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Daily 3504
HUBBLE SPACE TELESCOPE
DAILY REPORT # 3504 PERIOD COVERED: DOYs 339-341 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. STIS/CCD 9981 The Ultra Deep Field - STIS parallels We propose to obtain slitless spectroscopy of objects in the GEMS and GOODS area around the UDF. WFPC2 9980 The Ultra Deep Field - WFPC2 Parallels The ACS Ultra Deep Field {UDF} is a survey carried out by using Director's Discretionary time. The main science drivers are galaxy evolution and cosmology. The primary instrument is the Advanced Camera for Surveys but WFPC2, NICMOS, and STIS will also be used in pure parallel mode. The data will be made public. The UDF consists of a single ultra-deep field {410 orbits in total} within the CDF-S GOODS area. We request a modification of the default pure parallel programs. Rather than duplicate the redder bands which will be done much better with ACS, we propose to observe in the near-ultraviolet F300W filter. These data will enable study of the rest-frame ultraviolet morphology of galaxies at 0z1, allowing determination of the morphological k-correction and the location of star formation within galaxies, using a sample that is likely to be nearly complete with multi-wavelength photometry and spectroscopic redshifts. The results can be used to interpret observations of higher redshift galaxies by ACS. NIC3 9979 The Ultra Deep Field - NICMOS Parallels This is a plan to manage the NICMOS pure parallels of the ACS Ultra Deep Survey. We will obtain a mix of F110W and F160W images along sight-lines within the mosaiced ACS fields of the CDF-S GOODS and GEMS surveys, with these sight-lines enabling an examination of the space density and morphologies of the reddest galaxies. ACS/CCD/WFC 9978 The Ultra Deep Field with ACS The ACS Ultra Deep Field {UDF} is a survey carried out by using Director's Discretionary time. The main science driver are galaxy evolution and cosmology. The primary instrument is the Advanced Camera for Surveys but WFPC2 and NICMOS will also be used in parallel. The data will be made public. The UDF consists of a single ultra-deep field {410 orbits in total} within the CDF-S GOODS area. The survey will use four filters: F435W {55 orbits}, F606W {55 orbits}, F775W {150 orbits}, and F850LP {150 orbits}. The F435W {B} and F606W {V} exposures will be one magnitude deeper than the equivalent HDF filters. The F775W {I} exposure will be 1.5 magnitude deeper than the equivalent HDF exposure. The depth in F775W and F850LP is optimized for searching very red objects - like z=6 galaxies - at the detection limit of the F850LP image. The pointing will be RA{J2000}=3 32 40.0 and Decl.{J2000}=-27 48 00. These coordinates may change slightly due to guide star availability and implementation issues. We will attempt to include in the field both a spectroscopically confirmed z=5.8 galaxy and a spectroscopically confirmed type Ia SN at z=1.3. The pointing avoids the gaps with the lowest effective exposure on the Chandra ACIS image of CDFS. This basic structure of the survey represents a consensus recommendation of a Scientific Advisory Committee to the STScI Director Steven Beckwith. A local Working Group is looking in detail at the implementation of the survey. ACS/HRC/WFC/NIC3 9890 Probing the Dynamics and Shock Physics of the Cas A Supernova Remnant Cassiopeia A {Cas A; SN 1680} is the youngest known and closest example of an oxygen-rich, core-collapse supernova remnant. A two-year WFPC2 survey of part of the remnant yielded many new insights including realization of the stunning amount of fine-scale detail present in the ejecta, and the first precise location of the reverse shock front in the main shell via rapid emission and structural changes visible over 2 yrs. In addition, these data revealed over 100 new ejecta knots located out ahead of the forward blast wave in a small region where only a handful were known from ground-based images. We propose a follow-up survey program aimed at obtaining hi-res images of the entire remnant in the ejecta's four major emission lines. A separate set of ACS and NIC3 [Si VI] images of the NW reverse shock filaments will be taken 3-4 months following the main Cycle 12 survey images. These will allow us to the trace individual ejecta knot deceleration dynamics, excitation, and evolution during reverse shock passage. Analysis of the emission line fluxes will make use of custom shock models generated by us for Cas A. These data will also provide data on outer knot chemistry and expansion asymmetries particularly in regard to the collimation of the NE and SW jets of O, Si, Ca-rich ejecta. A major aim of this program is to acquire a superb two-year image database covering the entire remnant to allow a detailed shock physics and dynamics study. NIC2 9875 The Fundamental Plane of Massive Gas-Rich Mergers We propose deep NICMOS H-band imaging of a carefully selected sample of 33 luminous, late-stage galactic mergers. This program is part of a comprehensive investigation of the most luminous mergers in the nearby universe, the ultraluminous infrared galaxies {ULIGs}. The high-resolution HST images will complement an extensive set of ground-based data that include long-slit NIR spectra from a recently approved Large VLT Programme. This unique dataset will allow us to derive with unprecedented precision structural -and- kinematic parameters for a large unbiased sample of objects spanning the entire ULIG luminosity function. These data will refine the fundamental plane of massive gas-rich mergers and enable us to answer the following questions: {1} Do ultraluminous mergers form elliptical galaxies, and in particular, giant ellipticals? {2} Do ULIGs evolve into optically bright QSOs? The results from this detailed study of massive mergers in the local universe will be relevant to understanding galaxy formation and evolution at earlier epochs, and in particular, the dusty sub-mm population that accounts for more than half of the star formation at z 1. STIS/CCD 9866 First Spectroscopic Study of a Unique Set of Young Stars in the Orion Nebula We propose to obtain the first spectra of the central stars of Orion proplyds for which the stars are visible in WFPC images. While it is known that the central stars are broadly late-type, they have never been spectrally classified or studied in detail as pre-MS objects. The Orion proplyds are generally thought to be protoplanetary disks similar to the primordial disk of the Solar System. They offer a unique opportunity to understand the physical conditions of protoplanetary disks in a nebular environment generally believed to be typical of that in which most stars formed. Models of the proplyds are available which predict the observable IR spectral energy distribution using the spectral type of the central star as part of the numerical input. Further progress in understanding proplyds will require knowledge of the spectral types of these stars. We will use already-proven diagnostics for spectrally classifying late-type PMS stars. In addition, many emission lines are expected in objects of this age which can be used to look for infall and outflow. Different accretion models of young stars predict different line widths, so our observations can help test models of late-type pre-MS stars and can be used to compare as pre-MS objects the proplyd stars with other pre-MS stars. 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 9861 ACS Imaging of beta Pic: Searching for the origin of rings and asymmetry in planetesimal disks The emerging picture for planetesimal disks around main sequence stars is that their radial and azimuthal symmetries are significantly deformed by the dynamical effects of either planets interior to the disk, or stellar objects exterior to the disk. The cause of these tructures, such as the 50 AU cutoff of our Kuiper Belt, remains mysterious. Structure in the beta Pic planetesimal disk could be due to dynamics controlled by an extrasolar planet, or by the tidal influence of a more massive object exterior to the disk. The hypothesis of an extrasolar planet causing the vertical deformation in the disk predicts a blue color to the disk perpendicular to the disk midplane. The hypothesis that a stellar perturber deforms the disk predicts a globally uniform color and the existence of ring-like structure beyond 800 AU radius. We propose to obtain deep, multi-color images of the beta Pic disk ansae in the region 15"-220" {200-4000 AU} radius with the ACS WFC. The unparalleled stability of the HST PSF means that these data are uniquely capable of delivering the color sensitivity that can distinguish between the two theories of beta Pic's disk structure. Ascertaining the cause of such structure provide a meaningful context for understanding the dynamical history of our early solar system, as well as other planetesimal systems imaged around main sequence stars. ACS/HRC 9851 Host Galaxies of Reverberation-Mapped AGNs We propose to obtain unsaturated ACS high-resolution images of all reverberation-mapped active galactic nuclei in order to remove the point-like nuclear light from each image, thus yielding a "nucleus-free" image of the host galaxy. This will allow investigation of host-galaxy properties: our particular interest is determination of the host-galaxy starlight contribution to the reverberation mapping observations, which is necessary for accurate determination of the relationship between the AGN continuum flux and the size of the broad Balmer-line emitting region of AGNs. Because this relationship is used to estimate black-hole masses of large samples of distant AGNs, correct determination of the slope of this relationship is critically important. 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}. WFPC2 9809 Saturn's rings and small moons on the eve of Cassini We propose to continue our long-term survey of Saturn's rings and small moons to obtain a coherent set of high resolution, multi-color WFPC2 images of Saturn and its rings during the final year before the arrival of the Cassini spacecraft at Saturn in mid-2004. Our Cycle 6-11 programs {6806, 7427, 8398, 8660, 8802, and 9341} explored the rings from their nearly edge-on aspect {southern hemisphere spring} to summer solstice in late 2002. We now propose to take advantage of the especially favorable viewing geometry of Cycle 12 to obtain UBVRI, F255W, and methane-filter PC images of the rings, small moons, and planet at the lowest phase angle {0.07 degrees} observable to date. A key goal is to measure for the first time the expected sharp spike in the opposition brightness of the rings and small moons, which will characterize the structure and particle properties of the rings and the surfaces of the satellites. We will also follow the chaotic behavior of Prometheus and Pandora, two small moons which may be perturbing each other gravitationally. Here, our goals are to catch the satellites in the act of any new coupled motions and to determine the changes in semimajor axis, eccentricity, and orbital inclination of the moons resulting from their most recent large chaotic interaction in 2000. This will complete our continuous WFPC2 coverage of these moons from 1994 until mid-2004, when Cassini's cameras will at long last surpass the capabilities of the HST. The Cycle 12 observations will also enable us to determine zonal winds and regional variations in Saturn's atmosphere prior to Cassini's arrival. ACS/HRC/WFC 9793 The Grism-ACS Program for Extragalactic Science {GRAPES} We propose an ACS grism spectroscopic survey with a wide component and an ultradeep single ACS field. The wide component covers the well-imaged GOODS Chandra Deep Field south and the deepest field will be the Ultra Deep field to be observed in cycles 11 and 12. The Grism ACS Program for Extra-galactic Science {GRAPES} will: {1} Probe the reionization epoch by robustly determining the luminosity function of Lyman-alpha emitters, Lyman break galaxies and low luminosity AGNs at z~6, and thus the sources of ionizing photons at the end of the "dark ages". A similar census of ionizing photon sources at z=4-6 needed to maintain the ionized state of the IGM will also be achieved. {2} Study galaxy formation and evolution by finding galaxies in a contiguous redshift range between z=4-7 and evolution of black holes through a census of low-luminosity AGNs. {3} Study star-formation and galaxy assembly at its peak at z=1-2 by identifying star-forming galaxies by their emission lines, old galaxies by the 4000 AA break and any combination of new and old populations showing both lines and breaks. {4} Allow the deepest unbiased spectroscopy yet, for identification of objects to I=27. {5} Enhance the value of multiwavelength data in the UDF and GOODS field to the astronomical community. WFPC2 9712 Pure Parallel Near-UV Observations with WFPC2 within High-Latitude ACS Survey Fields In anticipation of the allocation of ACS high-latitude imaging survey{s}, we request a modification of the default pure parallel program for those WFPC2 parallels that fall within the ACS survey field. Rather than duplicate the red bands which will be done much better with ACS, we propose to observe in the near-ultraviolet F300W filter. These data will enable study of the rest-frame ultraviolet morphology of galaxies at 0z1. We will determine the morphological k-correction, and the location of star formation within galaxies, using a sample that is likely to be nearly complete with multi-wavelength photometry and spectroscopic redshifts. The results can be used to interpret observations of higher redshift galaxies by ACS. WFPC2 9709 POMS Test Proposal: 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. NICMOS 8790 NICMOS Post-SAA calibration - CR Persistence Part 1. 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. 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 10042 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 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. STIS/CCD 10000 STIS Pure Parallel Imaging Program: Cycle 12 This is the default archival pure parallel program for STIS during cycle 12. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) HSTAR 9227: While guiding on two FGSs, after successful GS Acquisition (2,1,2) @ 339/13:46:40Z, LOL occurred @ 339/13:59:47Z due to SSLE on FGS 1, followed by new sequential update (#44 Command) @ 339/14:00:40Z. Spacecraft was successfully guiding on two FGS in spite of this event. FHST Map @ 339/13:54:56Z had large roll error, V1 = 109.467 arcsec, 3-axis error (RSS). Under investigation. HSTAR 9228: GS Acquisition (2,1,2) @ 339/15:22:45Z, which began during ZOE, resulted in FL backup at AOS, without indication flags, using FGS 2 (2,0,2). Unable to determine FGS modes and Flag Bit changes, pending SSR dump @ 340/00:50:45Z. FHST Map @ 339/15:31:01Z showed vehicle axis errors V1 = -154.931, V2 = -4.564, V3 = 9.748 arcsec. From SSR dump, analysis indicates GS Acquisition failed due to SSLE @ 339/15:26:25Z. Under investigation. HSTAR 9229: GS Acquisition (2,1,2) @ 339/16:58:50Z resulted in FL back (2,0,2) using FGS 2 due to SSLE on FGS 2. FHST Map @ 339/17:07:06Z showed vehicle axis errors V1 = -157.647, V2 = -6.698, V3 = 3.693 arcsec. Under investigation. HSTAR 9233: GS Acquisition (1,2,1) @ 342/02:25:24Z resulted in FL backup due to SSLE on FGS 2. GS Re-acquisitions @ 342/04:02:04Z and 05:38:07Z will also result in FL backup. Under investigation. COMPLETED OPS REQs: None OPS NOTES EXECUTED: None SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 25 25 FGS REacq 19 19 FHST Update 41 41 LOSS of LOCK SIGNIFICANT EVENTS: None |
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