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Daily 3569
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3569 PERIOD COVERED: DOYs 72-74 OBSERVATIONS SCHEDULED NIC3 9999 The COSMOS 2-Degree ACS Survey NICMOS Parallels The COSMOS 2-Degree ACS Survey NICMOS Parallels. This program is a companion to program 9822. 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. FGS 9879 An Astrometric Calibration of the Cepheid Period-Luminosity Relation We propose to measure the parallaxes of 10 Galactic Cepheid variables. There is no other instrument on or off the earth that can consistently deliver HST FGS level of precision for critical parallaxes. When these parallaxes {with 1-sigma precisions of 10% or better} are added to our recent HST FGS parallax determination of delta Cep {Benedict et al 2002}, we anticipate determining the Period-Luminosity relation zero point with a 0.03 mag precision. In addition to permitting the test of assumptions that enter into other Cepheid distance determination techniques, this calibration will reintroduce Galactic Cepheids as a fundamental step in the extragalactic distance scale ladder. A Period-Luminosity relation derived from solar metallicity Cepheids can be applied directly to extragalactic solar metallicity Cepheids, removing the need to bridge with the Large Magellanic Cloud and its associated metallicity complications. STIS/CCD/MA1 9868 Timing of the proposed optical counterpart of the 16 ms LMC X-ray pulsar PSR J0537-6910 PSR J0537-6910 is a fast, young {~ 5, 000 yrs} X-ray pulsar -still undetected in radio- at the the center of the SNR N157B in the LMC. PSR J0537-6910 is a champion pulsar - with a period of 16 ms it is the fastest rotator among ordinary pulsars, with the sharpest X-ray pulse among young pulsars. It is the most energetic one {together with the Crab}, with a rotational energy loss log{dE/dt} ~ 38.7 erg/s, and its space velocity { 1, 000 km/s}, inferred from the shape of its X-ray bow-shock nebula, is probably one of the highest in the pulsar family. Taking advantage of the refined Chandra position of the X-ray pulsar, we have recently performed multi-band high-resolution imaging with the ACS {GO 9471} and we found a potential counterpart, characterized by unusual colours. Here, we propose to observe the candidate counterpart with the STIS/NUV-MAMA in its TIME-TAG mode to search for pulsations at the X-ray period, which would unambiguously confirm the proposed identification. 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. STIS/CCD/MA1 9848 A SNAPSHOT Survey of Sharp-Lined Early B-Type Stars Although spectrum synthesis studies of the UV spectra of sharp-lined main sequence B stars provide us with some our best determinations of the abundances of the Fe group and neutron capture elements and the chemical evolution in our galaxy and the Magellanic Clouds, the HST archive is virtually devoid of high resolution spectra of the bright nearby B stars that have become to be regarded as abundance standards. For example, there are NO observations of HR 1886, iota Her, and tau Her, the sharpest-lined representatives {V sin i 5 km/s} of spectral classes B1 V, B3 IV-V and B5 IV, and only a few tiny spectral intervals of gamma Peg {B2 IV}. Information on the abundances of the Fe group is important for computing opacities for stellar evolution calculations and for determining astrophysical f-values. There are no suitable galactic standards in the HST database to compare with recent HST/STIS observations of B stars in the Magellanic Clouds and the likely future observations of similar objects in M31 and other nearby galaxies. To correct this deficiency, we propose SNAPSHOT observations with the STIS E140M and E230M gratings of 33 of the best bright abundance standards in nearby clusters and the galactic field. Using this data we will determine the abundances of the Fe group and heavy elements using the technique of spectrum synthesis with LTE and NLTE treatments. We waive the proprietary period. ACS/WFC/WFPC2 9822 The COSMOS 2-Degree ACS Survey We will undertake a 2 square degree imaging survey {Cosmic Evolution Survey -- COSMOS} with ACS in the I {F814W} band of the VIMOS equatorial field. This wide field survey is essential to understand the interplay between Large Scale Structure {LSS} evolution and the formation of galaxies, dark matter and AGNs and is the one region of parameter space completely unexplored at present by HST. The equatorial field was selected for its accessibility to all ground-based telescopes and low IR background and because it will eventually contain ~100, 000 galaxy spectra from the VLT-VIMOS instrument. The imaging will detect over 2 million objects with I 27 mag {AB, 10 sigma}, over 35, 000 Lyman Break Galaxies {LBGs} and extremely red galaxies out to z ~ 5. COSMOS is the only HST project specifically designed to probe the formation and evolution of structures ranging from galaxies up to Coma-size clusters in the epoch of peak galaxy, AGN, star and cluster formation {z ~0.5 to 3}. The size of the largest structures necessitate the 2 degree field. Our team is committed to the assembly of several public ancillary datasets including the optical spectra, deep XMM and VLA imaging, ground-based optical/IR imaging, UV imaging from GALEX and IR data from SIRTF. Combining the full-spectrum multiwavelength imaging and spectroscopic coverage with ACS sub-kpc resolution, COSMOS will be Hubble's ultimate legacy for understanding the evolution of both the visible and dark universe. STIS 9786 The Next Generation Spectral Library We propose to continue the Cycle 10 snapshot program to produce a Next Generation Spectral Library of 600 stars for use in modeling the integrated light of galaxies and clusters. This program is using the low dispersion UV and optical gratings of STIS. The library will be roughly equally divided among four metallicities, very low {[Fe/H] lt -1.5}, low {[Fe/H] -1.5 to -0.5}, near-solar {[Fe/H] -0.3 to 0.1}, and super-solar {[Fe/H] gt 0.2}, well-sampling the entire HR-diagram in each bin. Such a library will surpass all extant compilations and have lasting archival value, well into the Next Generation Space Telescope era. Because of the universal utility and community-broad nature of this venture, we waive the entire proprietary period. STIS/CCD/MA1 9759 Confirmation of New Candidates for the Study of Intergalactic Helium The reionization of intergalactic helium is believed to take place between redshift 3 and 4. The study of HeII Lyman-alpha absorption in four quasars at 2.7z3.3 demonstrates the great potential of such an intergalactic-medium {IGM} probe and suggests that the reionization epoch is at higher redshifts. Clean quasar sightlines may be found only from massive pre-selection processes in the optical and UV, because of random, severe absorption by intervening Lyman-limit systems. The SDSS has discovered approximately 36000 quasars, and we propose to verify the UV detectability in 70 top candidates for helium studies extending to even higher redshift. Our proposed approach has already proven successful, and additional positive confirmations will allow follow-up observations, with STIS or COS, to pinpoint the epoch of reionization of the IGM, and the evolution of its properties near that period. ACS/HRC/WFC/NIC2 9753 Morphologies of EROs and Field Galaxies in SIRTF's First Look Survey: A Rich Early Release Dataset The SIRTF First Look Survey {FLS} will be the first scientific program undertaken with NASA's next Great Observatory. The FLS provides the first large sample of dusty galaxies to redshifts to z 2 and a census of large-scale global IR properties {luminosities, color temperatures, total dust mass, etc.} HST observations to measure morphology are critical to provide insight into the mechanisms which build up the various galaxy components--disks, bulges as well as chaotic morphologies. We will measure quantitative morphology of fifty extremely red objects {EROs} with targeted NICMOS pointings and hundreds of field galaxies with ACS in parallel in the FLS. We aim to understand how EROs fit into the evolutionary sequence of galaxy formation. The combined HST and SIRTF observations will provide clues into the physical processes responsible for generating powerful far-IR sources or, conversely, may explain why some galaxies are inactive in the far-IR. Ancillary ground-based optical, near-IR, and radio data have already been obtained and DEIMOS spectra are scheduled for June, 2003. We waive the proprietary period for the HST observations and if executed early in Cycle 12 the FLS will be the first complete SIRTF+HST survey made available to the astronomical community, well in advance of the majority of the Legacy observations and all of the GTO surveys. STIS/CCD/MA1 9724 Towards a global understanding of accretion physics - Clues from an UV spectroscopic survey of cataclysmic variables Accretion inflows and outflows are fundamental phenomena in a wide variety of astrophysical environments, such as Young Stellar Objects, galactic binaries, and AGN. Observationally, cataclysmic variables {CVs} are particularly well suited for the study of accretion processes. We are currently carrying out a Cycle 11 STIS UV spectroscopic snapshot survey of CVs to fully exploit the diagnostic potential of these objects for our understanding of accretion physics. While the data obtained so far are of excellent quality, the number of targets that will be observed in Cycle 11 is too small for a statistically significant analysis {only 19 objects out of our 149 accepted Cycle 11 snapshot targets have been observed at the time of writing}. We propose here to extend this survey into Cycle 12, building a homogenous database of accretion disc and wind outflow spectra covering a wide range of mass transfer rates and binary inclinations. We will analyze these spectra with state-of-the-art accretion disc model spectra {SYNDISK}, testing our current knowledge of the accretion disc structure, and, thereby, providing new insight into the so far not well understood process of viscous dissipation. We will use our parameterised wind model PYTHON for the analysis of the radiation driven accretion disc wind spectra, assessing the fundamental question whether the mass loss rate correlates with the disc luminosity. In addition, our survey data will identify a number of systems in which the white dwarf significantly contributes to the UV flux, permitting an analysis of the impact of mass accretion on the evolution of these compact stars. This survey will triple the number of currently available high-quality accretion disc / wind outflow / accreting white dwarf spectra, and we waive our proprietary rights to permit a timely use of this database. ACS/WFC 9575 Default {Archival} Pure Parallel Program. The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels in POMS. ACS/WFPC2 9488 Cosmic Shear - with ACS Pure Parallel Observations The ACS, with greater sensitivity and sky coverage, will extend our ability to measure the weak gravitational lensing of galaxy images caused by the large scale distribution of dark matter. We propose to use the ACS in pure parallel {non- proprietary} mode, following the guidelines of the ACS Default Pure Parallel Program. Using the HST Medium Deep Survey WFPC2 database we have measured cosmic shear at arc-min angular scales. The MDS image parameters, in particular the galaxy orientations and axis ratios, are such that any residual corrections due to errors in the PSF or jitter are much smaller than the measured signal. This situation is in stark contrast with ground-based observations. We have also developed a statistical analysis procedure to derive unbiased estimates of cosmic shear from a large number of fields, each of which has a very small number of galaxies. We have therefore set the stage for measurements with the ACS at fainter apparent magnitudes and smaller, 10 arc-second scales corresponding to larger cosmological distances. We will adapt existing MDS WFPC2 maximum likelihood galaxy image analysis algorithms to work with the ACS. The analysis would also yield an online database similar to that in archive.stsci.edu/mds/ 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 8578 First Spectroscopy of an Asteroid and its Satellite: {45} Eugenia and S/1998 {45} 1 We recently made the first-ever discovery of a satellite of an asteroid from the Earth, using adaptive optics {Merline et al. 1999a, 1999b}. We propose here to acquire the first separate, comparative, and simultaneous spectra of an asteroid and its satellite. We will employ the UV-capabilities and high-spatial-resolution properties of STIS to study {45}Eugenia, and its satellite, S/1998{45}1, by obtaining medium-resolution spectra over the range 2900-10300 Angstrom, using only two grating settings, on a single HST orbit. We will determine whether the spectra, and hence surface compositions, are similar or different in a parent-satellite pair, and to test hypotheses concerning satellite production mechanisms. From the orbital parameters, determined using our ground-based adaptive-optics images, we have already determined that {45}Eugenia has a surprisingly low density of 1.2 g cm^-3. We know the spectrum of Eugenia is a {Tholen} FC-type, which is similar to the common C-types, but differs by the lack of a UV-band or UV-dropoff and by subtle, but measurable differences in the spectral slope. Both the UV-region and the existence of subtle absorption features in the near-IR {~ 0.9 micron} are diagnostic of the specific differences between F-, C-, and {Bus'} X-class. HST spectroscopy is the only way to separate the pair, because ground-based adaptive optics is not available in the UV and cannot yet provide adequate resolution in the visible. STIS/CCD 10085 STIS Pure Parallel Imaging Program: Cycle 12 This is the default archival pure parallel program for STIS during cycle 12. 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. WFPC2 10070 WFPC2 CYCLE 12 Supplemental Darks Part 2/3 This dark calibration program obtains 3 dark frames every day to provide data for monitoring and characterizing the evolution of hot pixels. 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. STIS/CCD 10030 STIS/CCD Spectroscopic Sensitivity Monitor for Cycle 12 Monitor sensitivity of each CCD grating mode to detect any change due to contamination or other causes. 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 10017 CCD Dark Monitor-Part 1 Monitor the darks for the STIS CCD. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) HSTAR 9350: GS Acquisition (2,1,2) @ 072/15:22:45Z ended in FL backup on FGS 1 due to QF2STOPF. Prior FHST FM updates both had low errors. Under investigation. COMPLETED OPS REQs: None OPS NOTES EXECUTED: 1208-0 Adjust ACS Error Count Limit @ 073/0619z 1208-1 Adjust ACS Error Count Limit @ 074/0747z 0916-0 Tabulation of Slew Attitude Error (Miss-distance) @ 075/0827z SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 33 33 FGS REacq 11 11 FHST Update 52 52 LOSS of LOCK SIGNIFICANT EVENTS: Executed first commands from CCS SUN "F" String to the HST Observatory @ 072/18:36Z. All 486 and NSSC-1 loads were uplinked from CCS "A". Command transferred from CCS "F" to CCS "D" @ 074/03:50Z, transferred command to CCS "F" @ 075/08:40Z. Test events have been scheduled to verify CCS "H" String, CCS Release 5.0.3.1 capability to successfully support GCMR/ODM traffic. |
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