the 1185-1580A region} so that the kinematic signature of the outflow can definitely be detected. The foreground stars will allow us to determine whether the outflow is from the Galactic Center or the Sco-Cen OB associations. Absorption line column densities will be used to estimate the outflowing mass and energy by assuming a metallicity and ionizing source for the gas. NIC2 9768 Enabling Coronagraphic Polarimetry with NICMOS We propose to enable a new mode on NICMOS that combines the powerful diffracted light rejection of the coronagraph with the diagnostic power of polarimetry. This new capability will open a new regime in high contrast imaging that has not been possible before. We will enable this capability by observing calibration targets with the coronagraph and the NIC2 polarizers in place. The enabled science includes, but is not limited to, detection and imaging of circumstellar debris in polarized light, the polarized emission surrounding bright planetary nebulae, and the extended structure around bright active galaxies. A similar capability is possible with the ACS, and therefore HST would provide the only platform for this extremely high contrast imaging covering the entire near-UV, optical and near-infrared wavelength regime. 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. ACS 9760 ACS Imaging of the Gemini Deep Deep Survey Fields: Galaxy Assembly at z = 1.5 We are presently carrying out the deepest redshift survey ever undertaken {the Gemini Deep Deep Survey}. Spectra of extraordinary quality have been taken in order to obtain redshifts in the so-called "redshift desert" at 1z2. This redshift range corresponds to the epoch of peak galaxy formation. In this proposal we request 40 orbits of ACS imaging to determine the morphologies of 100-120 candidate early-type galaxies with known redshifts in our survey fields. We seek to determine if these systems are indeed elliptical galaxies and to link their morphological states to their spectroscopically determined ages, recent star-formation histories, and to the evolving global stellar mass function at the peak epoch of galaxy assembly. WFPC2 9710 POMS Test Proposal: WFII backup parallel archive proposal This is a POMS test proposal designed to simulate scientific plans. 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 9708 STIS Pure Parallel Imaging Program: Cycle 11 This is the default archival pure parallel program for STIS during cycle 11. ACS 9674 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 9608 CCD Bias Monitor - Part 2 Monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4, to build up high-S/N superbiases and track the evolution of hot columns. STIS 9606 CCD Dark Monitor-Part 2 Monitor the darks for the STIS CCD. WFPC2 9595 WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt3/3 This dark calibration program obtains 3 dark frames every day to provide data for monitoring and characterizing the evolution of hot pixels. STIS 9507 STIS/UV snapshot survey of bright AGN We propose a UV spectroscopic snapshot survey of bright AGN, quadrupling the number of Seyferts UV spectra and adding dozens of new quasars, aimed at the following goals: begin enumerate em Finding the relationship between the intrinsic luminosity of the AGN and the maximum velocity {and width} of the outflow emanating from it, and determining the frequency of outflows in low-z AGN as a function of luminosity. em Surveying IGM absorption line systems in numerous new sight-lines. em Identifying promising targets for observations with the future highly sensitive Cosmic Origin Spectrograph. end enumerate A 35-minute snapshot with exposures in either the G140L or G230L will yield spectra with a minimum S/N 15 per resolution element at all wavelengths for all our potential targets. This will allow us to be sensitive to absorption lines to a limiting equivalent width of 0.3 Angstrom at the 3 Sigma level. In order to facilitate rapid observational followup, we waive the data proprietary period entirely. ACS 9480 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/MA2 9474 Intriguing Transient Sources in M87 We have found a remarkable number of transient point sources in M87. Within the jet itself we have observed dramatic changes in less than a year. The point sources are seen well in the bluest regions of the spectrum, where we obtain high spatial resolution, are free from cosmic ray artifacts and obtain excellent discrimination against the underlying old, red galaxy. They display a variety of unusual properties: one is brighter than any in the catalogue of novae in M31; several are very close to the jet; another hints at rapid variability. We propose to investigate the population of transient sources in M87 and to probe the intrinsic jet variability on short timescales by taking images in the near UV. Do the sources show nova-type light curves? Is there a decline-rate/luminosity relation? If yes, may we use it for distance estimation, as in Galactic novae, and hence constrain the still very important Virgo distance. Are there very rapidly varying sources, flare stars or gravitational lenses? Is the variable stellar population related to the excess globular cluster frequency in M87? Is there a population of flickering objects in and around the jet, which may be responsive emission arising from their close proximity to a BL Lac nucleus {viewed down the jet axis}? Can we find variability in the jet itself indicative of light week length scales? ACS 9472 A Snapshot Survey for Gravitational Lenses among z = 4.0 Quasars Over the last few years, the Sloan Digital Sky Survey has revolutionized the study of high-redshift quasars by discovering over 200 objects with redshift greater than 4.0, more than doubling the number known in this redshift interval. The sample includes eight of the ten highest redshift quasars known. We propose a snapshot imaging survey of a well-defined sample of 250 z 4.0 quasars in order to find objects which are gravitationally lensed. Lensing models including magnification bias predict that at least 4% of quasars in a flux-limited sample at z 4 will be multiply lensed. Therefore this survey should find of order 10 lensed quasars at high redshift; only one gravitationally lensed quasar is currently known at z 4. This survey will provide by far the best sample to date of high-redshift gravitational lenses. The observed fraction of lenses can put strong constraints on cosmological models, in particular on the cosmological constant Lambda. In addition, magnification bias can significantly bias estimates of the luminosity function of quasars and the evolution thereof; this work will constrain how important an effect this is, and thereby give us a better understanding of the evolution of quasars and black holes at early epochs, as well as constrain models for black hole formation. NICMOS 9360 Paschen-alpha Imaging of a SIRTF-Selected Nearby Galaxy Sample We propose to carry out a NICMOS snapshot survey in the Paschen-alpha {PAlpha} emission line and H-band of the sample of galaxies being observed at 3.5 -- 160 microns as part of SIRTF Nearby Galaxies Survey {SINGS} and a related guaranteed time survey of starburst galaxies. The PAlpha images, accessible only from HST, will be combined with groundbased HAlpha imaging to measure the extinction in the star-forming centers of these galaxies, and obtain robust, extinction- corrected maps of the massive star formation rate {SFR}. The PAlpha data by themselves will provide reliable `extinction- free' SFRs, and a cross-calibration of the {dust--affected} HAlpha-- and UV--based SFRs. The PAlpha--based SFR measurements will extend the SFR-vs.-gas density law {Schmidt--law} to surface densities at least 30 times higher than what is accessible using HAlpha--based SFR measurements alone, bridging the gap between normal galaxies and IR--luminous starbursts. Furthermore, the combination of the HST PAlpha images with the SIRTF images and spectra, as well as ancillary ground--based UBVRIJHK images and GALEX UV images being obtained as part of the SINGS project, will provide a definitive study of the radiative transfer of starlight and dust heating in star--forming galaxies. The processed NICMOS images will be incorporated into the public SINGS Legacy Data Archive, to enable scores of follow-up studies by the astronomical community at large. FGS 9335 Masses of Pre-Main Sequence Binaries We propose to continue to map the orbits of young star binaries in the Taurus and Ophiuchus star forming regions. Our goal is to measure their masses dynamically. This is important because there are still no low mass young stars with reliably known masses so calculations of their evolution to the main sequence are uncalibrated. STIS 9331 Variable Interstellar Absorption toward HD 219188 --- Probing the Structure of an Interstellar Within the last 10 years, strong, narrow Na I absorption has appeared at v_SUN ~ -38 km s^-1 toward the halo star HD 219188; that absorption has continued to strengthen, by a factor 2--3, over the past three years. The line of sight appears to be moving into/through a relatively cold, quiescent intermediate velocity {IV} cloud, due to the 13 mas/year proper motion of HD 219188. We propose to monitor the continuing changes in the IV absorption toward HD 219188 over the next three years with STIS echelle spectra --- making use of the rich diagnostics provided by the UV lines of various neutral and singly ionized species to determine abundances/depletions and physical conditions {temperature, density, ionization} as functions of depth within the cloud. In addition to providing a unique view of the detailed structure of an interstellar cloud, these data will yield constraints on grain scattering parameters {from the variation of ionization with depth} and on any dependence of depletion on local density. GTO/ACS 9291 Formation of High Redshift Radio Galaxies This programme uses ACS observations of high redshift radio galaxies {HzRGs} to investigate massive galaxy and cluster formation in the early Universe. By carrying out deep observations of a few z 3.8 targets the following four questions will be studied: {1} Are HzRGs massive central-cluster galaxies formed through hierarchical assembly of Lyman break galaxies? Detailed brightness distributions colors and morphologies of HzRG clumps will be measured and compared with those of Lyman break galaxies. {2} Are HzRGs located in dense {proto-} clusters and if so what are the properties of the associated large-scale structures? Lyman alpha excesses, colors and morphologies of objects in field will be used to search for companion galaxies of HzRGs. {3} What are the origin and fate of giant gas halos associated with HzRGs and what role do they play in the formation of massive galaxies? The morphologies and locations of Ly-alpha clumps will be compared with those of continuum clumps. {4} Is nuclear activity a source of star formation in the early Universe? The properties of continuum and Ly-alpha clumps along will be compared in relation to the radio jet. NIC1/NIC2/NIC3 8792 NICMOS Post-SAA calibration - CR Persistence Part 3 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. 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/MA1 10341 The D/H Ratio in C/2002 T7 {LINEAR} Measuring the D/H ratio in comets is one of the most important scientific objectives in planetary science. A comparison of the D/H ratio in comets to the value measured in the Earth's oceans can be used to assess whether cometary impacts contributed significantly to the delivery of water and other volatiles to the Earth. A comparison of the cometary ratio with the value in other solar system reservoirs {e.g., in the solar wind and the atmospheres of the Giant Planets}, and to values observed in the interstellar medium, can be used to determine how primitive cometary matter is. Our recent detection of the deuterium Lyman-alpha line in C/2001 Q4 {NEAT} demonstrates that HST has a new and potentially important role to play in this exciting area of research. Fortuitously, another moderately bright comet, C/2002 T7 {LINEAR}, is well-placed for HST observations in early June, and we request 8 orbits of HST time to measure deuterium in this comet. If our observations are successful, the number of comets for which D/H has been measured will be nearly doubled. 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/WFC 10268 Recovery of three faint Kuiper Belt Objects discovered with HST We propose 6 orbits to make ACS/WFC follow-up observations of three faint Kuiper Belt Objects {KBOs} that we discovered in the Large Cycle 11 program GO 9433 {G. Bernstein, PI; Bernstein et al. 2004}. These KBOs are the faintest -- and therefore smallest -- KBOs known. Two of these objects can be recovered {and the third easily recovered and its colors probed} only with HST. Any future studies of small KBOs will require knowledge of our three faint KBOs. With the proposed observations, the locations of these KBOs will be known quite well until after first light for JWST. Without the proposed observations, these three small KBOs will be effectively lost. This small program represents a small investment of HST time to solidify the legacy of the Bernstein et al. Large GO program. With the proposed observations, we will be able to determine with certainty the dynamical classes of these three KBOs, testing the hypothesis that small KBOs are predominantly classical KBOs. We will also test the suggestion that classical KBOs are uniformly quite red. Lastly, our observations will enable physical studies {e.g., spectroscopy} with JWST a decade from now. All these measurements will provide important evidence for theories on the formation and evolution of the Solar System. WFPC2 10073 Earth Flats This proposal monitors flatfield stability. This proposal obtains sequences of Earth streak flats to construct high quality flat fields for the WFPC2 filter set. These flat fields will allow mapping of the OTA illumination pattern and will be used in conjuction with previous internal and external flats to generate new pipeline superflats. These Earth flats will complement the Earth flat data obtained during cycles 4-11. 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. ACS/HRC/WFC 10060 CCD Daily Monitor This program consists of basic tests to monitor, the read noise, the development of hot pixels and test for any source of noise in ACS CCD detectors. This programme will be executed once a day for the entire lifetime of ACS. ACS/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 coronographic monitoring is required to assess the changing position of the spots. 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 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. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) HSTAR 9442: At AOS, GS Acquisition (1,3,1) @156/15:45:40Z resulted in FL backup on FGS 3 due to SSLE on FGS 1. Preceding FHST FM Updates showed very low errors and the following FHST Map was not able to be generated due to LOS. Under investigation. HSTAR 9443: GS acquisition (3,2,3) @ 157/10:59:30Z required multiple attempts to reach FL backup due to SRLE on FGS 3. ESB message AOChex was observed indicating Coarse Mode Angle Check fail. Prior FHST FM Updates @ 157/10:00:08Z and 10:02:53Z showed good attitude error vector. FHST Map @ 157/11:12:19Z showed 3-axis (RSS) error value ~ 18.00 arcsec. Subsequent GS Reacquisition (3,2,3) @ 157/12:13:33Z resulted in FL backup. Under investigation. COMPLETED OPS REQs: 17172-0 Battery 4 Capacity Test @ 156/1435z 17186-0 GENSLEW for prop 10341, slot 13 @ 156/2041z 17187-0 GENSLEW for prop 10341, slot 14 @ 156/2043z 17188-0 GENSLEW for prop 10341, slot 1 @ 156/2044z 17189-0 GENSLEW for prop 10341, slot 2 @ 156/2045z 17190-0 GENSLEW for prop 10341, slot 3 @ 156/2047z 17191-0 GENSLEW for prop 10341, slot 4 @ 156/2048z 17192-0 GENSLEW for prop 10341, slot 5 @ 156/2050z 17193-0 GENSLEW for prop 10431, slot 6 @ 156/2051z OPS NOTES EXECUTED: 0900-1 COMMAND PROBLEM @ 158/0922z 0900-1 COMMAND PROBLEM @ 158/1759z 0916-0 Tabulation of Slew Attitude Error (Miss-distance) @ 159/0043z SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 34 34 FGS REacq 11 11 FHST Update 60 60 LOSS of LOCK SIGNIFICANT EVENTS: Successfully performed on-orbit Target Reacquisition test 156/14:14Z - 16:30Z. All activities were conducted via the SMS, no real-time commanding was involved. The test was monitored and the proper sequence of events was seen in the FGS quaternions, as expected and as could be observed, given the real-time contacts. Successfully returned Battery 4 to FSW 6-battery system and restored EPS subsystem to its nominal on-orbit configuration @ 156/14:24Z. RMGA routinely scheduled power cycle (ON/OFF) scheduled 159/12:10Z - 13:10Z to provide lubrication to the gyro bearings (OR 17185 with attached ROP PO-07). |
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