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Daily 3566
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3566 PERIOD COVERED: DOY 69 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/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/WFC 9575 Default {Archival} Pure Parallel Program. The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels in POMS. ACS/WFC/HRC 9771 The local Hubble flow and the density field within 6 Mpc Great progress has been made recently in accurate distance measurements of nearby galaxies beyond the Local Group based on the luminosity of the tip of the red giant branch {TRGB}. Over the last three years, snapshot surveys with HST have provided us with the TRGB distances for more than a hundred nearby galaxies obtained with an accuracy of about 10%. The local velocity field within 5 Mpc exhibits a significant anisotropy which disagrees with a spherical Virgo-centric flow. The local Hubble flow is very cold, with 1-D rms deviations of ~30 km/s. Cosmological simulations with Cold Dark Matter can only realize such low dispersions with a combination of a low mean density of matter and a substantial component with negative pressure. There may be a constraint on the equation of state w=-p/rho. Our observations will concentrate on 116 galaxies whose expected distances lie within 4 - 6 Mpc, allowing us to trace a Dark Matter distribution in the Local Volume with twice the information currently available. The program is a good one for SNAP mode because the order and rate that the observations are made are not very important, as long as there is good completion over several years. 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. 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 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. 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 9819 The Physical Character of the Smallest-Scale Interstellar Structures The origin{s} of interstellar structure recently seen on very small {tens of AU} scales is a puzzle that has inspired a number of possible theoretical interpretations. In particular, fluctuations in density and/or ionization fraction which can arise naturally in a turbulent medium may give rise to the observed structure. We propose to use STIS to accurately measure and compare selected interstellar absorption line profiles toward two binary star systems to test specific predictions of these models. In addition to NaI line profile variations between the stars indicative of structure on scales of ~2000 to 5000 AU, one member of each system shows temporal {proper motion induced} variations in one component indicative of structure on scales of ~20 AU. Such temporally variable components allow one to explore the structure of the interstellar medium on the smallest scales, and a detailed physical understanding of these structures requires the diagnostic power of the many interstellar species observable in the ultraviolet. By re-observing the HD 32039/40 system we will be able to confirm or invalidate our {turbulence inspired} model for the origin of this particular temporal fluctuation. The HD 36408AB system will allow us to study two locations near the edge of an individual cloud, and provide a new understanding of the surface layers of interstellar clouds. STIS/MA1/MA2 9739 Are We Missing the Dominant Sites of Star Formation in Local UV-Bright Starbursts? We propose to explore the ages, extinctions, and masses of young stellar clusters in four nearby dwarf starburst galaxies {He 2-10, NGC 5253, NGC 4214, and IIZw40}. We will combine available archival data with new, high resolution HST observations from the ultraviolet to the infrared. All four galaxies are known from ground based radio/infrared observations to contain highly obscured, massive stellar clusters, which dominate the far infrared flux. Despite the fact that almost all of the infrared flux comes from regions which are obscured at UV and optical wavelengths, these galaxies are consistent with the well known correlation between the UV slope {beta} and the ratio of far infrared flux to ultraviolet flux at 1600 Angstroms. Because the UV and IR fluxes are decoupled, this observation implies that a simple foreground screen model, where UV photons from hot stars are reprocessed into the infrared by local dust, is not the proper interpretation for why these galaxies follow the beta relation. We propose to investigate the underlying mechanisms responsible for this observed correlation in these UV bright galaxies, and explore the implication for high redshift starbursts. 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. 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 9634 POMS Test Proposal: WFII targeted parallel archive proposal The parallel opportunities available with WFPC2 in the neighborhood of bright galaxies are treated in a slightly different way from the normal pure parallels. Local Group galaxies offer the opportunity for a closer look at young stellar populations. Narrow-band images in F656N can be used both to identify young stars via their emission lines, and to map the gas distribution in star-forming regions. Thus, the filter F656N is added to the four standard filters. Near more distant galaxies, up to about 10 Mpc, we can map the population of globular clusters; for this purpose, F300W is less useful, and only F450W, F606W, and F814W will be used. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) HSTAR 9349: During LOS, NICMOS suspended @ 069/14:02:42Z due to an Intel Debug Exception with Status Buffer Message 104, Parameter 2, Time 32482 received. At the time NICMOS was executing Proposal 09999. Under investigation. COMPLETED OPS REQs: 17095-0 Dump NICMOS Memory after Suspend @ 069/16:43z 17096-4 NICMOS Suspend Recovery @ 069/18:25z OPS NOTES EXECUTED: NONE SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 11 11 FGS REacq 06 06 FHST Update 12 12 LOSS of LOCK SIGNIFICANT EVENTS: NICMOS suspended (during LOS) @ 069/14:02:42Z due to an Intel Debug Exception, received Status Buffer Message 104, Parameter 2, Time 32482. At the time of the suspend, NICMOS was executing Proposal 09999 "The COSMOS 2-Degree ACS Survey NICMOS Parallels". See HSTAR 9349. Following NICMOS Suspend, dumped NICMOS memory @ 069/16:43Z (OR 17995 and ROP NS-9). Successfully recovered NICMOS to Operate mode with FOM moves @ 069/18:21Z (OR 17096 and excerpts from COP 19.12). Command Timing test scheduled 070/12:00Z - 22:00Z with GDOC, SOC, HITT, and CCS using CCS "H"String with CCS Release 5.0.3.1 and PRD O6300ST. The purpose of this testing is to check the command timing for CCS Release 5.0.3.1 with historical, baselined numbers. O'Keefe, Beckwith, and Zubrin to Debate Hubble on CNN Tonight March 9, 2004 Mars Society President Dr. Robert Zubrin, Space Telescope Science Institute Director Dr. Steve Beckwith, and NASA Administrator Mr. Sean O'Keefe will discuss the Hubble Space Telescope on CNN tonight. At issue is Mr. O'Keefe's controversial decision to desert the space telescope. Both Dr. Zubrin and Dr. Beckwith oppose Hubble abandonment. The show will air twice, first within the Anderson Cooper newshour beginning at 7 PM EST, and then again during the Aaron Brown newshour which starts at 10 PM EST. |
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