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Daily 3534
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3534 PERIOD COVERED: DOY 19 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 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/HRC 9853 A Search for Young Binary Brown Dwarfs: Constraining Formation Scenarios and Masses Through Multiplicity We propose to use the Advanced Camera for Surveys / High Resolution Camera to conduct a direct imaging multiplicity survey of 34 young brown dwarfs in the nearest regions of recent star formation, the T association Taurus-Auriga and the OB association Upper Scorpius. The determined multiplicity fraction, the separation distribution, and the mass ratio distribution will offer stringent observational constraints on proposed brown dwarf formation scenarios. Moreover, the small semi-major axes of known field and open cluster brown dwarf binaries suggest the exciting possibility of our identifying several very close binaries { 15 AU}. Continued monitoring of these systems would yield, on a decade timescale, the first dynamical mass estimates of T Tauri brown dwarfs. With masses intermediate between those of stars and planets, brown dwarfs offer our best hope of relating the reasonably well understood processes of star formation to the less well understood processes of planet formation. 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 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. 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 9789 The Distance to the Pleiades Despite its fundamental importance to stellar astrophysics, the distance to the Pleiades open cluster remains in great dispute. Main-sequence fitting results in a distance of 132.3 +/- 1.9 pc, while the Hipparcos average parallax for Pleaides member stars gives a distance of 116.4 +/- 2.9 pc. If the Hipparcos distance is to be believed, our current understanding of stellar astrophysics is dramatically incomplete. On the other hand, it has been proposed that the Hipparcos parallax measurement to the Pleiades suffers systematic uncertainties which result in the discrepancy with the main-sequence fitting technique. The question will remain open until an independent distance measurement to the Pleiades cluster is performed. We will use ACS imaging to determine the parallax to the Pleiades to an accuracy of about 1.5%. This will resolve the current controversy over the distance to the cluster once and for all. 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. ACS/WFC/WFPC2 9810 Accurate and Robust Calibration of the Extragalactic Distance Scale with the Maser Galaxy NGC4258 The extragalactic distance scale {EDS} is defined by a comparison of Cepheid Period-Luminosity {PL} relations for nearby galaxies and the LMC, whose uncertain distance is thereby the SOLE anchor. Studies of maser sources orbiting the central black hole in the galaxy NGC4258 have provided the most accurate extragalactic distance ever {7.2+/- 0.5Mpc}. Since this distance is well determined and based on GEOMETRIC arguments, NGC4258 can provide a much needed new anchor for the EDS. We propose multi-epoch BVIH observations of NGC4258 in order to discover about 100 Cepheids and to characterize their light curves with 2-3 times greater accuracy than was previously possible with WFPC2. At 90 orbits {48 in Cycle 12; 42 in Cycle 13}, this is a relatively large program. However, the result will have a major impact on the EDS, and substantial attention must be paid to characterization and minimization of systematic errors, as from metallicity, crowding, and blending. The resulting dataset will be the most complete for Cepheids in any galaxy yet studied with HST. In an ongoing NASA-funded program {OSS-SARA}, we are using new analysis techniques and radio data to reduce uncertainty in the geometric distance to 3% {0.07 mag}. With this improved geometric distance and the BVIH data, we will be able to calculate the zero point of the PL relation ROBUSTLY to 4% {0.09 mag}. 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. 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. 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. NIC3 9998 NICMOS Cycle 12 Grism Calibration and Standard Stars to 2.5microns This is the grism calibration proposal. 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 10033 MAMA Sensitivity and Focus Monitor Cycle 12 Monitor sensitivity of each MAMA grating mode to detect any change due to contamination or other causes. Also monitor the STIS focus in a spectroscopic and an imaging mode. 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/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. WFPC2 10068 WFPC2 CYCLE 12 Standard Darks This dark calibration program obtains dark frames every week in order to provide data for the ongoing calibration of the CCD dark current rate, and to monitor and characterize the evolution of hot pixels. Over an extended period these data will also provide a monitor of radiation damage to the CCDs. 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 10072 WFPC2 CYCLE 12 INTERNAL MONITOR This calibration proposal is the Cycle 12 routine internal monitor for WFPC2, to be run weekly to monitor the health of the cameras. A variety of internal exposures are obtained in order to provide a monitor of the integrity of the CCD camera electronics in both bays {gain 7 and gain 15}, a test for quantum efficiency in the CCDs, and a monitor for possible buildup of contaminants on the CCD windows. WFPC2 10082 POMS Test Proposal: WFII backup parallel archive proposal This is a POMS test proposal designed to simulate scientific plans 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.) HSTAR 9291: During ZOE, GS Acquisition (1,2,1) @ 019/12:03:39Z resulted in FL back up (1,0,1). Under investigation. HSTAR 9292: GS Acquisition (3,2,3) @ 019/20:12:42Z resulted in FL backup using FGS 2 due to SSLE (QF3SSLEX) on FGS 3. Prior FHST FM Updates @ 019/19:35:15Z and 19:38:00Z showed good attitude error vector. FHST Map @ 019/20:32:08Z showed 3-axis (RSS) error value ~ 11.00 arcsec. Subsequent GS Reacquisition (3,2,3) @ 019/21:29:47Z resulted in FL backup. Under investigation. COMPLETED OPS REQs: None OPS NOTES EXECUTED: None SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 11 11 FGS REacq 3 3 FHST Update 24 24 LOSS of LOCK SIGNIFICANT EVENTS: HST Command Timing test scheduled 020/12:00Z - 22:00Z with GDOC, SOC, HITT, and CCS using CCS "D" String with CCS Release 5.0.3.1 and PRD O06300ST. The purpose of this testing is to check the command time for CCS Release 5.0.3.1 with historical, baselined numbers. |
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