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Daily 3451
HUBBLE SPACE TELESCOPE
DAILY REPORT # 3451 PERIOD COVERED: DOYs 261-264 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. ACS/HRC 9976 The Parallaxes and Proper Motions of Two Nearby Neutron Stars We propose to measure the parallax of two nearby neutron stars to the highest possible level of accuracy, ~.0.5 mas. The primary goal is to determine the neutron-star radius at infinity with better than 1 km precision, and therewith obtain a direct constraint on the equation of state of matter at supra-nuclear density. The required flux and temperature determinations are easiest for the so-called isolated or radio-quiet neutron stars because of their apparently completely thermal spectrum. We argue that the importance of the possible results warrants a study to the best possible level of the best possible sources, and request 24 orbits for the two brightest isolated neutron stars, RX J1856.5-3754 and RX J0720.4-3125. We will also determine whether the enigmatic RX J0720.4-3125 is an old magnetar or an accreting source, based on its luminosity and proper motion. STIS/ACS/HRC 9975 Ozone, Condensates, and Dust in the Martian Atmosphere We propose to utilize the unique UV capabilities of STIS and ACS/HRC in order to study the spatial and seasonal variations in ozone, condensates, and dust in the Martian atmosphere. The data obtained will be critical in addressing recent breakthroughs in understanding the basic radiative, transport, and microphysical processes that provide for both long-term and short-term balance within the global Mars climate system. The proposal includes both Cycle 11 & 12 observations in order to span the classic dust storm season on Mars and provide the first good opportunity for HST to observe a dusty atmosphere on the planet. The UV observations will complement visible and IR observations that will be made during the Mars Global Surveyor Extended Mission and will provide support for the future UV observations of MARCI on the 2005 Mars Reconnaissance Orbiter. STIS 9973 Intensive Coverage of the Eta Carinae Event in 2003 For a variety of reasons, HST can provide a very special and unique data set when Eta Car experiences its next spectroscopic event in mid-2003. Explaining the phenomenon is only part of the motivation. This star and its ejecta have unique characteristics that make them important for several branches of astrophysics; and when a spectroscopic event occurs, it's like varying the parameters in an experiment {or rather, set of experiments}. The 2003 event may be the only chance in the forseeable future to obtain such a data set, especially with HST. Eta Carinae has extreme parameters; it is mysterious in surprisingly basic ways; and HST/STIS can gather useful data on it at a terrific rate. As we explain below, the proposed data set will be valuable in several independent ways: It will help solve a specific set of current problems, it will constitute a large and unique archival data base for both stellar and nebular astrophysics, and it will be well-suited for educational uses. 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/WFC/HRC 9895 The Role of Groups in the Evolution of Galaxies at Intermediate Redshifts Groups are the most common environment experienced by galaxies, yet they remain the least studied. The tidal fields and dynamical friction encountered by galaxies in groups probably holds the key to understanding the role of environment in driving the evolution of galaxies since z ~ 1. To study the evolution of galaxies in the group environment, we propose the first unbiased HST study of groups at moderate redshifts. Unlike previous HST group samples, that relied on radio or X-ray properties, our kinematically selected sample is drawn from a large redshift survey and is not biased towards unusually dense groups. HST imaging is essential to determine the morphology of galaxies in these systems and contrast this with the properties of galaxies in denser and more evolved groups and rich clusters at these epochs. HST data are also required to adequately compare the properties of groups at intermediate redshifts with local group samples derived from the 2df and Sloan surveys. We will combine the HST images with deep ground-based observations to study how morphologies and stellar populations of galaxies in groups have evolved in time. These observations are key to understanding the decline in the volume averaged star formation rate in the universe. STIS/CCD/MA1 9894 UV Spectroscopic Observations of Luminous Narrow-line Seyfert 1 Galaxies Narrow-line Seyfert 1 galaxies {NLS1s} have remarkably different properties than Active Galactic Nuclei with broad optical lines. The most promising explanation for this behavior is that NLS1s have a higher accretion rate relative to Eddington {L/M} than do broad-line Seyferts. Despite uniformity in optical line properties, detailed analysis reveals a divergence of the UV emission line properties that can be traced differences in the shape of the continuum. A link with similarly divergent X-ray properties suggests that there may be variations in L/M even among NLS1s. To test this scenario, we propose UV spectroscopic of two X-ray extreme NLS1s. These observations offer the opportunity to advance our understanding in the scatter in the relationship between line width and black hole mass, to understand physics of gas in AGN optical and UV emission-line regions, and to understand recently-discovered peculiar line-less high-z quasars that may be the early universe counterpart of luminous NLS1s. ACS/WFC 9891 A snapshot survey of rich stellar clusters in the Large and Small Magellanic Clouds Rich stellar clusters are vital to a wide variety of astrophysical research, from stellar evolution studies to the formation and evolution of galaxies. In this context, it is important to understand how rich star clusters form and evolve. The cluster systems in the LMC and SMC are particularly important in achieving this, because they are the only systems which contain clusters at all stages of evolution while being close enough to be studied as fully resolved stellar populations - although in general this requires the capabilities of HST. We have recently investigated the structural evolution of LMC and SMC clusters using archival WFPC2 data, and demonstrated a dramatic trend in the sizes of these clusters with age. We have shown that this trend likely represents genuine structural evolution in these clusters, although it is not clear whether we are observing a dynamical process or the signature of changing formation conditions. This result has implications for all astronomical research involving massive stellar clusters. To develop this work further requires the extension of our two samples, so that they are statistically quantifiable. This will allow a number of key questions regarding the structural evolution trend to be answered. We propose a two-colour ACS/WFC SNAP survey of rich Magellanic Cloud clusters to achieve this aim. The unique resolution and sensitivity of ACS/WFC is required for success, because of the crowded nature of the targets. The SNAP data will have a large number of additional applications, both to globular cluster and Magellanic Cloud research. STIS/CCD/MA2 9886 Boron in F Stars in the Hyades - Insights into the Li-Be Dip Dramatic deficiencies of Li in the mid-F stars of the Hyades were discovered by Boesgaard and Tripicco in 1986. Using ultraviolet, high-resolution spectra from the Keck 10-m telescope, Boesgaard and King have just discovered the corresponding deficiencies in Be in the same narrow temperature region in the Hyades. We propose a precision investigation into the B abundance in the Hyades F stars to ascertain if there is a B dip. Boron can only be observed with HST and we plan to use the resonance line of B I at 2497A. Each of these three light elements is destroyed inside stars, but each has a different threshold temperatu 2.5 x 10^6, 3.5 x 10^6, and 5 x 10^6 K for Li, Be, and B respectively. Consequently, these elements survive to increasingly greater depths in a star and their surface abundances act as a report on the depth and thoroughness of mixing in the star. The mixing mechanism in F stars is slow mixing, but not straight convective mixing. These observations will help determine the nature of the mixing mechanism{s}, and the connection to stellar rotation. The abundance of *all three* light elements in a cluster ofknown age and metallicity provides the necessary information to discern the internal stellar processes. This mixing must be occurring in other stars of this mass range {~10-25% more massive than the sun} and can best be studied in a cluster of stars of common origin and known characteristics. The Hyades cluster at 7 x 10^8 yr is close enough to contain stars bright enough for this investigation. NIC2 9875 The Fundamental Plane of Massive Gas-Rich Mergers We propose deep NICMOS H-band imaging of a carefully selected sample of 33 luminous, late-stage galactic mergers. This program is part of a comprehensive investigation of the most luminous mergers in the nearby universe, the ultraluminous infrared galaxies {ULIGs}. The high-resolution HST images will complement an extensive set of ground-based data that include long-slit NIR spectra from a recently approved Large VLT Programme. This unique dataset will allow us to derive with unprecedented precision structural -and- kinematic parameters for a large unbiased sample of objects spanning the entire ULIG luminosity function. These data will refine the fundamental plane of massive gas-rich mergers and enable us to answer the following questions: {1} Do ultraluminous mergers form elliptical galaxies, and in particular, giant ellipticals? {2} Do ULIGs evolve into optically bright QSOs? The results from this detailed study of massive mergers in the local universe will be relevant to understanding galaxy formation and evolution at earlier epochs, and in particular, the dusty sub-mm population that accounts for more than half of the star formation at z 1. 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/HRC 9853 A Search for Young Binary Brown Dwarfs: Constraining Formation Scenarios and Masses Through Multiplicity We propose to use the Advanced Camera for Surveys / High Resolution Camera to conduct a direct imaging multiplicity survey of 34 young brown dwarfs in the nearest regions of recent star formation, the T association Taurus-Auriga and the OB association Upper Scorpius. The determined multiplicity fraction, the separation distribution, and the mass ratio distribution will offer stringent observational constraints on proposed brown dwarf formation scenarios. Moreover, the small semi-major axes of known field and open cluster brown dwarf binaries suggest the exciting possibility of our identifying several very close binaries { 15 AU}. Continued monitoring of these systems would yield, on a decade timescale, the first dynamical mass estimates of T Tauri brown dwarfs. With masses intermediate between those of stars and planets, brown dwarfs offer our best hope of relating the reasonably well understood processes of star formation to the less well understood processes of planet formation. ACS/WFC 9847 The Structure and Physics of Extragalactic Jets As part of an ongoing investigation into the physics of jets, we propose to obtain ACS polarimetry of the jets of 3C 15, 3C 66B, 3C 346, 3C 371 and PKS 0521-36. This builds on our earlier HST work and completes a sample of 9 jets that spans the range of jet luminosities and morphological types. All of these jets have deep, multi-band HST imaging, and radio polarimetry at matching resolution, and all but one has Chandra data. Our goal is to investigate three fundamental issues, brought to light by recent HST and Chandra observations. These a {1} What is the energetic and magnetic field structure of jets? {2} What is the nature of particle acceleration in jets? {3} What is the nature of the X-ray emission from jets, and what is its relationship to lower energy emissions? Optical polarimetry provides unique information about all of these issues. Because of their vastly different radiative lifetimes {hundreds of years compared to millions}, optical and radio polarimetry probe different electron populations and emission regions. Comparison of radio and optical polarimetry can therefore yield direct information about the three-dimensional energetic and magnetic field structure of jets. Optical polarimetry traces the magnetic field configuration in and near electron acceleration regions, and when combined with optical and X-ray spectral index maps, polarimetry can yield key constraints about particle acceleration and the nature of the X-ray emission of jets. ACS/WFC 9842 A Snapshot Search for Halo Very-Low-Mass Binaries We propose a snapshot search for binary M subdwarf stars. These nearby stars have high velocities and low metallicies that identify them as members of the old Galactic halo {Population II}. ACS imaging is requested to search for secondary companions. This supplements a previous snapshot program that only obtained 10 observations. The observed binary fraction will be compared to the disk M dwarf fraction to look for differences in star formation. It is likely that a system suitable for orbital mass determinations will be found. In this case, future HST observations could determine the first masses for very-low-mass, low-metallicity stars. NIC2 9834 Finding Planets in the Stellar Graveyard: A Faint Companion Search of White Dwarfs with NICMOS We propose to do a deep search for substellar objects in orbit around white dwarfs with the newly refurbished NICMOS camera as part of the PI's doctoral thesis work. Direct imaging of planets around main sequence stars is difficult due to the large contrast ratio, a problem which is much less severe for companions to white dwarfs. White dwarfs are not usually considered in planet searches but recent theoretical work and observations are motivating new searches for planetary systems and dust disks around DAZ white dwarfs. We propose to conduct the search with the NIC2 coronagraph to find resolved companions and do photometry to search for unresolved companions through Near-IR excesses. We estimate that the survey will be sensitive to brown dwarfs, high mass jovian planets, and dust disks. By probing a wide range of orbital separations and companion masses, this survey will help to answer questions about the brown dwarf desert, common envelope evolution, and planet formation. HST and NICMOS provide a unique capability to do this search, as no ground based observatory with AO can adequately search for faint companions as close and with such high contrast. NIC2 9801 Are OH/IR Stars the Youngest post-AGB stars? A NICMOS Imaging Survey Essentially all well-characterized preplanetary nebulae {PPNe}-- objects in transition between the AGB and planetary nebula evolutionary phases - are bipolar, whereas the mass-loss envelopes of AGB stars are strikingly spherical. In order to understand the processes leading to bipolar mass-ejection, we need to know at what stage of stellar evolution does bipolarity in the mass-loss first manifest itself. We have recently hypothesized that most OH/IR stars {evolved mass- losing stars with OH maser emission} are very young PPNe. We are conducting a multiwavelength survey program of imaging and spectroscopic observations of such objects, using a large, morphologically unbiased sample selected using IRAS 12-to-25 micron colors. Our ongoing HST/SNAP imaging survey of the optically bright half of this sample with WFPC2 and ACS is highly successful: 19/32 objects observed are extended with bipolar/multipolar shapes {remaining objects are unresolved}. Slightly more than 50% of our sample are optically too faint or undetected but have strong near-IR counterparts -- we therefore propose a NICMOS SNAPshot imaging survey of these optically-faint OH/IR stars. These observations are crucial for determining how and when the bipolar geometry asserts itself. The results from our NICMOS survey {together with the WFPC2/ACS survey} will allow us to draw general conclusions about the onset of bipolar mass-ejection during late stellar evolution. Our complementary program of interferometric mapping of the OH maser emission in our sources is yielding kinematic information with spatial resolution comparable to that in the HST images. The HST/radio data will provide crucial input for theories of post-AGB stellar evolution. In addition, these data will also indicate whether the multiple concentric rings, "searchlight beams'', and truncated equatorial disks recently discovered with HST in a few PPNe, are common or rare phenomena. STIS/MA1 9790 Separating Activity and Accretion in T Tauri Stars Due to their unique evolutionary state, the naked {non-accreting} T Tauri stars {NTTS} are the only real proxies for what the underlying magnetically active star of a classical TTS {CTTS} system looks like. Comparative analysis then allows us to separate stellar properties from accretion properties in CTTS. In addition, the late-type NTTS are excellent candidates for studying rotation-activity relationships in fully convective stars and probing the properties of turbulent dynamos. With the limited data currently available, NTTS appear to be very magnetically active stars with higher than expected H-alpha/X-ray flux ratios but lower transition region fluxes relative to other active stars. However, the data are very incomplete. We will use HST-STIS observations of transition region line fluxes on 11 fully convective NTTS to establish the level and structure of dynamo generated emission in these young stars. In principal, these far ultraviolet emission lines are sensitive diagnostics of mass accretion onto CTTS, since accretion shocks on the stellar surface should produce substantial emission measure at 10^5 - 10^6 K. However, it is imperative that we first understand the emissions from NTTS before we can use these lines to study accretion onto CTTS. 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 9782 Measuring Black Hole Masses in Double Peaked Broad Lined AGNs To date there have been few black hole {BH} mass estimates for luminous broad line AGN, including those derived from reverberation mapping. In this context, objects with "double-peaked" broad lines are particularly important because the line emission is believed to arise in a relativistically rotating accretion disk. If this model is correct, then the BH mass can be determined directly from periodic variations in the line-profile shape. In two cases {Arp 102B and NGC 1097} such variations have been claimed. The goal of this proposal is to confront the relativistic disk model for the double-peaked Balmer lines with independent limits on the central masses for 5 of the nearest and brightest "double-peaked emitters" {NGC 1097, Arp 102B, Pictor A, 3C390.3, 3C332}, determined by using STIS long-slit spectroscopy to map the velocity field of circum-nuclear ionized gas. These observations will critically test the idea that the line emission in these objects comes from an accretion disk and thus provide unique insights into the physical processes operating in both the BLR and the "central engine". 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. ACS 9675 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/CAL 9628 MAMA Sensitivity and Focus Monitor Cycle 11 Monitor sensitivity of each MAMA grating mode to detect any change due to contamination or other causes. Also monitor the STIS focus in a spectroscopic and imaging mode. 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 9455 Mid-Ultraviolet Spectral Templates for Old Stellar Systems We propose a three-year program to provide both observational and theoretical mid-ultraviolet {2300A -- 3100A} spectral templates for interpreting the age and metallicity of globular clusters and elliptical galaxies from spectra of their integrated light. The mid-UV is the region most directly influenced by stellar age, and is observed directly in optical and infrared studies of high-redshift quiescent systems. The reliability of age and metallicity determinations remains questionable until non-solar metallicities and abundance ratios are considered, and stars spanning the color-magnitude diagram are included, as we propose here. With archival HST STIS spectra we have improved the list of mid-UV atomic line parameters, then calculated spectra from first principles which match observed spectra of standard stars up to one- fourth solar metallicity. We will extend both observations and calculations to stars of solar metallicity and beyond, and to those in short-lived stages hotter than the main-sequence turnoff, stars not currently well-represented in empirical libraries. The necessary line-list improvements will come from new high-resolution mid-UV spectra of nine field stars. A key application of the results of this program will be to the old systems now being discovered as `Extremely Red Objects' at high redshifts. Reliable age-dating of these places constraints on the epoch when large structures first formed in the universe. 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. NIC1/NIC2/NIC3 8792 NICMOS Post-SAA calibration - CR Persistence Part 3 A new proceedure proposed to alleviate the CR-persistence problem of NICMOS. Dark frames will be obtained immediately upon exiting the SAA contour 23, and everytime 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 i mages. Each observation will need its own CRMAP, as different SAA passages leave different imprints on the NICMOS detectors. WFPC2 10082 POMS Test Proposal: WFII backup parallel archive proposal This is a POMS test proposal designed to simulate scientific plans ACS/WFC 10056 Extreme Red Stars ACS provides unprecedented sensitivity in the far red, this coupled with recent astronomical pushes to ever cooler objects {e.g. new classifications for L and T stellar dwarfs, and extremely high redshift galaxies} increases the need for extending the photometric calibration to include such objects. We propose observations of 2 stellar objects for which STIS spectra will exist, as well as NICMOS grism. The two targets include a late M dwarf and a T dwarf. The M dwarf provides a temporal check with WFC and new constraint for the HRC. The T dwarf provides new results for the WFC. STIS/CCD 10000 STIS Pure Parallel Imaging Program: Cycle 12 This is the default archival pure parallel program for STIS during cycle 12. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) HSTAR 9155: GS Acquisition (3,1,1) @ 263/14:54:15Z failed to Gyro hold due to SRLE on FGS 1. Under investigation. COMPLETED OPS REQs: None OPS NOTES EXECUTED: 1158-2 Adjust NICMOS Error Count Limit @ 263/15:30z SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 60 58 (see HSTAR 9155) FGS REacq 60 60 FHST Update 114 114 LOSS of LOCK SIGNIFICANT EVENTS: Aft Flight Deck Telemetry testing scheduled 265/11:00Z - 20:00Z with GDOC, SOC, HITT, and CCS using CCS "B" String with CCS Release 4.0.3 and PRD S07200. The purpose of this testing is to verify SM-4 telemetry applicable to Aft Flight Deck, HITT, and SOC procedures and scenario files. Battery Capacity Test: Battery 1 returned to FSW 6-Battery system @ 261/10:10Z (OR 17035-1). Additionally, the +D SPA was unmasked in FSW and the Benchmark SOC and SOC 1 safing limits were reset to their 6-battery operational values of 330 A-h and 235 A-h, respectively. During the following 2 orbits, EPS SE confirmed the system was operating nominally in SWCC with the OCA enabled. Trickle charge was entered ~ 37 minutes into orbit day at the 330 A-h Benchmark and the +D SPA opened as expected. Capacity values will be updated when the merged data becomes available. Completed CCS Release 5.0.3 Event Analyzer Monitor and Compare testing 259/260/11:00Z - 17:00Z using CCS D, F, and C strings on Day 259 and CCS D and C strings on Day 261. CCS Release 5.0.3 events compared nominally against CCS Release 4.0.3 events. The test was configured with both real-time and simulated data and submitted to several HST telemetry scenarios. A few Event Analyzer Tool functions were exercised. |
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