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Daily 3597
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3597 PERIOD COVERED: DOY 113 OBSERVATIONS SCHEDULED ACS/HRC/WFC 10060 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 9722 Life in the fast lane: The dark-matter distribution in the most massive galaxy clusters in the Universe at z0.5 We propose two-filter ACS observations of a complete sample of 12 very X-ray luminous galaxy clusters at 0.5z0.7 as a cornerstone of a comprehensive multi-wavelength study of the properties of the most massive clusters in the universe. Our sample includes the famous systems Cl0016+16 and MS0451-03; all other clusters are new discoveries from the MACS survey. Being the counterparts of the best-studied systems at lower and higher redshift and comprising ALL massive clusters at 0.5z0.7 observable from Mauna Kea this sample will become the ultimate reference for cluster studies at z0.5. HST's unique capabilities will allow us to: 1} measure accurately the clusters' dark matter distribution on scales from tens to more than 500/h_50 kpc from observations of strong and weak gravitational lensing, 2} use galaxy-galaxy lensing to measure the shape, extent, and mass content of the dark-matter halos of both cluster and field galaxies, and 3} study the color morphology of mergers and the star formation history of galaxies in a high-density environment. The proposed observations are complemented by Chandra observations of all our targets {all 12 awarded, 11 executed to date} which provide independent constraints on the dark matter and gas distribution in the cluster cores, as well a by extensive groundbased observations of weak lensing on yet larger scales, galaxy dynamics, and the SZ effect. ACS/WFC 9766 The Globular Cluster Systems of Spiral Galaxies along the Hubble Sequence While the globular cluster {GC} systems of ellipticals and ongoing mergers have been relatively well-studied with HST, very little is known about the GC systems of spirals besides the Milky Way and M31. To constrain GC/galaxy formation models, especially where spirals are the merger progenitors of ellipticals, it is crucial to understand their GC properties. We propose to obtain ACS images of three edge-on spirals, spanning the Hubble sequence, with Keck spectroscopic follow-up. This will effectively double the number of well-studied spiral systems. We will detect 100-200 GCs per galaxy, sufficient to reveal GC subpopulations, their relative numbers, radial trends, and dependences on Hubble type {e.g., a bulge vs. disk origin for red GCs}. For half of our GCs we will be able to measure individual sizes. By providing a much-needed comparative benchmark, these data will allow researchers to better exploit the large existing HST database of GCs in E/S0 galaxies. ACS/WFC 9811 Establishing the Metallicity Distribution in Normal Giant Ellipticals NGC 3377 and 3379, the Leo Group ellipticals at d=11 Mpc, are the nearest E galaxies commonly regarded to be structurally" normal", and as such, they are keystone objects for understanding the evolution and early star formation history of large ellipticals. The ACS/WFC camera now gives us the ability to obtain the metallicity distribution function {MDF} of their stellar population by direct resolution and photometry of their halo stars. To do this, we will follow the same highly successful techniques we have previously used for NGC 5128 with WFPC2 {V, I} imaging: the {V-I} colors of the brightest red-giant stars are highly sensitive to metallicity, and their locations in the color-magnitude diagram can be used for direct construction of the MDF. This will be a major step forward to understanding the formation history of these cosmologically dominant galaxies. 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. NIC1/NIC2/NIC3 8792 NICMOS Post-SAA calibration - CR Persistence Part 3 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 10018 CCD Dark Monitor-Part 2 Monitor the darks for the STIS CCD. STIS/CCD 10020 CCD Bias Monitor - Part 2 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. 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. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) HSTAR 9393: GS Acquisition (2,0,2) @ 114/03:47:16Z failed. There were no flags indicating a GS Acquisition failure, except an ESB message a0a which is DETECT_FL_TIMEOUT (FGS Fine Lock failed - Timed out waiting for fine lock FGS: 2). FHST Map @ 114/04:31:25Z had errors of -15.686, 8.898, and -10.734. Under investigation. COMPLETED OPS REQs: None OPS NOTES EXECUTED: 1224-2 Bay 5 WEB Temp Limit Change @113/1053z 1225-0 - SMA Training (Open) SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 9 8 114/0347z (HSTAR#9393) FGS REacq 7 7 FHST Update 21 21 LOSS of LOCK SIGNIFICANT EVENTS: None |
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