HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3161<br /><br />PERIOD COVERED: DOYs 200 - 202<br /><br />OBSERVATIONS SCHEDULED [see HSTARS below for possible observation problems]<br /><br />NICMOS 9325<br /><br />Photometric Stability<br /><br />This NICMOS post-SMOV3b early calibration proposal carries out photometric<br />monitoring observations after SMOV3b, nominally spanning the approximate time<br />frame April-August 2002.<br /><br />ACS 9472<br /><br />A Snapshot Survey for Gravitational Lenses among z >= 4.0 Quasars<br /><br />Over the last few years, the Sloan Digital Sky Survey has revolutionized the<br />study of high-redshift quasars by discovering over 200 objects with redshift<br />greater than 4.0, more than doubling the number known in this redshift interval.<br />The sample includes eight of the ten highest redshift quasars known. We propose<br />a snapshot imaging survey of a well-defined sample of 250 z > 4.0 quasars in<br />order to find objects which are gravitationally lensed. Lensing models including<br />magnification bias predict that at least 4% of quasars in a flux-limited sample<br />at z > 4 will be multiply lensed. Therefore this survey should find of order 10<br />lensed quasars at high redshift; only one gravitationally lensed quasar is<br />currently known at z > 4. This survey will provide by far the best sample to<br />date of high-redshift gravitational lenses. The observed fraction of lenses can<br />put strong constraints on cosmological models, in particular on the cosmological<br />constant Lambda. In addition, magnification bias can significantly bias<br />estimates of the luminosity function of quasars and the evolution thereof; this<br />work will constrain how important an effect this is, and thereby give us a<br />better understanding of the evolution of quasars and black holes at early<br />epochs, as well as constrain models for black hole formation.<br /><br />ACS 9468<br /><br />ACS Grism Parallel Survey of Emission- line Galaxies at Redshift z pl 7<br /><br />We propose an ACS grism parallel survey to search for emission-line galaxies<br />toward 50 random lines of sight over the redshift interval 0 < zpl 7. We<br />request ACS parallel observations of duration more than one orbit at high<br />galactic latitude to identify ~ 300 HAlpha emission-line galaxies at 0.2pl zpl<br />0.5, ~ 720 O IILambda3727 emission-line galaxies at 0.3pl zpl 1.68, and pg<br />1000 Ly-alpha emission-line galaxies at 3pl zpl 7 with total emission line<br />flux fpg 2* 10^-17 ergs s^-1 cm^-2 over 578 arcmin^2. We will obtain direct<br />images with the F814W and F606W filters and dispersed images with the WFC/G800L<br />grism at each position. The direct images will serve to provide a zeroth order<br />model both for wavelength calibration of the extracted 1D spectra and for<br />determining extraction apertures of the corresponding dispersed images. The<br />primary scientific objectives are as follows: {1} We will establish a uniform<br />sample of HAlpha and O II emission-line galaxies at z<1.7 in order to obtain<br />accurate measurements of co-moving star formation rate density versus redshift<br />over this redshift range. {2} We will study the spatial and statistical<br />distribution of star formation rate intensity in individual galaxies using the<br />spatially resolved emission-line morphology in the grism images. And {3} we will<br />study high-redshift universe using Ly-alpha emitting galaxies identified at z<br />pl 7 in the survey. The data will be available to the community immediately as<br />they are obtained.<br /><br />ACS 9480<br /><br />Cosmic Shear With ACS Pure Parallels<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 />ACS 9502<br /><br />Evolution of the Tully-Fisher Relation of Field Spiral Galaxies<br /><br />We seek imaging of the FORS deep field {FDF} with the ACS to determine<br />morphological and structural parameters of a complete sample of 80 late-type<br />galaxies brighter than R_ lim=23^m {corresponding to ~ M_B^*+2 at z=0.5}<br />selected there. We already obtained spectra and derived velocity curves of these<br />galaxies using the ESO VLT. Only combined with the ACS HST observations this<br />will allow us to establish the Tully- Fisher relation between luminosity and<br />rotation of spirals at a mean redshift of 0.5 and therefore measure the<br />luminosity and mass evolution of spiral and irregular galaxies within about half<br />of the age of the Universe, strongly constraining current theories of galaxy<br />formation and evolution. Several other important scientific projects based on<br />the FDF, such as a study of the Fundamental Plane of field elliptical galaxies<br />at <z> ~ 0.3, a study of the size and type evolution of high-z galaxies {up to<br />z~5} and a study of galaxy-galaxy lensing will also benefit from these<br />observations.<br /><br />ACS 9399<br /><br />Insights into Elliptical Galaxy Formation from HST Imaging of Shell Galaxies<br /><br />We propose to use ACS to carry out an imaging survey of the cores of shell<br />galaxies. Key to understanding several aspects of shell formation is to<br />determine how far in do shells exist. Photometric detection from the ground is<br />limited by seeing and sampling to radii of at best R ~ 10 - 15 arcsec. In<br />velocity maps derived from high spatial resolution long-slit and integral-field<br />ground-based spectra we have found shell-like features with distinct kinematics<br />in several shell galaxy cores {R ~ 3 - 5 arcsec ~ 1 kpc}. Hence we believe that<br />shells may extend further in than previously known. HST provides the spatial<br />resolution and sampling needed to map out shells in the pronounced surface<br />brightness gradients of elliptical galaxy cores. The data will allow us to<br />detect and map inner shells, to measure their colors, to establish their<br />dynamics with the help of ground-based kinematics, to compare the inner surface<br />brightness profiles of shell and non-shell ellipticals, and to measure the mass<br />and distribution of the dust. Where shells are found, combined spatial and<br />velocity information will establish the orbital structure of shell- producing<br />merger debris on the basis of data, and will allow useful checks of the models<br />for formation of shell systems in early-type galaxies.<br /><br />ACS 9395<br /><br />Is Bulge Formation Still Going-On? An ACS Survey of Pseudo-Bulges<br /><br />Pseudo-bulges, i.e., bulges with an exponential light profile, have been<br />unveiled in the centers of many intermediate-type disks. Their structural<br />similarity with the disks provides support to theoretical scenarios in which<br />bulges may form due to secular evolution processes within the host disks. If at<br />play, these processes would likely be active throughout a large fraction of<br />cosmic history down to our days: `young' bulges should exist. Our previous HST<br />WFPC2 and NICMOS survey of ~100 spirals has provided V-H colors for 11 Sb-Sc<br />pseudo-bulges, and these could be interpreted as suggestive of relatively young<br />stellar ages. Furthermore, dense nuclei have been discovered in these<br />pseudo-bulges, and their V-H colors may imply stellar masses sufficiently large<br />to activate the formation of the pseudo- bulge by means of dynamical dissolution<br />of progenitor bars. However, the V-H color, on its own, is fully degenerate<br />towards stellar ages, metallicities and masses, as well as dust content. We<br />therefore propose to use ACS to observe the 11 pseudo-bulges of our combined<br />WFPC2 and NICMOS sample in the F330W, F435W, and F814W filters. Extending the<br />wavelength baseline to the bluer passbands is essential to break the<br />mass-age-metallicity-dust degeneracy, and will provide far more accurate<br />estimates for the stellar population properties of the pseudo-bulges and their<br />nuclei. Proving the existence of `young' bulges in the local Universe would have<br />a big impact in our understanding of the formation of the Hubble sequence.<br /><br />ACS 9567<br /><br />SBC Dark Current<br /><br />Dark current measurements will be made for the ACS SBC once a week.<br /><br />ACS 9454<br /><br />The Nature of the UV Continuum in LINERs: A Variability Test<br /><br />LINERs may be the most common AGNs, and the signposts of accretion onto the<br />massive black holes present in most galaxies. However, the LINER spectrum is the<br />result of UV excitation, and, in at least some LINERs, a nuclear cluster of hot<br />stars, rather than an AGN, dominates the energetics in the UV. Thus, it is still<br />unknown if the UV continuum, or the optical emission lines it excites, have<br />anything to do with an AGN. The demographics and accretion physics of<br />low-luminosity AGNs hinge on this question. We propose to search for variability<br />in a sample of 17 LINERs with compact UV nuclei. Variability can reveal an AGN<br />component in the UV continuum, even when its light is not dominant. We will test<br />systematically the handful of non-definitive reports of UV variability, and<br />potentially quantify the AGN contribution to the UV emission. Variability in all<br />or most objects will be strong evidence that LINERs mark dormant AGNs in most<br />galaxies. Alternatively, a general null detection of variability will suggest<br />that, even in LINERs with additional AGN signatures, the UV continuum is stellar<br />in origin. Contemporaneous monitoring with the VLA/VLBA of 11 objects which have<br />radio cores {five of which we already know are radio-variable} will reveal the<br />relations between UV and radio variations. The UV-variable objects will be<br />targeted for future, better-sampled, monitoring.<br /><br />ACS/CAL 9558<br /><br />ACS weekly Test<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 />ACS/HRC 9012<br /><br />HRC Coronagraph Acquisition.<br /><br />The Advanced Camera for Surveys [HRC] was used to verify the abilities of the<br />flight and ground software to perform isolated point-source acquisition onto the<br />coronagraph occulting spots and the Fastie Finger. Successful execution of these<br />acquisitions will also demonstrate the ability of the software to calculate the<br />centroid of the target positions and to perform automated telescope pointing.<br /><br />ACS/HRC 9379<br /><br />Near Ultraviolet Imaging of Seyfert Galaxies: Understanding the Starburst-AGN<br />Connection<br /><br />We propose a near-UV snapshot survey of 101 Seyfert galaxies using ACS/HRC and<br />the filter F330W, a configuration which is optimal to detect faint star forming<br />regions around their nuclei. These images will complement optical and near-IR<br />images available in the HST archive, thus providing a panchromatic atlas of the<br />inner regions of active galaxies, which we will use to study the starburst-AGN<br />connection. The main goals of this proposal are: {1} Determine the frequency of<br />circumnuclear starbursts in Seyferts, down to levels which cannot be observed<br />from the ground; {2} characterize the observational {fluxes, colors, structure,<br />sizes} and intrinsic {luminosities, masses, ages, global star-formation rate}<br />properties of these clusters; {3} derive the luminosity functions of young star<br />clusters around the nucleus of Seyferts and compare these results with those<br />from normal and starburst galaxies to determine their survival rate close to the<br />AGN; {4} address questions about the relation between AGNs and starbursts, like<br />the possible connection between the masses and luminosities of black holes and<br />starbursts, and the implications for the evolution of the black holes and their<br />host galaxy bulges. By adding UV images to the existing optical and near-IR<br />ones, this project will create an extremely valuable database for astronomers<br />with a broad range of scientific interests, from the properties of the AGN to<br />the properties of their host galaxies.<br /><br />ACS/WFC 9492<br /><br />Extragalactic Distances: the Need for Accurate Photometry of Blue Supergiants<br />and Cepheids<br /><br />The investigation of the Wind Momentum-Luminosity Relationship {WLR} of blue<br />supergiant stars as an independent extragalactic distance indicator has reached<br />a critical phase. Following our recent discovery and spectroscopic follow-up of<br />several tens of stars outside of the Local Group in NGC 300 and NGC 3621, we can<br />now calibrate the WLR in terms of spectral subtype and metallicity with a higher<br />accuracy than hithertho possible with the statistically limited samples<br />available in the nearby galaxies studied so far. This, however, requires<br />high-resolution imaging to obtain accurate BVI photometry of a significant<br />fraction of those stars for which we have spectroscopic information. This can be<br />effectively accomplished with eight ACS/WFC fields in these two galaxies. As a<br />further step, we can use the calibrated WLR to measure the first independent<br />extragalactic distance. We then propose additional imaging of six ACS/WFC fields<br />in M101 to select blue supergiant candidates for spectroscopic follow-up. Having<br />recently discovered more than a hundred new Cepheids in NGC 300, the<br />high-resolution imaging proposed for the photometry of blue supergiants can also<br />be used, with no additional observing effort, to verify the effects of blending<br />on the Cepheid distance to this galaxy, an important calibrator of secondary<br />distance indicators.<br /><br />ACS/WFC/HRC 8992<br /><br />ACS Early Release Observations.<br /><br />The Advanced Camera for Surveys [WFC and HRC] was used to perform early release<br />observations {ERO}, employing a variety of instruments to demonstrate the new<br />capabilities. The observations [not all in this iteration] will include: 1} WFC<br />observations of peculiar galaxies NGC 4676 {The Mice} and UGC 10214. This will<br />be used to study young stellar clusters formed through the process of galaxy<br />interaction. Any dark companion to UGC 10214 will also be searched for in<br />sensitive ACS/WFC observations. 2} Emission line and continuum imaging of the<br />Cone Nebula and M 17 with WFC to demonstrate the improved sensitivity and<br />angular resolution of ACS. 3} Coronagraphic imaging of HD 141569, a main<br />sequence star with circumstellar disk. 4} Coronagraphic imaging with the HRC of<br />the nearby quasar 3C 273 to investigate the physical properties of the host<br />galaxy and environments.<br /><br />ACS/WFC/HRC 9562<br /><br />Cycle 11 Internal Flat Field Stability.<br /><br />The Advance Camera for Surveys [WFC and HRC] was used to obtain flat field<br />stability and characterization samples of the ACS filter set. Only internal<br />exposures using the calibration lamps were required.<br /><br />GO 9428<br /><br />SINS: The Supernova Intensive Study-- Cycle 11<br /><br />Supernovae create the chemical history of the Universe, energize the<br />interstellar gas, form the spine of the extragalactic distance scale, and<br />provide the only direct evidence for an accelerating universe. SINS is a program<br />to study supernovae, near and far. HST is the perfect match in field and scale<br />for spatially-resolved observations of SN 1987A. There, a violent encounter<br />between the fast-moving debris and the stationary inner ring is well underway.<br />Monitoring this interaction will help solve the riddles of stellar evolution<br />posed by the enigmatic three-ring system of SN 1987A. Our UV observations of<br />Ly-Alpha emission reveal a remarkable reverse shock that provides a unique<br />laboratory for studying fast shocks and a powerful tool for dissecting the<br />structure of the vanished star. For more distant events, we propose<br />Target-of-Opportunity observations. In addition to one bright new supernova in<br />Cycle 11 discovered by any search at any time, we propose to discover two<br />supernovae for study in the ultraviolet at times specified in advance, using<br />the Lick Observatory Supernova Search. SINS will study the historic SN 1987A,<br />explore UV emission from supernovae, and press late-time observations of<br />supernovae into uncharted territory of infrared catastrophes, light echos, and<br />stellar remnants.<br /><br />NICMOS 8790<br /><br />NICMOS Post-SAA calibration - CR Persistence Part 1.<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.<br /><br />NICMOS 9360<br /><br />Paschen-alpha Imaging of a SIRTF-Selected Nearby Galaxy Sample<br /><br />We propose to carry out a NICMOS snapshot survey in the Paschen-alpha {PAlpha}<br />emission line and H-band of the sample of galaxies being observed at 3.5 -- 160<br />microns as part of SIRTF Nearby Galaxies Survey {SINGS} and a related guaranteed<br />time survey of starburst galaxies. The PAlpha images, accessible only from HST,<br />will be combined with groundbased HAlpha imaging to measure the extinction in<br />the star-forming centers of these galaxies, and obtain robust, extinction-<br />corrected maps of the massive star formation rate {SFR}. The PAlpha data by<br />themselves will provide reliable `extinction- free' SFRs, and a<br />cross-calibration of the {dust--affected} HAlpha-- and UV--based SFRs. The<br />PAlpha--based SFR measurements will extend the SFR-vs.-gas density law<br />{Schmidt--law} to surface densities at least 30 times higher than what is<br />accessible using HAlpha--based SFR measurements alone, bridging the gap between<br />normal galaxies and IR--luminous starbursts. Furthermore, the combination of the<br />HST PAlpha images with the SIRTF images and spectra, as well as ancillary<br />ground--based UBVRIJHK images and GALEX UV images being obtained as part of the<br />SINGS project, will provide a definitive study of the radiative transfer of<br />starlight and dust heating in star--forming galaxies. The processed NICMOS<br />images will be incorporated into the public SINGS Legacy Data Archive, to enable<br />scores of follow-up studies by the astronomical community at large.<br /><br />STIS 9506<br /><br />A SNAPSHOT SURVEY OF HIGH COLUMN DENSITY, LOW-Z LyAlpha ABSORBERS<br /><br />We propose a STIS G140L spectroscopic Snapshot program of bright {V<=16.5} AGN<br />not previously observed in the UV to discover new high-column density {N_H >=<br />10^15 cm^-2} LyAlpha absorbers in the local Universe {z <= 0.45}. Many more of<br />these high column density systems are needed because: {1} They contribute most<br />of the baryons to the local IGM; {2} They include systems for which valuable<br />metallicity and D/H measurements can be made with the Cosmic Origins<br />Spectrograph {COS}; {3} They include many of the ``warm-hot'' absorbers, thought<br />to be a large baryon reservoir in the local Universe; and {4} They are most<br />likely to be ``associated'' with galaxy halos. Because of their low-z, many of<br />these absorbers can be located relative to galaxies of known redshifts, allowing<br />an immediate scientific return from these snapshots. Perhaps the most important,<br />lasting results of this survey require higher resolution reobservations with COS<br />by our GTO team. Using these snapshots to select the best targets, we will<br />obtain COS R~22, 000 spectra to determine the D/H and metallicity of absorbers<br />in galaxy halos, groups, and voids. We will use pairs and ``constellations'' of<br />AGN to determine absorber sizes, shapes, and covering factors. Candidate<br />``warm-hot'' absorbers will be reobserved with COS to determine their numbers<br />accurately and to assess their metallicity, sizes, and relationships to galaxies<br />and galaxy groups.<br /><br />STIS 9611<br /><br />CCD Side 2 Gain Ratio Test<br /><br />Observe a bright spectrophotometric standard star at the center of the detector<br />with a wide slit {52x2} with the 3 low dispersion gratings at gain 1 and gain 4,<br />so that the ratio of gain 4 to gain 1 can be measured. {This will be used to<br />calibrate gain 4 relative to gain 1, which is already well measured.} Read out<br />some additional exposures through non-default amplifier B, which is used for<br />some calibration programs, so that the gains of amp B relative to amp D can be<br />measured. Place the target at row 900, close to the D amplifier and far from the<br />B amplifier, then take long and short exposures with G230LB with both<br />amplifiers, so that CTE can be measured over a broad range of counts. With gain<br />4/1, amp B/D, and CTE known from these measurements, find the sensitivity at row<br />900 relative to the central row.<br /><br />STIS/ACS 9498<br /><br />The Nature of the Close Binary Quasar LBQS 0103-2753<br /><br />We propose STIS spectroscopic and ACS imaging observations of the<br />small--separation quasar pair LBQS 0103-2753 A/B {= CT 344}. This quasar pair<br />with z = 0.85, has a projected separation of only 0.3 arcsec or 2.3 kpc. The<br />brighter member of the pair {V = 18.2} is a BAL quasar while the fainter {V =<br />19.4} is a quasar at a similar redshift without BALs. It is very likely that the<br />two quasars are a binary quasar, and not a chance superposition along the line<br />of sight or a gravitational lens {Junkkarinen et al. 2001}. The goals of the<br />STIS spectroscopic observations are to accurately measure the systemic redshifts<br />and redshift difference, to search for variability, and to quantify the emission<br />line differences between the two quasars. Deep ACS WFC images, in the F606W and<br />F814W filters, will be used to provide information on the host galaxy<br />morphologies, to look for the signatures of a merger/interaction -- in<br />particular disturbed isophotes and tidal tails, and to study any cluster of<br />galaxies around this quasar pair. These observations will test the lensing<br />versus binary hypothesis and help differentiate between merging and a high<br />relative velocity galaxy--galaxy interaction. Studies of binary quasars with<br />such close separations will put constraints on merger timescales and duty cycles<br />for AGN fueling at these separations.<br /><br />STIS/CCD 8904<br /><br />Bias Monitor-Part 2.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to monitor the bias in<br />the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4 in order<br />to build up high-S/N superbiases and track the evolution of hot columns.<br /><br />STIS/CCD 9066<br /><br />Closing in on the Hydrogen Reionization Edge of the Universe.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used in parallel constrain<br />the Hydrogen reionization edge in emission that marks the transition from a<br />neutral to a fully ionized IGM at a predicted redshifts.<br /><br />STIS/CCD 8902<br /><br />Dark Monitor-Part 2.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to monitor the darks.<br /><br />STIS/CCD 9317<br /><br />Pure Parallel Imaging Program: Cycle 10.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to perform the default<br />archival pure parallel program for STIS during cycle 10.<br /><br />STIS/CCD/MA2 9048<br /><br />Boron Constraints on Slow Mixing in Low Mass Stars.<br /><br />The Space Telescope Imaging Spectrograph [CCD and MA2] was used to observe the<br />atomic and nuclear characteristics of the light elements Li, Be and B, that make<br />their photospheric abundances ideal tracers of internal physical processes in<br />stars. Both Li and Be have been heavily utilized to this end since their<br />diminished abundances are a direct result of the extent of internal slow mixing<br />between surface and interior layers, as has been shown with ground-based data.<br />Boron provides a fresh and special probe because it survives to greater depths<br />inside stars than does Li or Be, and can thus uniquely reveal the depth of<br />mixing. It is proposed to observe B in stars with very large depletions of Li<br />and Be, i.e. stars which have been the most seriously affected by mixing.<br /><br />STIS/MA1/MA2 9120<br /><br />Planetary Nebulae In The LMC: A Study On Stellar Evolution And Populations.<br /><br />The Space Telescope Imaging Spectrograph [MA1 and MA2] was used to investigate<br />the final phase of the evolution of low- and intermediate-mass stars, the<br />Planetary Nebula {PN} ejection that is thought to provide the main source of<br />carbon and nitrogen enrichment in galaxies.<br /><br />STIS-FUV 9093<br /><br />Resolving Molecular Hydrogen Disks Around T Tauri Stars<br /><br />Molecular hydrogen is believed to be the dominant constituent of circumstellar<br />disks at radii ~ 0.1 - 5 AU around young stars. Fluoresced UV lines pumped by<br />Ly-Alpha are bright and offer a valuable probe of H_2 in disks around young<br />stars, with the ultimate goal being the ability to study the structure and<br />evolution of the planet forming regions around these stars. The limited H_2 data<br />now available for T Tauri stars {TTS} are inadequate to isolate the location of<br />molecular hydrogen emission, though the current data suggests emission from ~ 2<br />AU in the disk around DF Tau. We will use deep, high resolution {E140H} STIS-FUV<br />spectra to resolve the distinctive spectral line signature of Keplerian rotation<br />in disks around two nearly edge on TTS. These will be the first high resolution<br />UV spectra of any TTS and will provide the radius in the disk at which molecular<br />hydrogen can survive. This in turn indicates the inner boundary of the ``dead<br />zone" in TTS accretion disks which is the likely location for the formation of<br />planets.<br /><br />WF/PC-2 9318<br /><br />POMS Test Proposal: WFII Parallel Archive Proposal Continuation.<br /><br />The WF/PC-2 was used to perform the generic target version of the WFPC2 Archival<br />Pure Parallel program. The program was used to take parallel images of random<br />areas of the sky, following the recommendations of the Parallels Working Group.<br /><br />WFPC2 9599<br /><br />WFPC2 Cycle 11 UV Earth Flats<br /><br />Monitor flat field stability. This proposal obtains sequences of earth streak<br />flats to improve the quality of pipeline flat fields for the WFPC2 UV filter<br />set. These Earth flats will complement the UV earth flat data obtained during<br />cycles 8-10.<br /><br />WFPC2 8938<br /><br />WFPC2 CYCLE 9 SUPPLEMENTAL DARKS pt3/3.<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 />FLIGHT OPERATIONS SUMMARY:<br /><br />HSTARS: [For details see ]http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf]<br />8740 - SchedulerReqMgrServe process count 75 @200/0710z.FOT called and asked we<br /> had any problems on a-string appserver was grayed out when the appserver<br /> came back under ScheduleReqMgrServe had a process count of 75. Under<br /> investigation.<br /><br />8741 - FHST Roll Delay U2,3RD failed @201/1012z. The error box results<br /> [i.e "3Failed"] for mnemonics QEBSTFG0, QEBSTFG1, QEBSTFG2.<br /> The subsequent GSAcq3,1,3 at 201/10:28:26 was successful. Under<br /> investigation.<br /><br />COMPLETED OPS REQs:<br />16801-1 - CCC/VIK K52 Level Change [level 3] @200/1425z<br /><br />OPS NOTES EXECUTED:<br />1025 - CCC K52 Level 3 Limits @200/1442z<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 26 26<br />FGS REacq 21 21<br />FHST Update 49 48 201/1012z[HSTAR#8741]<br />LOSS of LOCK None<br /><br />Operations Notes: None<br /><br />SIGNIFICANT EVENTS:<br /><br />Successfully changed Battery 5 K52 Level 3 @ 200/14:25Z [OR 16801-1]. Battery<br />5 has continued to operate at elevated temperatures and has exhibited higher<br />load-share then the other batteries, which drives the VTFE/TRSWCC to lower<br />Voltage cut-off levels and results in Batteries 1 - 4 experiencing a gradual<br />capacity decline. See HSTARs 8678 and 8723.<br /><br />Successfully completed CCS Release 4.0.1 Extended Command testing on Day 198/199.<br />Objective of test was to delve deeper into the command system than had been done<br />with recent CCS command testing and further investigate possible problems noticed<br />earlier. Send /OBC FSW loads for NSSC-1 and 486 continuously for 2.5 hours, looking<br />for a system "freeze". None occurred. Verified CCS CCL does not recognize COS or<br />WFC3 redundant device. Should be in Release 4.0.2 [CR 6404]. IP Command line to<br />SOC dropped when VEST connected their command line. Known bug, GSCA 521<br />implementation will fix problem.