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Daily 3535
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3535 PERIOD COVERED: DOY 20 OBSERVATIONS SCHEDULED ACS 9984 Cosmic Shear With ACS Pure Parallels Small distortions in the shapes of background galaxies by foreground mass provide a powerful method of directly measuring the amount and distribution of dark matter. Several groups have recently detected this weak lensing by large-scale structure, also called cosmic shear. The high resolution and sensitivity of HST/ACS provide a unique opportunity to measure cosmic shear accurately on small scales. Using 260 parallel orbits in Sloan textiti {F775W} we will measure for the first time: beginlistosetlength sep0cm setlengthemsep0cm setlength opsep0cm em the cosmic shear variance on scales 0.7 arcmin, em the skewness of the shear distribution, and em the magnification effect. endlist Our measurements will determine the amplitude of the mass power spectrum sigma_8Omega_m^0.5, with signal-to-noise {s/n} ~ 20, and the mass density Omega_m with s/n=4. They will be done at small angular scales where non-linear effects dominate the power spectrum, providing a test of the gravitational instability paradigm for structure formation. Measurements on these scales are not possible from the ground, because of the systematic effects induced by PSF smearing from seeing. Having many independent lines of sight reduces the uncertainty due to cosmic variance, making parallel observations ideal. ACS/HRC/WFC 10059 CCD Daily Monitor This program consists of basic tests to monitor, the read noise, the development of hot pixels and test for any source of noise in ACS CCD detectors. This programme will be executed once a day for the entire lifetime of ACS. ACS/HRC/WFC 9863 Evolution of Young Stellar Outflows: XZ Tauri and HH 30 Our understanding of jet physics, whether at small {young stellar outflows} or large {galactic outflows} scales is reflected by our ability to model the dynamics of the interaction of a jet with its surroundings and itself. These models must be constrained by observations, which have typically shown slow, long-timescale changes. However, a unique opportunity to examine rapidly varying jet dynamics is available with an established history. XZ Tauri and HH 30 represent two substantially different young stellar outflows that have been simultaneously imaged by HST/WFPC2 over 6 epochs spanning 7 years. XZ Tau is a binary T Tauri system in which both stars are jet sources and have somehow created an amazing outflow that has undergone dramatic changes {turn-on of limb brightening, deceleration, interactions with the collimated stellar jets}. In comparison, the textbook protostellar disk of HH 30 emits a well-collimated, knotty bipolar jet, in which motions and knot mergers can be measured over timescales as short as a year. We wish to continue yearly monitoring of this unique field with ACS/WFC, and apply hydrodynamic jet models to reproduce the observations. ACS/HRC/WFC/STIS/CCD 9836 The role of dark matter and intracluster gas in galaxy formation and cluster evolution We propose a fully-sampled mosaic of 41 ACS images to survey galaxy morphologies and measure weak lensing signals to the turn-around radius in the X-ray luminous cluster, MS0451-03 {z=0.54}. The aim is to isolate the physical processes which affect the evolution of cluster galaxy morphologies in the context of well-defined dynamical system. The study will be used in contrast to a successful campaign undertaken in Cycle 9 on a optically-selected target. By comparing morphologies with spectroscopic and Chandra X-ray data, we will quantify the role of the intracluster medium and associated substructures and establish the timescales and physical regions within which the various environmental processes occur. ACS/WFC/WFPC2 9825 An ACS/WFC H-alpha Survey of the Orion Nebula We propose to survey nearly 500 square arcminutes of the Orion Nebula in H-alpha using the ACS/WFC, increasing the sky coverage by an order of magnitude over the sum of all previous HST observations. This survey will, for the first time, sample the majority of young stars and circumstellar environments in the extended Trapezium cluster of 2, 000 low-mass stars. Our primary goal is to determine the survival rate and statistical properties of protoplanetary disks in the type of radiation field and dynamical environment in which most stars are born. The survey will be used to search for new silhouette disks, bright proplyds, microjets, large-scale outflows, and to characterize the properties of these objects as a function of location in the nebula. We will determine accurate proper motions in regions where previous HST data exist. However, 90% of our fields will be observed with HST for the first time. This survey will provide the first complete census of pre-main sequence objects and outflows in an HII region and will constrain the extent of hazards to planet formation in such environments. The images will also provide a legacy for future stellar and nebular variability studies and proper motion measurements by providing a first epoch data base. NIC/NIC3 9865 The NICMOS Parallel Observing Program We propose to continue managing the NICMOS pure parallel program. Based on our experience, we are well prepared to make optimal use of the parallel opportunities. The improved sensitivity and efficiency of our observations will substantially increase the number of line-emitting galaxies detected. As our previous work has demonstrated, the most frequently detected line is Halpha at 0.7z1.9, which provides an excellent measure of current star formation rate. We will also detect star-forming and active galaxies in other redshift ranges using other emission lines. The grism observations will produce by far the best available Halpha luminosity functions over the crucial--but poorly observed--redshift range where galaxies appear to have assembled most of their stellar mass. This key process of galaxy evolution needs to be studied with IR data; we found that observations at shorter wavelengths appear to have missed a large fraction of the star-formation in galaxies, due to dust reddening. We will also obtain deep F110W and F160W images, to examine the space densities and morphologies of faint red galaxies. In addition to carrying out the public parallels, we will make the fully reduced and calibrated images and spectra available on-line, with some ground-based data for the deepest parallel fields included. NIC2 9752 A Search for the Exciting Sources in OMC-1 through NICMOS Polarization Measurements Orion contains the site of the nearest region of massive star formation to the Sun; only here can this pivotal process in galactic evolution be studied at the highest resolution. There are 10^5 solar luminosities of radiation emitted from the Orion Molecular Cloud {OMC-1}, possibly from a young massive star or protostar, or possibly from several, less luminous sources. Either way, the powering source{s} in the closest site of massive star formation has still not yet been identified. Here we propose to apply a new tool to determine which, of several prospective sources, might prove to be the heart of OMC-1. The sources cannot be seen directly because they lie in, or behind, a warm, dense molecular cloud. However, their presence can be inferred in polarized light, through the manner in which light is scattered off neighboring clouds. Heretofore, the spatial resolution has not been adequate to identify the locations of individual stars. We propose to use the NICMOS polarizers combined with the high spatial resolution of HST to achieve this, in spite of the high density of candidate objects in the core of Orion. The demands of accurately measuring the polarization vectors of small, diffuse objects relative to the surrounding background from dust-scattered light requires the high Strehl ratio and stable point-spread function only achievable from space. NICMOS 8791 NICMOS Post-SAA calibration - CR Persistence Part 2 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. The keyword 'USEAFTER=date/time' will also be added to the header of each POST-SAA DARK frame. The keyword must be populated with the time, in addition to the date, because HST crosses the SAA ~8 times per day so each POST-SAA DARK will need to have the appropriate time specified, for users to identify the ones they need. Both the raw and processed images will be archived as POST-SAA DARKSs. Generally we expect that all NICMOS science/calibration observations started within 50 minutes of leaving an SAA will need such maps to remove the CR persistence from the science images. Each observation will need its own CRMAP, as different SAA passages leave different imprints on the NICMOS detectors. STIS/CCD 10017 CCD Dark Monitor-Part 1 Monitor the darks for the STIS CCD. STIS/CCD 10019 CCD Bias Monitor - Part 1 Monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4, to build up high-S/N superbiases and track the evolution of hot columns. STIS/CCD 10085 STIS Pure Parallel Imaging Program: Cycle 12 This is the default archival pure parallel program for STIS during cycle 12. STIS/CCD/MA1 9797 Far-UV Spectrum and Pulsations of PSR 0656+14: Thermal vs. Nonthermal The brightest middle-aged pulsar PSR 0656+14 has been studied at near-IR/optical/near-UV and X-ray wavelengths. Its multiwavelength spectral distribution indicates that both surface thermal emission and nonthermal magnetospheric processes are contributing to the observed radiation. To separate the thermal and nonthermal components and investigate their properties, we propose to study the spectrum and pulsations of the pulsar with the STIS/FUV-MAMA detector in the wavelength range 1150--1700 AA, where it has never been observed. Combined with the previous HST and X-ray measurements of this pulsar, this study will go a long way toward quantifying thermal evolution of neutron stars, constraining the composition and equation of state of the superdense matter in the neutron star interiors, and understanding the acceleration and radiation mechanisms in pulsar magnetospheres. STIS/CCD/MA1 9874 Probing IGM Phases, Metals, and the Cosmic Web with New SDSS QSOs We propose STIS G140L SNAPSHOT observations of 100 new z 1 QSOs from the Sloan Digital Sky Survey for studies of the IGM. These targets will be chosen to simultaneously maximize IGM pathlength and to form closely spaced groups of 2-8 QSO sightlines within 1 h^-1 Mpc of a foreground galaxy. These observations will, in the long term, provide a rich database of target QSOs for detailed study by COS of the IGM phases, metallicity, and relationship to the large scale structure. In the near term, these observations will detect up to 10 Lyman alpha clouds with N_HI 10^14 and 3 clouds with N_HI 10^15, per target. Thus they will provide an immediate test of filamentary structure in the "cosmic web" within 1 h^-1 Mpc of galaxies. We ask for 22 minute exposures for each target with STIS/G140L to obtain S/N = 5-16 for these V = 16 - 18 QSOs. These observations will be sensitive to Lyman alpha equivalent widths ranging from 300 mA for the brighter sources to 600 mA at the fainter end. These targets represent a Deltaz pathlength of 17 {at 50% yield}, with Deltaz = 10 in the range where Lya, Lyb, and O VI lie in the HST band. These observations will also refine predictions of the FUV flux of QSOs based on the larger SDSS sample and will estimate the degree to which such factors as intrinsic and Galactic extinction, variability, and intervening absorption can be controlled. If successful, this technique could make UV-prequalification SNAPs of QSOs obsolete, at a significant savings of HST time. Our observations lie at the median duration for SNAPs, and in the range most likely to be executed. Our program accomplishes both near- and long-term goals at a relatively low investment of time, and thus is ideally suited for a SNAP proposal. To ensure maximum scientific return for our own purposes and for additional science {HVCs, Galactic halo} we waive the right to a proprietary data period. STIS/MA1 10034 Cycle 12 MAMA Dark Monitor This test performs the routine monitoring of the MAMA detector dark noise. This proposal will provide the primary means of checking on health of the MAMA detectors systems through frequent monitoring of the background count rate. The purpose is to look for evidence of change in dark indicative of detector problem developing. STIS/MA1 10083 HST UV Images of Saturn's Aurora Coordinated with Cassini Solar Wind Measurements A key measurement goal of the Cassini mission to Saturn is to obtain simultaneous solar wind and auroral imaging measurements in a campaign scheduled for Jan. 2004. Cassini will measure the solar wind approaching Saturn continuously from 9 Jan. - 6 Feb., but not closer to Saturn due to competing spacecraft orientation constraints. The only system capable of imaging Saturn's aurora in early 2004 will be HST. In this community DD proposal we request the minimum HST time needed to support the Cassini mission during the solar wind campaign with UV images of Saturn's aurora. Saturn's magnetosphere is intermediate between the "closed" Jovian case with large internal sources of plasma and the Earth's magnetosphere which is open to solar wind interactions. Saturn's aurora has been shown to exhibit large temporal variations in brightness and morphology from Voyager and HST observations. Changes of auroral emitted power exceeding one order of magnitude, dawn brightenings, and latitudinal motions of the main oval have all been observed. Lacking knowledge of solar wind conditions near Saturn, it has not been possible to determine its role in Saturn's auroral processes, nor the mechanisms controlling the auroral precipitation. During Cassini's upcoming approach to Saturn there will be a unique opportunity to answer these questions. We propose to image one complete rotation of Saturn to determine the corotational and longitudinal dependences of the auroral activity. We will then image the active sector of Saturn once every two days for a total coverage of 26 days during the Cassini campaign to measure the upstream solar wind parameters. This is the minimum coverage needed to ensure observations of the aurora under solar wind pressure variations of more than a factor of two, based on the solar wind pressure variations measured by Voyager 2 near Saturn on the declining phase of solar activity. The team of proposers has carried out a similar coordinated observing campaign of Jupiter during the Cassini flyby, resulting in a set of papers and HST images on the cover of Nature on 28 February 2002. STIS/MA1 9790 Separating Activity and Accretion in T Tauri Stars Due to their unique evolutionary state, the naked {non-accreting} T Tauri stars {NTTS} are the only real proxies for what the underlying magnetically active star of a classical TTS {CTTS} system looks like. Comparative analysis then allows us to separate stellar properties from accretion properties in CTTS. In addition, the late-type NTTS are excellent candidates for studying rotation-activity relationships in fully convective stars and probing the properties of turbulent dynamos. With the limited data currently available, NTTS appear to be very magnetically active stars with higher than expected H-alpha/X-ray flux ratios but lower transition region fluxes relative to other active stars. However, the data are very incomplete. We will use HST-STIS observations of transition region line fluxes on 11 fully convective NTTS to establish the level and structure of dynamo generated emission in these young stars. In principal, these far ultraviolet emission lines are sensitive diagnostics of mass accretion onto CTTS, since accretion shocks on the stellar surface should produce substantial emission measure at 10^5 - 10^6 K. However, it is imperative that we first understand the emissions from NTTS before we can use these lines to study accretion onto CTTS. WFPC2 10069 WFPC2 CYCLE 12 Supplemental Darks, Part 1/3 This dark calibration program obtains 3 dark frames every day to provide data for monitoring and characterizing the evolution of hot pixels. WFPC2 10084 WFII parallel archive proposal This is the generic target version of the WFPC2 Archival Pure Parallel program. The program will be used to take parallel images of random areas of the sky, following the recommendations of the 2002 Parallels Working Group. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) None COMPLETED OPS REQs: None OPS NOTES EXECUTED: None SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 11 11 FGS REacq 4 4 FHST Update 21 21 LOSS of LOCK SIGNIFICANT EVENTS: None |
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