HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3151<br /><br />PERIOD COVERED: DOY 184 - 188<br /><br />OBSERVATIONS SCHEDULED [see HSTARS below for possible observation problems]<br /><br />ACS 9564<br /><br />ACS Cycle 11: UV Earth Flats<br /><br />This proposal will obtain sequences of UV flats by observing the bright Earth.<br />The HRC UV filters were chosen for modes which were not obtained in the lab.<br />Since the UV transmission is likely to vary as a function of position on the<br />Pol_UV filters and on the coronograph, and since this behavior is currently<br />unconstrained by measurement, a good estimate for the missing UV flats cannot be<br />made. Although POL_UV and CORON transmissions change little at long wavelengths,<br />the UV transmission may change by amounts larger than can be estimated in the<br />absence of actual UV transmission measurements<br /><br />ACS 9443<br /><br />Calibration of the Geometric Distortion of ACS<br /><br />We propose to calibrate the geometric distortion of the WFC and HRC of ACS,<br />using the state-of-the-art techniques that we have developed for WFPC2. We are<br />confident that we can measure the distortion to at least an order or magnitude<br />higher accuracy than is called for in the ACS Manual. We will use the images<br />that are to be taken in GO-9028 and will re- image the field used there at<br />different orientation and through different filters, so as to improve knowledge<br />of the skewness of the field and the dependence of distortion on wavelength. Our<br />results will not only enhance the accuracy of our own proposed proper-motion<br />work in star clusters; they will greatly increase the accuracy of sparse-field<br />astrometry by others, such as solar-system and extragalactic work.<br /><br />ACS 9678<br /><br />Direct Measurement of the Size of the Largest Kuiper Belt Object<br /><br />We propose an ACS observation of a recently-discovered bright Kuiper Belt<br />Object.<br /><br />ACS 9568<br /><br />Grism/Prism Calibration<br /><br />A Planetary Nebula in the LMC and a Galactic White Dwarf are observed through<br />the prism of the High Resolution Channel to measure: 1} the dispersion of the<br />prism and its field dependence; 2} the prism throughput and its field<br />dependence. Therefore, these measurements will be carried out at several<br />positions on the chip including the centre and the corners of the HRC chip. The<br />same White Dwarf is observed together with a Galactic Wolf-Rayet star through<br />the grism of the Wide Field Channel in a number of positions complementing those<br />already observed in SMOV. The purpose here is to better characterize the field<br />dependence of the grism dispersion in the WFC.<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 9425<br /><br />The Great Observatories Origins Deep Survey: Imaging with ACS<br /><br />We propose a Treasury program of ACS imaging as part of the Great Observatories<br />Origins Deep Survey {GOODS}, covering 320{square}', or 32* the area of the two<br />original WFPC2 HDFs, to within 0.5--0.8 mag of their depth in four ACS bands,<br />BViz. The two GOODS fields, the Hubble Deep Field North and Chandra Deep Field<br />South, are the premier deep survey areas from X-- ray to radio wavelengths. ACS<br />data will provide unique angular resolution, sensitivity, and wavelength<br />coverage to close the gap between the deepest Chandra and SIRTF observations.<br />Supported by extensive imaging and spectroscopy from the VLT, Keck, Subaru,<br />NOAO, Gemini, VLA, JCMT, and other facilities, the combined GOODS data set will<br />make it possible to map the evolution of the Hubble sequence with redshift,<br />reconstruct the history of galaxy mass assembly, star formation and nuclear<br />activity from the epoch of reionization to the present, trace the growth of<br />density perturbations via cosmic shear, and, with properly phased z--band<br />observations, detect ~ 12 Type Ia supernovae at 1.2<z<1.8 to test the cosmic<br />acceleration and the presence of dark energy. All HST, SIRTF, Chandra, and<br />supporting GOODS data are non-- proprietary, with science--quality images and<br />catalogs released on a time scale of months. This will constitute the deepest,<br />largest, and most uniform panchromatic data set ever assembled to study the<br />distant universe.<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 9444<br /><br />The Region of the Hydrogen-Burning Limit in Omega Centauri and 47 Tucanae<br /><br />We propose a photometric study of the lower main sequences of Omega Cen and 47<br />Tuc, down to the region of the H-burning limit, which the deeper faintness limit<br />of ACS will allow us to reach. For the faintest stars, proper-motion separation<br />of cluster from field is essential; hence we include Cycle 13 observations. The<br />resulting color--magnitude diagrams {CMDs} and luminosity functions {LFs} will<br />allow study of stars in a mass regime and metallicity that have never been<br />accessible before, and will serve as an important check on theories of the<br />structure of low-mass stars. Our CMDs will check the luminosity--radius<br />relation, while the faint end of the LF can be used to check the<br />mass--luminosity relation. With 47 Tuc we extend these checks to a higher<br />metallicity than before, while in Omega Cen we investigate the effect of a range<br />of metallicity within a single cluster. In both clusters we will produce the<br />faintest existing MS and WD sequences, and the faintest LF. With this proposal<br />we initiate high-precision astrometry with ACS using the state-of-the-art<br />techniques that we have developed for WFPC2. A separate proposal addresses the<br />geometric distortion of ACS, but we can do well in the present work even with<br />approximate distortion corrections, as we can if necessary confine our<br />measurements to relative positions of closely neighboring stars.<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/WFC 9584<br /><br />ACS Default {Archival} Pure Parallel Program II.<br /><br />The Advanced Camera for Surveys [WFC] was used to test ACS pure parallels.<br /><br />ACS/WFC 9575<br /><br />Default {Archival} Pure Parallel Program.<br /><br />The Advanced Camera for Surveys [WFC] was used to test ACS pure parallels in<br />POMS.<br /><br />ACS/WFC 9373<br /><br />Reaching the Horizontal Branch in NGC 5128: Deepest Probe of a Giant Elliptical<br /><br />NGC 5128 is the nearest easily observable giant E galaxy, and is a unique<br />testing ground for stellar population models. Previous WFPC2 photometry of its<br />halo red-giant stars has shown that they are predominantly metal-rich<br />{<m/H>~-0.45}, but little is yet known about their spread in ages. With the<br />ACS/WFC camera, we propose to obtain deep {V, I} photometry down to the level of<br />its horizontal-branch population, with the goal of refining the metallicity<br />distribution function and gaining quantitative information on its age<br />distribution. This will be unique data for any giant elliptical galaxy and will<br />provide major new input to population synthesis techniques for such galaxies.<br /><br />ACS/WFC/HRC 9075<br /><br />Cosmological Parameters from Type Ia Supernovae at High Redshift.<br /><br />The Advanced Camera for Surveys [WFC and HRC] was used to obtain a Hubble<br />diagram of Type Ia supernovae {SNe Ia} that will be of long lasting value as a<br />record of the expansion history of the universe.<br /><br />CAL/WF2 9597<br /><br />Intflat Sweep, Visflat Sweep, and Filter Anomaly Check<br /><br />No abstract available.<br /><br />GO 9493<br /><br />Revealing the nature of low luminosity radio-galaxies with imaging polarimetry<br /><br />HST imaging of low luminosity FR I radio-galaxies allowed us to isolate for the<br />first time their optical nuclear emission from that of the host galaxy. Fluxes<br />of these unresolved nuclear sources strongly correlate with those of the radio-<br />cores, suggesting a common non-thermal origin. The picture which emerges is that<br />these radio-galaxies differ in many fundamental aspects from the other classes<br />of AGN as they might be lacking the substantial BLR, thermal disk emission and<br />torii, usually associated to active nuclei, probably reflecting a fundamentally<br />different accretion mode. On the other hand, these results support the<br />identification of FR I as the misoriented population of BL Lac objects. It is<br />crucial at this stage to firmly establish the synchrotron origin of these<br />nuclear sources. A simple and direct test can be performed by measuring their<br />polarization. In case of synchrotron emission we expect to detect significant<br />nuclear polarization, as routinely measured in BL Lac objects, at level of 3 -<br />20 We thus propose to obtain imaging polarimetry of a sample formed by the 9<br />nearest FR I radio- galaxies.<br /><br />GO 9364<br /><br />The Parallaxes and Proper Motions of Two Nearby Neutron Stars<br /><br />We propose to measure the parallax of two nearby neutron stars to the highest<br />possible level of accuracy, ~.0.5 mas. The primary goal is to determine the<br />neutron-star radius at infinity with better than 1 km precision, and therewith<br />obtain a direct constraint on the equation of state of matter at supra-nuclear<br />density. The required flux and temperature determinations are easiest for the<br />so-called isolated or radio-quiet neutron stars because of their apparently<br />completely thermal spectrum. We argue that the importance of the possible<br />results warrants a study to the best possible level of the best possible<br />sources, and request 24 orbits for the two brightest isolated neutron stars, RX<br />J1856.5-3754 and RX J0720.4-3125. We will also determine whether the enigmatic<br />RX J0720.4-3125 is an old magnetar or an accreting source, based on its<br />luminosity and proper motion.<br /><br />NICMOS 8979<br /><br />NICMOS Optimum Coronagraphic Focus Determination<br /><br />As originally designed the NICMOS coronagraph had two focii at conjugate points<br />in the optical path with the coronagraphic hole at the f/24 focus of the input<br />OTA beam, and the detector at the reimaged f/45 focus in Camera 2. Because of<br />the forward displacement of the cold optical bench holding the Camera 2<br />detector, as a result of the larger-than-expected expansion of the solid N2<br />cryogen {as described and documented by the 'Dewar Anomoly Review Board'}, the<br />two focii are now aconjugate. For direct imaging this is of little concern, and<br />the HST/NICMOS Camera 2 focus interface is established by co-locating the f/45<br />image plane on the detector. This is done by de-spacing the relayed focus<br />through a translative motion {with compensating comal tilt correction} of the<br />Pupil Alignment Mechanism {PAM}. The mirror which this mechanism drives is<br />upstream of the field divider mirror upon which the coronagraphic hole resides.<br />Therefore, achieving a "best" focus at the detector results in a "soft" focus<br />{in the f/24 image plane} at the coronagraphic hole. This leads to a<br />wavelength-dependent increase in the diffracted energy in the now-defocused<br />unocculted wings of a PSF from a target placed inside of the coronagraphic hole<br />{as the f/24 image plane will fall behind the surface of the camera 2 field<br />divider mirror} increasing the scattered and diffracted background around the<br />target and lowering the field contrast at the detector image plane. In principal<br />the coronagraphic stray light rejection would be most efficient by minimizing<br />the spot size of an input PSF in the hole. This, however, is traded against a<br />small degree of defocus at the detector. Ultimately, the best coronagraphic<br />performance is achieved where the image contrast between an unocculted target<br />and the residual background from an occulted source {both affected differently<br />by focus and subsequent scattering} is maximized. The purpose of this test is to<br />find the optimum PAM position to maximize the coronagraphic image:background<br />contrast ratio. Further details and background information may be found in the<br />SMOV/7157 test report "NICMOS Optimal Coronagraphic Focus Determination"<br />available from the NICMOS IDT.<br /><br />NICMOS 9269<br /><br />NICMOS Parallel Thermal Background<br /><br />NICMOS Camera 3 pure parallel exposures in the F222M filter will be obtained for<br />the entire duration of SMOV to establish the stability of the HST+NCS+Instrument<br />thermal emission.<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 />POMS 9677<br /><br />POMS Test Proposal: WFII backup parallel archive proposal<br /><br />This is a POMS test proposal designed to simulate scientific plans.<br /><br />SNAP 9356<br /><br />SNAPSHOT survey of the Planetary Nebulae population of the Galactic Bulge<br /><br />The spectacular structures seen in HST images of planetary nebulae {PNe} are<br />generally accepted as originating from hydrodynamical interactions between<br />stellar winds: the interacting-stellar wind model {ISW}. Traditionally, the<br />shaping is thought to occur after the star becomes hot enough to ionize the PN.<br />But recent HST images indicate that the shaping may occur earlier, and the newer<br />GISW model puts the shaping during the pre-planetary nebula evolution. The<br />relative importance of both models is not known: GISW shaping will account for<br />some fraction of PNe, but estimates range from 15--100 during the PN phase,<br />especially for the youngest PNe. We here propose an HST SNAPshot survey of<br />compact PNe in the Galactic Bulge, to test these predictions. The Bulge provides<br />the only PNe population for which progenitor masses are known and nebular ages<br />can be measured. In support of these HST measurements we have already measured<br />velocity fields and emission line fluxes. The survey will give an unbiassed<br />sampling of morphologies, and allow evolutionary sequences to be determined to<br />test the ISW versus the GISW model. By-products of the survey will be the<br />determination of nebular masses, diameters and filling factors. We will also<br />obtain the White Dwarf mass distribution in the Bulge, and the initial-final<br />mass function for low-mass stars.<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 9337<br /><br />Critical spectroscopic variations in Eta Carinae<br /><br />The very massive, unstable, persistently enigmatic star Eta Carinae has<br />implications for several branches of astrophysics. Despite a series of<br />remarkable discoveries in previous HST data, the nature of the central object<br />remains elusive. Fortunately, recent developments offer, for the first time, an<br />approach that can settle a number of long-standing questions which have been<br />obstacles to understanding this unique object. A 5.5-year spectroscopic and<br />X-ray cycle is now well established. STIS provides the most promising and very<br />likely the only way to test whether Eta Car is a 5.5-year binary system. If it<br />is, STIS gives by far the best constraints on the companion star, orbit, etc.,<br />needed to assess mechanisms for past outbursts and ejecta. If binary models<br />don't work, then the 5.5-yr effect is probably a thermal cycle which gives novel<br />information about the star's structure. In addition to the periodicity, the<br />unprecedented brightening found with STIS in 1999 has continued at a diminished<br />rate and merits follow up observations. We sense that these recently discovered<br />effects offer a likely breakthrough if Eta Car can be observed repeatedly with<br />STIS through the current 5.5-year period, 1998.0--2003.5. During HST Cycle 10<br />the pace is expected to increase as this object enters the phase preceding its<br />next major ``event.''<br /><br />STIS 9619<br /><br />Echelle Blaze Shift vs. MSM Monthly Offset<br /><br />In the near future, monthly MSM offsets will probably be disabled for STIS<br />echelle gratings, alleviating to some extent calibration problems associated<br />with the monthly offsets. The data from this program will be used to improve<br />empirical and optical models relating wavelength and blaze function shifts.<br />These models will in turn be used to improve the calibration of archival echelle<br />data obtained while monthly MSM offsets were enabled. The flux standard HZ43<br />will be observed with the E230H echelle grating at a central wavelength of 2513<br />Angstroms. Five exposures will be obtained, each with a different monthly offset<br />applied to the Mode Select Mechanism {MSM}.<br /><br />STIS 9554<br /><br />Unveiling the origin of post-AGB winds through STIS data<br /><br />The impact of fast, collimated jets on the spherical and slowly expanding<br />circumstellar envelopes of AGB stars, is believed to be responsible for the<br />remarkable bipolarity and high axial-velocities observed in most post-AGB<br />objects {protoplanetary and planetary nebulae}. We have recently discovered<br />inner, post-AGB jets in the prototype protoplanetary nebula He 3-1475, through a<br />preliminary analysis of STIS long-slit spectra. The high-spatial resolution<br />achieved by the HST and the spectroscopic capabilities of STIS have allowed us<br />for the first time to study the spatio-kinematic structure of post-AGB jets in<br />the stellar vicinity, before they have been strongly altered by the interaction<br />with the AGB shell. Such a study is crucial for understanding the {unknown}<br />mechanism that powers and collimate the winds of post-AGB stars. We request<br />funding to perform a comprehensive study of the STIS spectra for the whole set<br />of slits and gratings available for He 3-1475 and another well studied PPN, HD<br />44179. A preliminary inspection of the data reveals also in this source, a fast,<br />bipolar outflow at ~ 40 A.U. from the star. This is the first time that post-AGB<br />winds are seen at such small scale. A detailed analysis of the STIS data is<br />needed to tightly constraint the physical properties of the post-AGB jets and,<br />ultimately, to understand their origin.<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 8908<br /><br />CCD Imaging Flats C10.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to investigate<br />flat-field stability over a monthly period.<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 9280<br /><br />X-Ray Imaging of GPS and CSS Quasars.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to conduct a survey of<br />GPS and CSS radio-loud quasars, by studying their arcsecond structure in the<br />X-rays, by searching for X-ray jets, and by searching for signatures of<br />intermittent AGN activity.<br /><br />WF/PC-2 9043<br /><br />Cepheid Distances to Early-type Galaxies.<br /><br />The WF/PC-2 was used to continue observations in the HST Key Project on the<br />Extragalactic Distance Scale and the HST project on the "Calibration of Nearby<br />Type Ia Supernovae'' that have greatly improved our knowledge of the Hubble<br />Constant by providing a solid zero point for the Tully- Fisher {TF} relation and<br />Type Ia Supernovae {SNIa}. However, severe inconsistencies remain for distance<br />estimators to early-type galaxies such as surface brightness fluctuations {SBF},<br />the planetary nebula luminosity function {PNLF}, the fundamental plane {FP}, and<br />the globular cluster luminosity function {GCLF}. As a result, the distance to<br />the Virgo cluster core remains uncertain by as much as 20 determination is<br />directly affected by a lingering 0.1 mag {5 uncertainty in the photometric<br />calibration of the WFPC2. Resolving these issues is essential not only to firm<br />up the extragalactic distance scale, but also to understand the mass and<br />velocity structure of the local universe. SBF in particular is emerging as the<br />method of choice for mapping local velocity fields to 10, 000 kms because it<br />offers an order of magnitude less Malmquist bias than TF, and SNIa are too rare<br />to study large scale flows effectively. This project will tighten the<br />photometric calibration of the WFPC2, and provide a solid Cepheid calibration<br />for SBF and PNLF.<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 />WF/PC-2 9107<br /><br />The Fundamental Plane for Nuclear Black Holes.<br /><br />The WF/PC-2 was used to conduct more in-depth searches for supermassive black<br />holes in galaxy centers. Previous work has led to the discoveries that {1} most<br />or all hot galaxies contain massive dark objects at their centers, presumably<br />black holes; {2} there is a remarkably tight correlation between the black-hole<br />mass and the luminosity-weighted velocity dispersion of the hot component of the<br />galaxy. This mbh-Sigma relation has a scatter which is <0.3 dex in mbh and<br />consistent with zero. This relationship suggests a strong link between<br />black-hole formation, AGN activity, and galaxy formation, and once it is<br />understood this link should advance our understanding of all three processes.<br />The goal of this proposal is to investigate the scatter in the mbh-Sigma<br />relation and the role of possible second parameters, by examining a sample of<br />galaxies at fixed velocity dispersion Sigma=200+/- 20 kms. This approach<br />decouples the effects of a second parameter from uncertainties in the shape of<br />the mbh-Sigma relation, and minimizes spurious correlations because all of the<br />galaxies will be studied using the same well-tested observational and modeling<br />techniques.<br /><br />WFPC2 9310<br /><br />Cycle 10 WFPC2 Flood Preflash Test<br /><br />The data from this new proposal will allow an assessment of the effect of a<br />super-preflash, such as the one suggested by Janesick {Scientific Charge-Coupled<br />Devices, James R. Janesick, SPIE Press Monograph, 2001}, on the CTE performance<br />of WFPC2. Previous WFPC2 preflash calibration programs have successfully tested<br />the effects of relatively low preflashes {or fat zeros} on the CTE, in order to<br />determine the optimum level at which the CTE problems are minimized. Typical<br />preflash exposures from these proposals added 50-10000 electrons. However, in<br />his new book, Janesick {2001} suggests that radiation-induced traps can not be<br />completely eliminated with low-level preflashes, that such a preflash merely<br />exposes the incoming photons to new traps. Instead, he recommends the use of a<br />light flood, effectively super-preflashing the chips to levels 2-3 times full<br />well, reading out the preflash, then taking external images.<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. FLIGHT OPERATIONS<br />SUMMARY:<br /><br />HSTARS: [For details see ]http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf]<br /><br />8724 Minor Frames on A/string took a Hit @ 184/04:14:36z. At 184/04:14:36z the<br /> Idoc noticed a message on the A/string events page. It said "Fep R/T SCT<br /> rollback: Previous = 2002.184/04:14:35, current = 2002.184/02:58:48." The<br /> Fot also saw the message so I contacted the RT [George]. After checking,<br /> george called back and related to us that the minor frames that came down<br /> took a hit in communication and also had a bad SCT time. He, however saw<br /> where it corrected itself and now has the correct SCT time. George also did<br /> say that the string is presently healthy and he will look more in depth at<br /> it at day light.Under investigation.<br /><br />8725 LGA Switch During Fwd Link SMS189 @ 184/00:00:00z.Products delivered for<br /> SMS189 contained LGA/Receiver switch during MA Forward link<br /> at 02.192 22:42:10. Under investigation.<br /><br />8726 e-cycle of AppServer_A icon on patrol @ 185/03:03:00z.Danny Ly re-cycled<br /> the scheduler request manager after the process count went from 1 to 40 and<br /> this resolved nothing. Then at 185/0303z the IDOC re-cycled the AppServer_A.<br /> This was all done per what Arnold Philips told us to do. Paul Bissot told<br /> me to make it clear that there was no way to run the job unless the queue<br /> was removed. Arnold saved the job queue off to side. Under investigation.<br /><br />8727 GSACQ[3,2,2] Fine Lock Backup on FGS 3 @ 186/04:05:39z. GSACQ[3,2,2] at<br /> 186/04:02:21 resulted in fine lock back-up on FGS 3 due to search radius<br /> limit exceeded on FGS 2 at 04:05:39. A second acquisition attempt resulted<br /> in scan step limit exceeded on FGS 3 at 04:07:06. An additional search radius<br /> limit exceeded flag occurred on FGS 2 at 04:08:41. Three subsequent REACQ's<br /> also failed to Fine Lock Backup on FGS 3. Two 486 status buffer messages were<br /> received, A07 "FGS coarse track failed, timed out waiting for data valid", and<br /> A05 "FGS coarse track failed, search radius limit exceeded". Under investigation.<br /><br /> ******Observations affected: WFPC 190 to 227, NICMOS 225 to 234, STIS 160 to 162,<br /> ACS 154 to 155.<br /><br />8728 COMMAND ERROR @ 187/16:50:02z. In the process of commanding the<br /> spacecraft for SSR 1 playback, procedure completed, then received<br /> command error [DSDCMDER]. Reason unknown. Had just completed one<br /> playback and was starting another playback on SSR 1. Under investigation.<br /><br />8729 Unable to access CCS from externally @ 188/00:00:00z.Attempted to access<br /> CCS version 3.5.0.0.71 from home on CCS "A" String. Desktop showed not time<br /> increment. DW submittal yielded following error message: Failed to submit<br /> request. Exception type is: class.java.net.UnknolwnHost.Exception.<br /> Exception text is vibi02.ccs.hst.nasa.gov. Verified via CCS string status web<br /> page that "A" String was listed as current prime operational string. Additionally,<br /> verified with STOCC SS. Under investigation.<br /><br />8730 C string recycle @ 188/20:07:00z.CCS "C" Re-cycled @ 188/20:07Z per Response<br /> Team suggestion as a precautionary measure due to their discovery of ISP hits<br /> on the string while excessive real-time minor frame gaps occurred.Under investigation.<br /><br />COMPLETED OPS REQs: None<br /><br />OPS NOTES EXECUTED:<br /><br />0915-1 HSTAR Documentation for FHST Map/Update Failures<br />1021-0 Battery 5 Temperature Limit Adjust<br />0924-0 HSTAR Documentation for Guide Star Acq Failure/Loss of Lock<br />1022-1 ICDZ5BMN limit change<br />0916-0 Tabulation of Slew Attitude Error [Miss-distance]<br /> Guide Star Acquisitions:<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 33 33<br />FGS REacq 39 39<br />FHST Update 65 64 185/07:52:24z<br />LOSS of LOCK None<br /><br />Operations Notes:<br /><br />1. SMS for SA189M00_F1 approved @ 184/1000z.<br />2. ESB code 901 is "FHST Error Box Fail" due to the FHST update failure<br /> @ 185/07:52:24z [no HSTAR required].<br />3. ESB code a07 is "FGS Coarse Track failed - Timed out waiting for<br /> data valid" [HSTAR # 8727].<br />4. ESB code a05 is "FGS Coarse Track failed - Search Radius Limit exceeded<br /> [HSTAR # 8727].<br />5. The CCS-A App Server had to be recycled twice [185/0320 & 185/1200z] to<br /> restore function. This impacts scheduled historical event extracts.<br /> [Ref: HSTAR # 8726].<br /><br />SIGNIFICANT EVENTS: None