HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3214<br /><br />PERIOD COVERED: DOY 276<br /><br />OBSERVATIONS SCHEDULED<br /><br />NICMOS 8791<br /><br />NICMOS Post-SAA calibration - CR Persistence Part 2<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. The keyword 'USEAFTER=date/time' will also be added to the<br />header of each POST-SAA DARK frame. The keyword must be populated with the time,<br />in addition to the date, because HST crosses the SAA ~8 times per day so each<br />POST-SAA DARK will need to have the appropriate time specified, for users to<br />identify the ones they need. Both the raw and processed images will be archived<br />as POST-SAA DARKSs. Generally we expect that all NICMOS science/calibration<br />observations started within 50 minutes of leaving an SAA will need such maps to<br />remove the CR persistence from the science images. Each observation will need<br />its own CRMAP, as different SAA passages leave different imprints on the NICMOS<br />detectors.<br /><br />STIS/MA1 8921<br /><br />MAMA Fold Distribution.<br /><br />The Space Telescope Imaging Spectrograph [MA1] was used to monitor the<br />performance of MAMA microchannel plates using a MAMA fold analysis procedure.<br />The fold analysis provides a measurement of the distribution of charge cloud<br />sizes incident upon the anode giving some measure of changes in the pulse-height<br />distribution of the MCP and, therefore, MCP gain.<br /><br />STIS/CCD/MA1 9184<br /><br />A Survey for Missing Baryons in Highly Ionized Intergalactic Gas at Low<br />Redshift.<br /><br />The Space Telescope Imaging Spectrograph [CCD and MA1] was used to observe six<br />additional low-z QSOs with the STIS FUV E140M echelle mode {7 km s^-1<br />resolution}. Combined with archival data, this will increase the sample redshift<br />path by a factor of ~7 compared to the published data. With the echelle data, we<br />will {1} measure the number of O VI absorbers per unit redshift {dN/dz} and<br />their minimum cosmological mass density with a limiting equivalent width of<br />W_Lambda ~50 mAngstrom , {2} examine whether the O VI absorption arises in<br />photoionized, collisionally ionized, or multiphase gas, and {3} study the<br />dependence of the O VI system properties on environment. In addition to testing<br />this prediction regarding the location of the missing baryons, the data will<br />have applications to many other topics such as low-z LyAlpha absorbers and the<br />physical properties and abundances of gas in the Milky Way halo.<br /><br />NICMOS 9386<br /><br />Infrared Photometry of a Statistically Significant Sample of KBOs<br /><br />While the discovery rate of Kuiper Belt objects is accelerating, the physical<br />study of this new region of the solar system has been slowed by a lack of basic<br />astrophysical data. Photometric observations of the majority of the more than<br />400 known KBOs and Centaurs are rudimentary and incomplete, particularly in the<br />infrared. The multicolor optical-infrared photometry that exists for a small<br />subset of KBOs often shows significant discrepancies between observations by<br />different observers. Their intrinsic faintness puts them at the practical limits<br />of ground-based systems. In July 2001 we began what will be the largest uniform<br />sample of optical photometry of KBOs with a WFPC2 SNAPSHOT program that will<br />perform accurate photometry at V, R, and I on a sample of up to 150 targets. We<br />seek to greatly enhance the value of this survey by obtaining J and H photometry<br />on the same sample using NICMOS. Combined optical and infrared broad band<br />photometry is a far more powerful tool for physical studies than is either<br />alone. Our sample includes objects that will be observed at thermal infrared<br />wavelengths by SIRTF and will be used with those data to derive the first<br />accurate diameters, albedos, and surface properties for a large sample of KBOs.<br /><br />ACS/HRC 9391<br /><br />High-Resolution Imaging of Pluto's Surface<br /><br />We will collect a series of observations with the ACS/HRC from which we will<br />derive a two-color global map of Pluto's surface. We will image Pluto at F435W<br />and F555W, wavelengths that have been extensively studied from the ground over<br />the past 50 years. The maps will provide albedos with accurate error<br />determinations down to 52 degrees South latitude. These observations will<br />provide a second epoch of HST mapping of the active surface of Pluto as it<br />continues to recede from the Sun and will provide an important context for other<br />detailed studies of Pluto.<br /><br />FGS/1 9407<br /><br />Astrometry of a Star Hosting an Extrasolar Planet: The Mass of Upsilon<br />Andromedae.<br /><br />axis and inclination} produced by the outermost extra-solar planet orbiting the<br />F8V star Upsilon Andromedae. These observations will permit us to determine the<br />actual mass of the planet by providing the presently unknown sin i factor<br />intrinsic to the radial velocity method which discovered this object. An<br />inclination, i = 30degrees, within the range of one very low precision<br />determination using reanalyzed HIPPARCOS intermediate data products, would<br />produce the observed radial velocity amplitude, K = 66 ms with a companion mass<br />of ~8 M_Jupiter. Such a mass would induce in Upsilon Andromedae a perturbation<br />semi-major axis, Alpha = 0arcs0012. The proposed observations will yield a<br />planetary mass, rather than, as previous investigations have done, only suggest<br />a planetary mass companion.<br /><br />STIS 9435<br /><br />Systematic Search for Rotation at the Base of Outflows from T Tauri Stars<br /><br />We wish to search for rotation signatures in the initial portion {first 100 AU}<br />of a sample of outflows emanating from T Tauri stars {TTSs}. This project<br />originates from our detection of systematic transverse radial velocity shifts in<br />STIS spectra of the DG Tau jet {Bacciotti et al., 2002}. The shifts, observed in<br />a region where the flow is already collimated, but has not yet manifestly<br />interacted with its environment, are consistent with the predictions of magneto-<br />centrifugal launching models, and may constitute the first observed indication<br />for rotation in the initial portion of a jet flow. Rotation is a fundamental<br />ingredient in star formation theories, thus we propose to confirm the above<br />result by carrying out a systematic survey in similar flows. We plan to take for<br />each jet a STIS spectrum in the 6300 -- 6800 Angstrom range, with the slit<br />perpendicular to the flow direction and at a distance of about 0.''3 from the<br />source {i.e., in our targets, 40 -- 70 AU along the jet depending on inclination<br />angle}. Since the flows are resolved transversely with HST, the proposed slit<br />orientation allows for the direct detection of systematic velocity shifts. Where<br />found, we will check for consistency between the sense of rotation observed and<br />that of the underlying disk through CO interferometric measurements. As a<br />by-product, estimates of the excitation conditions across the flow {including<br />ionization fraction} and of the mass outflow rates will be derived.<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 />NICMOS 9484<br /><br />The NICMOS Parallel Observing Program<br /><br />We propose to manage the default set of pure parallels with NICMOS. Our<br />experience with both our GO NICMOS parallel program and the public parallel<br />NICMOS programs in cycle 7 prepared us to make optimal use of the parallel<br />opportunities. The NICMOS G141 grism remains the most powerful survey tool for<br />HAlpha emission-line galaxies at cosmologically interesting redshifts. It is<br />particularly well suited to addressing two key uncertainties regarding the<br />global history of star formation: the peak rate of star formation in the<br />relatively unexplored but critical 1<= z <= 2 epoch, and the amount of star<br />formation missing from UV continuum-based estimates due to high extinction. Our<br />proposed deep G141 exposures will increase the sample of known HAlpha emission-<br />line objects at z ~ 1.3 by roughly an order of magnitude. We will also obtain a<br />mix of F110W and F160W images along random sight-lines to examine the space<br />density and morphologies of the reddest galaxies. The nature of the extremely<br />red galaxies remains unclear and our program of imaging and grism spectroscopy<br />provides unique information<br /><br />regarding both the incidence of obscured star bursts and the build up of stellar<br />mass at intermediate redshifts. In addition to carrying out the parallel program<br />we will populate a public database with calibrated spectra and images, and<br />provide limited ground- based optical and near-IR data for the deepest parallel<br />fields.<br /><br />NICMOS 9485<br /><br />Completing A Near-Infrared Search for Very Low Mass Companions to Stars within<br />10 pc of the Sun<br /><br />Most stars are fainter and less massive than the Sun. Nevertheless, our<br />knowledge of very low mass {VLM} red dwarfs and their brown dwarf cousins is<br />quite limited. Unknown are the true luminosity function {LF}, multiplicity<br />fraction, mass function, and mass-luminosity relation for red and brown dwarfs,<br />though they dominate the Galaxy in both numbers and total mass. The best way to<br />constrain these relations is a search for faint companions to nearby stars. Such<br />a search has several advantages over field surveys, including greater<br />sensitivity to VLM objects and the availability of precise parallaxes from which<br />luminosities and masses can be derived. We propose to complete our four-filter<br />NICMOS snapshot search for companions to stars within 10 pc. With a 10 sigma<br />detection limit of M_J ~ 20 at 10 pc, we can detect companions between 10 and<br />100 AU that are at least 9 mag fainter than the empirical end of the main<br />sequence and at least 6.5 mag fainter than the brown dwarf Gl 229B. When<br />completed, our search will be the largest, most sensitive, volume-limited search<br />for VLM companions ever undertaken. Our four-filter search will permit<br />unambiguous identification of VLM-companion candidates for follow-up<br />observation. Together with IR speckle and deep imaging surveys, our program will<br />firmly establish the LF for VLM companions at separations of 1-1000 AU and the<br />multiplicity fraction of all stars within 10 pc.<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 />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 />WFPC2 9593<br /><br />WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt1/3<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 />CAL/WF2 9597<br /><br />Intflat Sweep, Visflat Sweep, and Filter Anomaly Check<br /><br />No abstract available.<br /><br />STIS 9605<br /><br />CCD Dark Monitor-Part 1<br /><br />Monitor the darks for the STIS CCD<br /><br />STIS 9607<br /><br />CCD Bias Monitor - Part 1<br /><br />Monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1<br />at gain = 4, to build up high-S/N superbiases and track the evolution of hot<br />columns.<br /><br />STIS 9633<br /><br />STIS parallel archive proposal - Nearby Galaxies - Imaging and Spectroscopy<br /><br />Using parallel opportunities with STIS which were not allocated by the TAC, we<br />propose to obtain deep STIS imagery with both the Clear {50CCD} and Long-Pass<br />{F28X50LP} filters in order to make color-magnitude diagrams and luminosity<br />functions for nearby galaxies. For local group galaxies, we also include G750L<br />slitless spectroscopy to search for e.g., Carbon stars, late M giants and S-type<br />stars. This survey will be useful to study the star formation histories,<br />chemical evolution, and distances to these galaxies. These data will be placed<br />immediately into the Hubble Data Archive.<br /><br />ACS 9647<br /><br />CCD Daily Monitor Part I<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 9656<br /><br />Stability of the ACS CCD: geometry, flat fielding, photometry<br /><br />A moderately crowded stellar field, located ~6' West of the centre of the<br />cluster 47 Tuc, is observed repeatedly {every three weeks with the WFC, every<br />other month with the HRC} in various filters, spending 1 orbit per epoch.<br />Different filters will be used every time, so that over the course of the year<br />all filters will have been employed at least twice. The most common filters will<br />be checked more frequently. The same field has been observed in the course of<br />the SMOV phase and the positions and magnitudes of the most prominent stars have<br />been accurately measured. Although the field is neither a proper astrometric nor<br />a proper photometric standard one, the positions and magnitudes of the objects<br />in it can be used to monitor any local and large scale variations in the<br />platescale and sensitivity of the detectors. It should be noted that for the<br />filters which have already been used during the SMOV phase it will be sufficient<br />to take one single image, without CR-SPLIT, since the exposure time is always<br />short {20-30 sec} and there will be so many stars that the few of them which are<br />affected by cosmic rays can be discarded as outliers in the photometry. For<br />narrow and medium band filters not exercised on this target in the SMOV phase,<br />however, a baseline will have to be set. This expenditure of time will apply to<br />the current cycle only. At variance with the approach used in SMOV, there is no<br />need for large telescope slews to place the same objects on opposite sides of<br />the detectors, thence allowing the programme to remain compact and efficient.<br />All exposure level parameters are set to their default values, except for the<br />amplifier gain of the WFC exposures in the F606W band, which will be collected<br />with the gain value of 2 for the WFC for compatibility with the SMOV<br />observations. The exposure time is typically 30 seconds for the WFC, 60 sec for<br />the HRC. No attempt will be made to attain a predefined or the same orientation<br />on the sky amongst different epochs. Typically, for the WFC, five exposures will<br />be accommodated in one orbit. For the HRC, about 10 exposures can be fitted<br />within one orbit<br /><br />WFPC2 9676<br /><br />POMS Test Proposal: WFII parallel archive proposal<br /><br />This is the generic target version of the WFPC2 Archival Pure Parallel program.<br />The program will be used to take parallel images of random areas of the sky,<br />following the recommendations of the 2002 Parallels Working Group.<br /><br />POMS 9677<br /><br />POMS Test Proposal: WFII backup parallel archive proposal<br /><br />STIS 9692<br /><br />STIS Pure Parallel Imaging Program: Cycle 10<br /><br />FLIGHT OPERATIONS SUMMARY:<br /><br />Significant Spacecraft Anomalies: [The following are preliminary reports of<br />potential non-nominal performance that will be investigated.]<br /><br />HSTAR 8800: GS Acquisition [2,1,1] @ 276/10:18:02Z resulted in FL backup<br />using FGS 1 due to SSLE [QF2SSLEX] on FGS 2. Following FHST Map @ 276/10:50Z s<br />showed errors. The guide star acquisition for this observation was non nominal,<br />further analysis will determine if a repeat observation is required.<br /><br />HSTAR 8801: CCS "B" and "G" Strings HSTPS dump statistics different @ 276/23:30Z.<br />for dumps @ 276/20:02:15Z - 276/20:24:44Z and 276/21:46:15Z - 22:34:45Z. When FOT<br />issued a HSTPS start command on both strings, the messages science data socket<br />connection data accepted and new real-time science data session started were<br />seen only on the "G" String, not on the "B" String. However, the "B" String HSTPS<br />collected the dumps. Re-cycled the system and re-booted the HSTPS.<br /><br />HSTAR 8802: GS Acquisition [2,1,2] @ 277/01:13:32Z, which began during ZOE, resulted<br />in FL back-up on FGS [1,0,1] due to SSLE flag on FGS 2. Prior FHST U1,2FM updates<br />@ 277/01:07:27Z and 277/01:10:12Z were successful with the following axis errors:<br />First Update: V1 = -29.918, V2 = 58.496, V3 = -37.578 and Second Update: V1 = -0.307,<br />V2 = -1.383, V3 = 3.418. The guide star acquisition for this observation was non nominal,<br />further analysis will determine if a repeat observation is required.<br /><br />COMPLETED OPS REQs: None<br /><br />OPS NOTES EXECUTED: None<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 11 11<br />FGS REacq 6 6<br />FHST Update 25 25<br />LOSS of LOCK<br /><br />SIGNIFICANT EVENTS:<br /><br />Successfully completed Command Communication Controller [CCC] Test 276/12:00Z - 13:15Z.<br />Verified all options on the CCC GUI function and the CCC functionality interface with<br />the CCS. At the conclusion of the test, the string was handed over to the FOT for a<br />real-time NCC and command checkout. Successfully transmitted NOOP and FIVEBLCK<br />commands. While returning the string back to Prime Ops, the transition was<br />unsuccessful due to a CCC issue. A Packet Filter flush was executed by the FOT and<br />command capability was moved back to Prime Ops. An HSTAR will be written.<br /><br />Successfully completed Real-time WSC [ANCC] Interface Test 276/14:00Z - 18:40Z.<br />The is the first test with the ANCC since the move to the WSC. Verified CCS 4.0.1<br />capability to send GCMRs and received ODMs for TDRSS SN forward and return link<br />configurations. Although during the test all SSAR DG2 supports failed, HITT later<br />connected the string to the Real-time NCC and successfully captured real-time Cross<br />Service @ 276/22:00Z, verifying CCS Release 4.0.1 capability to interface with the<br />TDRSS SN.<br /><br />'C' string configured for PRIME OPS @ 276/1322z for 4.0.1 IP Command check-out.<br />Sent NOOP and FIVEBLK commands in IP Packet Filter Mode.<br /><br />'B' string configured for PRIME OPS @ 276/1338z<br /><br />'G' string configured for PRIME OPS @ 277/0025z [ref HSTAR # 8801, recycle<br />'B' string]