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Daily 3542
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3542 PERIOD COVERED: DOYs 30-32 OBSERVATIONS SCHEDULED S/C/NIC1/NIC3 9994 NICMOS Focus Stability The purpose of this activity is to determine if the best focus determined in SMOV is stable. This program will execute in approximately one month intervals starting about 1 month after the last execution of proposal 8980. 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 9969 FGS Astrometry of the Extrasolar Planet of Epsilon Eridani We propose observations with HST/FGS in Position Mode to determine the astrometric elements {perturbation orbit semimajor axis and inclination} of the candidate extra-solar planet around the K2 V star Epsilon Eridani that has been detected by Doppler spectroscopy. These observations will also permit us to determine the actual mass of the planet by providing the sin{i} factor which can not be determined with the radial velocity method. High precision radial velocity {RV} measurements spanning the years 1980.8--2000.0 for the nearby {3.22 pc} star Epsilon Eri show convincing variations with a period of ~ 7 yrs. These data represent a combination of six independent data sets taken with four different telescopes. A least squares orbital solution using robust estimation yields orbital parameters of period, P = 6.9 yrs, velocity K- amplitude = 19 m/s, eccentricity e = 0.6, projected companion mass M_B sin{i} = 0.83 M_Jupiter. An estimate of the inclination yields a perturbation semi-major axis, Alpha = 0arcs0022, easily within the reach of HST/FGS astrometry. ACS/HRC/WFC 9919 The Morphological, Photometric, and Spectroscopic Properties of Intermediate Redshift Cluster Galaxies: New and fundamental constraints on the evolutionary state of high redshift clusters will be made by obtaining deep, multiband images {SDSS r, i, z} over the central 1.5 Mpc regions of seven distant clusters in the range 0.76 z 1.27. The ACS data will allow us to {1} definitively establish the morphological composition and star formation rates as functions of clustercentric radius, local density, x-ray luminosity {obtained from accompanying Chandra, and XMM data}, {2} explore the relationship between substructure, kinematics, and morphology, {3} strongly constrain the galaxy merger frequency and the origins of elliptical and S0 galaxies, {4} measure the mass distribution independently from the light {via gravitational lensing} enabling comparisons with kinematically derived masses, and {5} study the evolution of the structure of the brightest cluster members. The clusters selected for this program already have extensive spectroscopic observations and NIR imaging is either in hand or underway from approved ground based programs. To date, the lower part of this redshift range has only been marginally studied with HST. Our sample includes the two most distant, spectroscopically confirmed superclusters and will significantly increase the baseline over which evolutionary effects can be studied. The data will also be used to identify very high-z galaxies via their unique spectral properties. FGS 9883 Parallaxes of Extreme Halo Subgiants: Calibrating Globular Cluster Distances and the Ages of the Oldest Stars The ages of the oldest stars are a key constraint on the evolution of our Galaxy, the history of star formation, and cosmological models. These ages are usually determined from globular clusters. However, it is alternatively possible to determine ages of extreme Population II subgiants in the solar neighborhood based on trigonometric parallaxes, without any recourse to clusters. This approach completely avoids the vexing issues of cluster distances, reddenings, and chemical compositions. There are 3 known nearby, extremely metal-deficient Pop II subgiants with Hipparcos parallax errors of 6-11% which are available for such age determinations. At present, based on the latest isochrones, the derived ages of these stars {HD 84937, HD 132475, and HD 140283} are all close to 14 Gyr, uncomfortably close to or higher than current estimates of the age of the universe. However, the errors in the Hipparcos parallaxes imply uncertainties of at least 2 Gyr in the ages of the 3 stars. We propose to measure parallaxes of these three Pop II subgiants using HST's Fine Guidance Sensor 1R. We expect to reduce the Hipparcos parallax error bars by factors of 5-6, providing the most stringent test yet of current theoretical stellar models of Pop II stars and pushing the age uncertainties to below 0.5 Gyr. These data will also provide a major new constraint on the distance scale of globular clusters, with wide implications for stellar evolution and the calibration of Pop II standard candles. 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. ACS/WFC 9860 ESSENCE: Measuring the Dark Energy Equation of State The accelerating universe appears to be dominated by a dark energy with a significant negative pressure. The ratio of the pressure to density of this mysterious energy {its equation of state} is an observable which can differentiate between the proliferating candidate theories. We propose to estimate the dark energy equation of state by observing Type Ia supernovae at redshifts near z=0.7 with HST in concert with the on-going ESSENCE NOAO Survey program that is discovering and studying supernovae between 0.3z0.8. We show that an interesting constraint on the equation of state can be made with supernovae observed at modest redshifts given the current knowledge of the matter density. We will follow 10 Type Ia supernovae discovered from the ground and passed to HST without disrupting its schedule. The full data set will constrain the equation of state to 10% and strictly limit the range of possible dark energy models. In keeping with the ESSENCE policy, these observations will available to the community immediately. STIS/CCD 9854 Anomalous Flux Ratios in Quadruple Gravitationally Lensed QSOs We propose to observe eight {8} gravitationally lensed systems which exhibit quadruple images of the background high redshift quasars. Models invoking a smooth potential fit the observed image positions accurately, in most cases better than 5 milliarcseconds. But the same models dramatically fail to predict the observed flux ratios. These anomalous flux ratios can be attributed to micro- or milli-lensing in the massive lensing halo. In this proposal, we will isolate the source of the anomalous flux ratios by using the superior resolution of HST/STIS to obtain spectrophotometric data and compare the emission line flux ratio of the QSOs to the continuum flux ratios. Due to the much larger size of the broad emission line regions, the flux ratios in the emission lines should only be affected by milli-lensing if the sub-halos are comparable or larger in projected size than the source region. That is, flux ratios observed in the QSO continuum are senstive to substructure on all scales {both micro- and milli-lensing}, while the broad emission lines are insensitive to micro-lensing due to the larger physical size of the source emission region. This sample of eight quasars will provide the definitive evidence to distinguish between possible sources causing the observed anomalous flux ratios. 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. NIC2 9801 Are OH/IR Stars the Youngest post-AGB stars? A NICMOS Imaging Survey Essentially all well-characterized preplanetary nebulae {PPNe}-- objects in transition between the AGB and planetary nebula evolutionary phases - are bipolar, whereas the mass-loss envelopes of AGB stars are strikingly spherical. In order to understand the processes leading to bipolar mass-ejection, we need to know at what stage of stellar evolution does bipolarity in the mass-loss first manifest itself. We have recently hypothesized that most OH/IR stars {evolved mass- losing stars with OH maser emission} are very young PPNe. We are conducting a multiwavelength survey program of imaging and spectroscopic observations of such objects, using a large, morphologically unbiased sample selected using IRAS 12-to-25 micron colors. Our ongoing HST/SNAP imaging survey of the optically bright half of this sample with WFPC2 and ACS is highly successful: 19/32 objects observed are extended with bipolar/multipolar shapes {remaining objects are unresolved}. Slightly more than 50% of our sample are optically too faint or undetected but have strong near-IR counterparts -- we therefore propose a NICMOS SNAPshot imaging survey of these optically-faint OH/IR stars. These observations are crucial for determining how and when the bipolar geometry asserts itself. The results from our NICMOS survey {together with the WFPC2/ACS survey} will allow us to draw general conclusions about the onset of bipolar mass-ejection during late stellar evolution. Our complementary program of interferometric mapping of the OH maser emission in our sources is yielding kinematic information with spatial resolution comparable to that in the HST images. The HST/radio data will provide crucial input for theories of post-AGB stellar evolution. In addition, these data will also indicate whether the multiple concentric rings, "searchlight beams'', and truncated equatorial disks recently discovered with HST in a few PPNe, are common or rare phenomena. 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 9785 Search for Core-disrupting Wide-Angle Winds We propose to obtain observations with STIS/FUV-MAMA of H$_2$ fluorescent lines along the cavity surrounding the star T Tau N. Since H$_2$ fluorescent lines are direct tracers of shock-excitation in low-mass star-forming regions, the high resolution achievable with STIS will allow us to delineate the region of interaction between the wind and the cloud, and to investigate the geometry of the outflow at unprecedentedly close distances to its source, 100 AU. Our observations will allow us to confirm, map out, and provide quantitative estimates of the off-axis {wide-angle} flow for the first time. Understanding the geometry of the wind is crucial because {1} it determines whether outflows can disrupt their natal cores, and {2} it tests theories of jet production and collimation. ACS/HRC 9782 Measuring Black Hole Masses in Double Peaked Broad Lined AGNs To date there have been few black hole {BH} mass estimates for luminous broad line AGN, including those derived from reverberation mapping. In this context, objects with "double-peaked" broad lines are particularly important because the line emission is believed to arise in a relativistically rotating accretion disk. If this model is correct, then the BH mass can be determined directly from periodic variations in the line-profile shape. In two cases {Arp 102B and NGC 1097} such variations have been claimed. The goal of this proposal is to confront the relativistic disk model for the double-peaked Balmer lines with independent limits on the central masses for 5 of the nearest and brightest "double-peaked emitters" {NGC 1097, Arp 102B, Pictor A, 3C390.3, 3C332}, determined by using STIS long-slit spectroscopy to map the velocity field of circum-nuclear ionized gas. These observations will critically test the idea that the line emission in these objects comes from an accretion disk and thus provide unique insights into the physical processes operating in both the BLR and the "central engine". STIS 9633 STIS parallel archive proposal - Nearby Galaxies - Imaging and Spectroscopy Using parallel opportunities with STIS which were not allocated by the TAC, we propose to obtain deep STIS imagery with both the Clear {50CCD} and Long-Pass {F28X50LP} filters in order to make color-magnitude diagrams and luminosity functions for nearby galaxies. For local group galaxies, we also include G750L slitless spectroscopy to search for e.g., Carbon stars, late M giants and S-type stars. This survey will be useful to study the star formation histories, chemical evolution, and distances to these galaxies. These data will be placed immediately into the Hubble Data Archive. ACS 9438 The Origin of the Intergalactic Globular Cluster Population in Abell 1185 We request deep V and I observations with ACS to examine the properties of a newly discovered population of intergalactic globular clusters in the core of the rich galaxy cluster Abell 1185. Our previous WFPC2 observations of this field {GO-8164} revealed an excess of five times the number of objects at the expected magnitudes of globular clusters compared to the Hubble Deep Fields. The colors and luminosity function of these intergalactic globular clusters will place strong constraints on their origin, which in turn will yield new insights to the evolution of galaxy populations in dense environments 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. S/C 4974 TRTTEST No available description 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. 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. WFPC2 10082 POMS Test Proposal: WFII backup parallel archive proposal This is a POMS test proposal designed to simulate scientific plans WFPC2 10073 Earth Flats This proposal monitors flatfield stability. This proposal obtains sequences of Earth streak flats to construct high quality flat fields for the WFPC2 filter set. These flat fields will allow mapping of the OTA illumination pattern and will be used in conjuction with previous internal and external flats to generate new pipeline superflats. These Earth flats will complement the Earth flat data obtained during cycles 4-11. 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. 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 10050 ACS Earth Flats High signal sky flats will be obtained by observing the bright Earth with the HRC and WFC. These observations will be used to verify the accuracy of the flats currently used by the pipeline and will provide a comparison with flats derived via other techniques: L-flats from stellar observations, sky flats from stacked GO observations, and internal flats using the calibration lamps. Weekly coronographic monitoring is required to assess the changing position of the spots. ACS/WFC 10046 CCD Hot Pixel Annealing Hot pixel annealing will be performed once every 4 weeks. The CCD TECs will be turned off and heaters will be activated to bring the detector temperatures to about +20C. This state will be held for approximately 12 hours, after which the heaters are turned off, the TECs turned on, and the CCDs returned to normal operating condition. To assess the effectiveness of this procedure, a bias and two dark images will be taken after the annealing procedure for both WFC and HRC. The HRC darks are taken in parallel with the WFC darks. ACS/WFC 10043 External CTE Monitor Monitor CTE changes during cycle 11. Determine CTE. 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/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 9302: GS Acquisition (1,2,1) @ 031/02:35:23Z failed to RGA control due to SRLE on FGS 1. Prior FHST FM Updates U2,3FM @ 031/02:10Z and 02:13Z had good attitude errors. GS Re-acquisition @ 031/04:06:26Z took two attempts, but was successful. Under investigation. HSTAR 9303: GS Acquisition (3,2,2) @ 032/02:33:19Z resulted in FL backup (3,0,3) due to SSLE on FGS 3. Subsequent GS Re-acquisitions (3,2,2) @ 032/04:09:56Z, 032/05:45:05Z, 032/07:21:49Z, 032/08:57:45Z, and 032/10:33:42Z will also result in FL backup.Under investigation. HSTAR 9304: GS Acquisition (1,2,2) @ 032/12:14:00Z resulted in FL backup using FGS 2 due to SSLEX on FGS 1. Prior FHST FM Updates @ 032/11:53Z and 11:55Z showed good attitude error vector. FHST Map @ 032/12:50Z showed error values of -20.737, -13.107, and -14.441 arcsec. Under investigation. HSTAR 9306: GS Acquisition (1,2,1) @ 033/03:45:46Z resulted in FL backup using FGS 1. After coming out of the ZOE @ 033/03:51:56Z, no flags were observed. Under investigation. COMPLETED OPS REQs: 17085 TRT Trending Test 2004-030 @030/2228z OPS NOTES EXECUTED: 1160-2 Default Config for TLMDIAGs @030/2351z SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 27 26 031/0235z (HSTAR#9302) FGS REacq 16 16 FHST Update 57 57 LOSS of LOCK SIGNIFICANT EVENTS: Successfully completed the second TRT Trending Test 030/21:01Z - 22:28Z (OR 17085 with attached Transient Rate Trending Test script). The test performed exactly as expected. A very preliminary look at the data indicates extended transitions were seen for some of the iterations. This data will now be combined with the first run of this test to look for trends. Subsequent GS acquisition (using FGS 2) @ 030/23:55Z was successful. |
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