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Daily 3870
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science DAILY REPORT # 3870 PERIOD COVERED: DOY 147-150 OBSERVATIONS SCHEDULED ACS/HRC 9854 Anomalous Flux Ratios in Quadruple Gravitationally Lensed QSOs We propose to observe eight {8} gravitationally lensed systems which exhibit quadruple images of the background high redshift quasars. Models invoking a smooth potential fit the observed image positions accurately, in most cases better than 5 milliarcseconds. But the same models dramatically fail to predict the observed flux ratios. These anomalous flux ratios can be attributed to micro- or milli-lensing in the massive lensing halo. In this proposal, we will isolate the source of the anomalous flux ratios by using the superior resolution of HST to obtain spectrophotometric data and compare the emission line flux ratio of the QSOs to the continuum flux ratios. Due to the much larger size of the broad emission line regions, the flux ratios in the emission lines should only be affected by milli-lensing if the sub-halos are comparable or larger in projected size than the source region. That is, flux ratios observed in the QSO continuum are senstive to substructure on all scales {both micro- and milli-lensing}, while the broad emission lines are insensitive to micro-lensing due to the larger physical size of the source emission region. This sample of eight quasars will provide the definitive evidence to distinguish between possible sources causing the observed anomalous flux ratios. NICMOS 8790 NICMOS Post-SAA calibration - CR Persistence Part 1. 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. S/C 10700 Guide Star Test for the Deep Impact Encounter This proposal is to perform guide star tests on the critical HST science visits circum- encounter of the Deep Impact mission with comet 9P/Tempel 1. ACS/HRC/WFC 10438 The Late Formation of Satellite Galaxies Tiny isolated HII regions have been discovered up to 30 kpc from the closest galaxy in the NOAO Survey for Ionization in Neutral Gas Galaxies {SINGG}. These halo HII regions can be ionized by only a few OB stars and seem to be most commonly found in interacting systems. They may represent the beginning of the formation of satellite galaxies at low redshift and/or are the source of the numerous intracluster planetary nebula. The halo HII regions are a unique mode of star formation in a low density and low metallicity environment and high resolution HST images are required to identify their underlying stellar populations. Determining the stellar populations of these HII regions will establish whether in-situ star formation is a significant contributor to the stellar content and enrichment of galactic halos and intergalactic space. In particular, ACS/HRC observations are required for their resolution, UV sensitivity, and wide wavelength coverage, allowing young and intermediate age populations to be identified. Parallel ACS/WFC observations will explore the possibility of a further stellar population in the interactive debris. The results of this project have implications on the formation of satellite galaxies, the origin of Galactic halo B stars, IGM ionization and enrichment, and star formation principles. ACS/HRC 10431 A Search for Faint Companions of Altair We propose to use the innovative new technique of spectral deconvolution {Sparks & Ford 2002} to search for very faint companions, possibly extrasolar planets shining by reflected light, around Altair, the nearest bright, single star to the Sun. The technique offers a Poisson-limited detection capability that brings Jovian-class planets into the realm of feasibility for a select few stars. We turn the wavelength dependence of the coronagraphic PSF to advantage and use it to eliminate stray light from the host star. As part of the detection process, we obtain a spectrum over the wavelength range, 750 nm to 1 micron, with 9% resolution. The search will be orders of magnitude more sensitive than all previous efforts and should take us to within about an order of magnitude of the Jovian luminosity flux limit. ACS/WFC/WFPC2 10402 The Formation and Evolution of Spirals: An ACS and WFPC2 Imaging Survey of Nearby Galaxies Over 50% of galaxies in the local universe are spirals. Yet the star formation histories and evolution of this crucial population remain poorly understood. We propose to combine archival data with new ACS/WFC and WFPC2 observations of 11 galaxies, to tackle a comprehensive investigation of nearby spirals covering the entire spiral sequence. The new observations will fill a serious deficiency in HST's legacy, and maximize the scientific return of existing HST data. The filter combination of UBVI, and Halpha is ideal for studying stellar populations, dust properties, and the ISM. Our immediate scientific objectives a {i} to use the resolved cluster populations, both young massive clusters and ancient globular clusters as a chronometer, to understand how spirals assembled as a function of time; {ii} study the rapid disruption properties of young clusters; and {iii} understand dust distributions in spirals from pc to kpc scales. Each of these goals provides an important step towards charting the evolution of galaxies, and an essential baseline for interpreting the galaxy populations being surveyed in both the early and present universe. The resolution of our survey, which exploits the excellent imaging capabilities of HST's two optical cameras, will enable us to understand the record of star cluster, and galaxy formation in a level of detail which is not possible for more distant systems. Finally, the proposed observations will provide a key to interpret an extensive, multiwavelength archive of space- and ground- based data at lower spatial resolution {SPITZER, CHANDRA, GALEX, NICMOS P alpha and H band imaging} for local spirals. ACS/HRC/WFC 10399 Accurate and Robust Calibration of the Extragalactic Distance Scale with the Maser Galaxy NGC4258 II The extragalactic distance scale {EDS} is defined by a comparison of Cepheid Period-Luminosity {PL} relations for nearby galaxies and the LMC, whose uncertain distance is thereby the SOLE anchor. Studies of masers orbiting the central black hole in NGC4258 have provided the most accurate extragalactic distance ever {7.2+/-0.5 Mpc}, and new radio data and analysis techniques will reduce the uncertainty to 3.5% {0.07 mag} by 2005. Since this distance is well determined and based on geometric arguments, NGC4258 can provide a much needed new anchor for the EDS. Ultimately, the combination of an independent measurement of H0 and measurements of CMB fluctuations {e.g., WMAP} can be used to directly constrain cosmological parameters including the equation of state of dark energy. In our Cycle 12 proposal, we defined a program spanning two cycles. The Cycle 12 portion was accepted. We have acquired WFC images and are constructing well sampled PL relations in 3 colors {BVI}. The purpose of the Cycle 13 observations is to address systematic sources of error and is crucial for the success of the entire program. To disentangle the effects of reddening and metallicity, and to characterize the effects of blending, we require 50 orbits to obtain H-band photometry {NICMOS/NIC2} and high resolution images {ACS/HRC}. WFPC2/ACS/WFC 10397 The Ghosts of Galaxies: Tidal Debris and the Formation of Clusters Intergalactic stellar populations and tidal debris are now recognized as important components of galaxy clusters. This project examines the interrelated processes of galaxy destruction, recycling of tidal debris, and creation of dwarf galaxies and intergalactic star clusters, all of which are part of the grand scheme of cluster formation. We propose deep multicolor imaging of two examples of newly created tidal debris, the spectacular plumes in the Centaurus and Coma clusters. The Centaurus observations will extend our earlier work, which demonstrated the existence of tidal debris dwarf galaxies and star cluster in the body of the Centaurus plume. Deep ACS/WFC observations can determine rough ages and cluster membership, better characterizing the new debris. The Coma observations will reproduce this work for a second plume feature, in the quintessential rich cluster of galaxies. Parallel WFPC2 observations will investigate the central intracluster spaces at the bottom of the each cluster's potential, where older debris is thickest. ACS/WFC/WFPC2 10394 Deep imaging of newly discovered globular clusters in the outer halo of M31 Globular clusters {GCs} are fossil relics with which we can investigate the processes of galaxy formation and growth. We have recently discovered a sample of GCs, as part of a very wide area CCD survey of M31. These clusters span a range in projected galactocentric distance of 20 - 80 kpc, more than double the radii of the previous most remote known GC. Here we apply for deep ACS images of 13 GCs, which will allow us to study their stellar populations, line-of-sight distances and structural parameters. These will be used to: a} Investigate the merger history of M31, through an examination of variations in the RGB and HB morphologies, particularly to obtain metallicities and check for the presence of any second parameter effect in the HB. d} Determine, in conjuction with ground-based spectroscopy, the dynamical mass of M31 at large radius, providing a direct probe of the mass distribution of its dark halo. ACS/HRC/WFC 10389 ACS CCDs daily monitor - Cycle 13 - Part 2 This program consists of a set of basic tests to monitor, the read noise, the development of hot pixels and test for any source of noise in ACS CCD detectors. The files, biases and dark will be used to create reference files for science calibration. This programme will be for the entire lifetime of ACS. ACS/HRC/WFC/WFPC2 10384 Focus Monitor The focus of HST is measured from WFPC2/PC and ACS/HRC images of stars. Multiple exposures are taken in parallel over an orbit to determine the influence of breathing on the derived mean focus. Observations are taken of clusters with suitable orientations to ensure stars appear in all fields. ACS/HRC 10377 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 coronagraphic monitoring is required to assess the changing position of the spots. WFPC2 10363 WFPC2 CYCLE 13 Intflat and Visflat Sweeps and Filter Rotation Anomaly Monitor Using intflat observations, this WFPC2 proposal is designed to monitor the pixel-to- pixel flatfield response and provide a linearity check. The intflat sequences, to be done once during the year, are similar to those from the Cycle 12 program 10075. The images will provide a backup database as well as allow monitoring of the gain ratios. The sweep is a complete set of internal flats, cycling through both shutter blades and both gains. The linearity test consists of a series of intflats in F555W, in each gain and each shutter. As in Cycle 12, we plan to continue to take extra visflat, intflat, and earthflat exposures to test the repeatability of filter wheel motions. ACS/WFC 10352 A Study of the Physics of Extended Relativistic X-ray Jets, Discovered in our We will measure the changing flow speeds, magnetic fields, and energy fluxes in well-resolved quasar jets found in our short-exposure Chandra survey by combining new, deep Chandra data with radio and optical imaging. We will image each jet with sufficient sensitivity to estimate beaming factors and magnetic fields in several distinct regions, and so map the variations in these parameters down the jets. HST observations will help diagnose the role of synchrotron emission in the overall SED, and may reveal condensations on scales less than 0.1 arcsec. ACS/WFC 10343 X-ray from misaligned FRI jets: IC/CMB emission from a fast spine? There is evidence that FRI jets have a fast "spine", consisting of relativistically moving plasma, and a slow "wall", decelerated by entrainement of ambient gas. This opens the interesting possibility that inverse Compton scattering of the CMB photons {IC/CMB} off the relativistic electrons could contribute to the high-energy emission from the fast spine. This strongly beamed radiation is visibile only in closely aligned FRI jets, i.e., acccording to unification schemes, in BL Lac objects. Thus, we propose to observe 2 radio-selected BL Lacs with prominent radio jets to search for IC/CMB X-ray emission and confirm unification models. This study will impact models for the origin of the FRI/II division. ACS/HRC 10255 A Never Before Explored Phase Space: Resolving Close White Dwarf / Red Dwarf We propose an ACS Snapshot imaging survey to resolve a well-defined sample of highly probable white dwarf plus red dwarf close binaries. These candidates were selected from a search for white dwarfs with infrared excess from the 2MASS database. They represent unresolved systems {separations less than approximately 2" in the 2MASS images} and are distributed over the whole sky. Our HST+ACS observations will be sensitive to a separation range {1-20 AU} never before probed by any means. The proposed study will be the first empirical test of binary star parameters in the post-AGB phase, and cannot be accomplished from the ground. By resolving as few as 20 of our ~100 targets with HST, we will be able to characterize the distribution of orbital semi-major axes and secondary star masses. ACS/SBC 10231 Tracing the Reionization History of Intergalactic Helium out to Redshift 3.8 We have found He II absorption in a quasar at redshift 3.82 via our Cycle 12 program of UV snapshots. This is the highest redshift yet at which He II absorption has been observed, and we propose to study helium ionization in the IGM along this new, long, unobscured sightline to high- redshift. The object has UV flux comparable to that of the rare handful of other z3 quasars known to be suitable for helium studies, and it is also in the Continuous Viewing Zone. Theproposed spectrum will allow us to study the evolution and properties of the IGM and ionizing radiation from z=3.8 {the IGM environment near the quasar} all the way down to z=2.8. This redshift range may span the epoch of helium reionization, and even extends to high enough redshift to enable improved helium opacity measures using both He II Ly-alpha and Ly-beta. This program is now approved to use ACS prism. ACS/HRC 10198 Probing the Dynamics of the Galactic Bar through the Kinematics of Microlensed The observed optical depths to microlensing of stars in the Galactic bulge are difficult to reconcile with our present understanding of Galactic dynamics. The main source of uncertainty in those comparisons is now shifting from microlensing measurements to the dynamical models of the Galactic bar. We propose to constrain the Galactic bar models with proper motion observations of Bulge stars that underwent microlensing by determining both the kinematic identity of the microlensed sources and the importance of streaming motions. The lensed stars are typically farther than randomly selected stars. Therefore, our proper motion determinations for 36 targeted MACHO events will provide valuable constraints on the dynamics of bulge stars as a function of distance. The first epoch data for our proposed events is already available in the HST archive so the project can be completed within a single HST cycle. The exceptional spatial resolution of HST is essential for completion of the project. Constraints on the total mass in the bulge will ultimately lead to the determination of the amount of dark matter in inner Galaxy. ACS/WFC/NIC3 10195 Probing the Surroundings of a Highly Luminous Redshift 6.5 Galaxy We propose deep images of a recently discovered galaxy at z=6.535, which is among the most luminous Lyman-alpha emitting galaxies known at high redshift. The brightness and rarity of this source imply that it is associated with a high peak in the matter density distribution. {It is the brightest Lyman alpha source in 2e5 comoving Mpc3, with a luminosity of 6 L*.} Further objects in this peak are expected to be visible with HST's sensitivity. The Lyman alpha line has a large rest frame equivalent width, with a lower bound 100 Angstroms. Such a large equivalent width would be impossible for objects embedded in neutral gas, and instead requires either that {a} the universe was reionized before z=6.5 or {b} the galaxy resides in a local ionized bubble, in which case an additional contribution to the ionizing photon budget from presently undetected neighbors is required. With 19 orbits of ACS and NICMOS imaging, we will measure this object's morphology and spectral energy distribution, thus searching for either active nuclei or old stellar populations. We will also search for possible neighbors, which could establish the first known galaxy group at z6, and may provide sufficient ionizing flux to allow the escape of the observed Lyman alpha photons in a neutral universe. If neighbors are not found, it will lead to an upper bound on the neutral fraction in the general IGM at z=6.5. ACS/HRC 10185 When does Bipolarity Impose itself on the Extreme Mass Outflows from AGB Stars? An ACS SNAPshot 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? Our previous SNAPshot surveys of a PPNe sample {with ACS & NICMOS} show that roughly half our targets observed are resolved, with well-defined bipolar or multipolar morphologies. Spectroscopic surveys of our sample confirm that these objects have not yet evolved into planetary nebulae. Thus, the transformation from spherical to aspherical geometries has already fully developed by the time these dying stars have become preplanetary nebulae. From this new and surprising result, we hypothesize that the transformation to bipolarity begins during the very late AGB phase, and happens very quickly, just before, or as the stars are evolving off the AGB. We propose to test this hypothesis quantitatively, through a SNAPshot imaging survey of very evolved AGB stars which we believe are nascent preplanetary nebulae; with our target list being drawn from published lists of AGB stars with detected heavy mass-loss {from millimeter-wave observations}. This survey is crucial for determining how and when the bipolar geometry asserts itself. Supporting kinematic observations using long-slit optical spectroscopy {with the Keck}, millimeter and radio interferometric observations {with OVRO, VLA & VLBA} are being undertaken. The results from this survey {together with our previous work} will allow us to draw general conclusions about the onset of bipolar mass-ejection during late stellar evolution, and will provide crucial input for theories of post-AGB stellar evolution. Our survey will produce an archival legacy of long-standing value for future studies of dying stars. NIC2 10176 Coronagraphic Survey for Giant Planets Around Nearby Young Stars A systematic imaging search for extra-solar Jovian planets is now possible thanks to recent progress in identifying "young stars near Earth". For most of the proposed young {~ 30 Myrs} and nearby {~ 60 pc} targets, we can detect a few Jupiter-mass planets as close as a few tens of AUs from the primary stars. This represents the first time that potential analogs of our solar system - that is planetary systems with giant planets having semi-major axes comparable to those of the four giant planets of the Solar System - come within the grasp of existing instrumentation. Our proposed targets have not been observed for planets with the Hubble Space Telescope previously. Considering the very successful earlier NICMOS observations of low mass brown dwarfs and planetary disks among members of the TW Hydrae Association, a fair fraction of our targets should also turn out to posses low mass brown dwarfs, giant planets, or dusty planetary disks because our targets are similar to {or even better than} the TW Hydrae stars in terms of youth and proximity to Earth. Should HST time be awarded and planetary mass candidates be found, proper motion follow-up of candidate planets will be done with ground-based AOs. ACS/WFC 10152 A Snapshot Survey of a Complete Sample of X-ray Luminous Galaxy Clusters from Redshift 0.3 to 0.7 We propose a public, uniform imaging survey of a well-studied, complete, and homogeneous sample of X-ray clusters. The sample of 73 clusters spans the redshift range between 0.3-0.7. The samples spans almost 2 orders of magnitude of X-ray luminosity, where half of the sample has X-ray luminosities greater than 10^44 erg/s {0.5-2.0 keV}. These snapshots will be used to obtain a fair census of the the morphology of cluster galaxies in the cores of clusters, to detect radial and tangential arc candidates, to detect optical jet candidates, and to provide an approximate estimate of the shear signal of the clusters themselves, and potentially an assessment of the contribution of large scale structure to lensing shear. NIC3 10150 NICMOS observations of A1689 The potential of galaxy clusters as ``cosmic telescopes'' has been known for a long time, but practical results in the pre-ACS era have been scarce due to two main problems: the uncertainty in determining the magnification distribution of the cluster {the ``optics'' of the instrument} and the presence of numerous bright cluster galaxies which cover the field of view and hinder the detection of background galaxies. We have developed techniques to solve these two problems working with our ACS observations of A1689, the most powerful lens in the sky, and for the first time we have been able to determine the "specifications" of a cosmic telescope with a useful level of precision, thanks to the detection and identification of more than 100 multiple images with reliable redshift information. We propose to observe the high magnification region in the A1689 field in the F110W band with a 3x3 mosaic of NIC3 pointings; the resulting image will reach a lens-corrected limiting magnitudes of 29.5 for point sources, surpassing in depth the UDF NICMOS observations and providing an unique dataset with multiple scientific returns. NIC3/WFPC2/ACS/WF 10131 C Determining the Origin of Virgo's Intracluster Stars Intracluster stars constitute about 20% of the total stellar population of a typical galaxy cluster, and their existence provides a vital clue for our understanding of cluster formation and evolution. However, to exploit their probative value, we need to know their origins: are they the remnants of dwarf galaxies, long since destroyed by the cluster potential, or have the stars been harassed from their parent galaxies at recent epochs? To answer this question, we propose to use the Wide-Field Channel of ACS to make an I, {V-I} color-magnitude diagram of Virgo's intracluster stars. From the position and morphology of the population's red giant branch, we will be able to determine the metallicity distribution function of the stars, and thereby determine their likely origin and ejection mechanisms. Only HST with the ACS has the sensitivity and resolution to perform this fundamental measurement. This program has two options. Option one uses conventional methods of cluster photometry and requires 37 orbits of exposure time. Option two involves a novel analysis technique, which promises to achieve most of the same science in two- thirds the time {23 orbits}. We describe this alternative method of analysis and demonstrate its use via simulations. ACS/WFC 10119 Solving the Mystery of the Short-Hard Gamma-Ray Bursts Seven years after the afterglow detections that revolutionized studies of the long- soft gamma-ray bursts, not even one afterglow of a short-hard GRB has been seen, and the nature of these events has become one of the most important problems in GRB research. The forthcoming Swift satellite will report few-arcsecond localizations for short-hard bursts in minutes, however, enabling prompt, deep optical afterglow searches for the first time. Discovery and observation of the first short-hard optical afterglows will answer most of the critical questions about these events: What are their distances and energies? Do they occur in distant galaxies, and if so, in which regions of those galaxies? Are they the result of collimated or quasi-spherical explosions? In combination with an extensive rapid-response ground-based campaign, we propose to make the critical high-sensitivity HST TOO observations that will allow us to answer these questions. If theorists are correct in attributing the short-hard bursts to binary neutron star coalescence events, then the short-hard bursts are signposts to the primary targeted source population for ground- based gravitational-wave detectors, and short-hard burst studies will have a vital role to play in guiding their observations. FGS 10110 Parallaxes of Extreme Halo Subgiants: Calibrating Globular Cluster Distances and the Ages of the Oldest Stars The ages of the oldest stars are a key constraint on the evolution of our Galaxy, the history of star formation, and cosmological models. These ages are usually determined from globular clusters. However, it is alternatively possible to determine ages of extreme Population II subgiants in the solar neighborhood based on trigonometric parallaxes, without any recourse to clusters. This approach completely avoids the vexing issues of cluster distances, reddenings, and chemical compositions. There are 3 known nearby, extremely metal-deficient Pop II subgiants with Hipparcos parallax errors of 6-11% which are available for such age determinations. At present, based on the latest isochrones, the derived ages of these stars {HD 84937, HD 132475, and HD 140283} are all close to 14 Gyr, uncomfortably close to or higher than current estimates of the age of the universe. However, the errors in the Hipparcos parallaxes imply uncertainties of at least 2 Gyr in the ages of the 3 stars. We propose to measure parallaxes of these three Pop II subgiants using HST's Fine Guidance Sensor 1R. We expect to reduce the Hipparcos parallax error bars by factors of 5-6, providing the most stringent test yet of current theoretical stellar models of Pop II stars and pushing the age uncertainties to below 0.5 Gyr. These data will also provide a major new constraint on the distance scale of globular clusters, with wide implications for stellar evolution and the calibration of Pop II standard candles. ACS/HRC 10102 Rings of Uranus: Dynamics, Particle Properties and Shepherding Moons Last year, our Uranian ring and moon observing program {GO-9823} resulted in the discovery of two moons, S/2003 U 1 and S/2003 U 2. We imaged two additional small moons, Ophelia and S/1986 U 10, that had not been seen since the Voyager encounter of 1986. Furthermore, our data show faint arcs and clumps orbiting within the rings, which were not seen by Voyager and are completely unexpected. We employed several "tricks" of the HRC to achieve this remarkable sensitivity; specifically, we used the CLEAR filter and oriented the images so that the planet, though vastly overexposed, did not interfere with the ring/moon region of interest to us. This allowed us to detect 25th-magnitude moons circling a 5th-magnitude planet. Now we propose to complete the task by carrying out a comprehensive survey of the system using the same techniques. Our goals are to recover the moons, better discern their orbital elements, and learn more about the dynamics of the ring clumps. In particular, we need to {1} understand the long-term stability of S/2003 U 2, which orbits perilously close to the larger moon Belinda; {2} complete our search for moons, which was only ~ 50% complete last year, and {3} better understand how the clumps and arcs within the ring system might relate to nearby "shepherding" moons, seen or unseen. This program is now a merger of two programs 10275 and 10102. The former is our new program, whereas the latter is the second year of our three-year program to study the light scattering properties of Uranus's rings as they approach their edge-on presentation in 2007. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) HSTARS: 9836 - GSacq(2,1,2) Failed to RGA control @ 149/18:03:59z The GSacq(2,1,2) scheduled at 149/17:54:18 failed to RGA control due to search radius limit exceeded on FGS 1 and FGS 2. the following Reacqs also failed due to SRLEX. A real time map at 20:35 showed errors of -10.781, 39.085, and 7.170 . 9837 - ACS Target Acquistion Failed Due to Guide Star Failure. @ 149/18:09:33z ACS target acquisition scheduled at 149/18:07:50 failed due to GSacq failure. ACS Status Buff message 954, P= 1, T = 13745 COMPLETED OPS REQUEST: (None) COMPLETED OPS NOTES: (None) SCHEDULED SUCCESSFUL FAILURE TIMES FGS Gsacq 34 33 Hstar # 9836 FGS Reacq 28 25 Hstar # 9836 FHST Update 57 57 LOSS of LOCK SIGNIFICANT EVENTS: (None) |
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