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Daily 3635
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3635 PERIOD COVERED: DOY 168 OBSERVATIONS SCHEDULED ACS/HRC 9703 Coronagraphic Search for Planets around Nearby Stars We will use the HRC coronagraph to search for planets, disks, and exo-zodiacal dust around nearby stars. We have selected the following stars: alpha Cen A and B, tau Ceti, and epsilon Eridani. The observations of each star will be taken at two or more epochs. The observations will be broken into a sequence of short exposures and taken at different roll angles to compensate for "telescope breathing" during the orbit. As a further precaution, the observations will be scheduled after the closest possible nearby pointing in order to minimize thermal changes in the OTA during the first orbit of observations. After matching phases, the PSFs from one star will be subtracted from the other star. 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/SBC 10047 ACS UV Contamination Monitor A standard star field {NGC6681} is observed every three months, alternating between after and before annealing operations, through all the ACS broad band UV filters. NGC6681 hosts several UV spectro - photometric standard stars for which accurate spectra have been {and will continue to be} measured with STIS. Two SBC dark current exposures taken as the last exposure of each SBC sequence. Also, to minimize SBS turn-on/turn-off cycles and in order to check the lab flats for the SBC detector, internal observations using the deuterium lamp with F125LP are being taken inflight, following the UV monitor observations. The internal flats have been taken ~monthly since SMOV, and the degradation of the lamp has been monitored. The total exposure time to date is ~15 hours giving a total of 8600 counts/pixel. The goal is 10, 000 counts/pixel such that the resulting pipeline flat has uncertainties of ~1% due to poisson counting statistics. Thus, approximately 3 additional hours of observation are required. 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. 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. NIC2 9856 A near-IR imaging survey of submm galaxies with spectroscopic redshifts Submillimeter {submm} surveys with SCUBA have identified a population of obscured star-forming and active galaxies at high redshift. Our recent spectroscopic campaigns with the Keck-10m telescope have uncovered redshifts for 37 SCUBA galaxies. The wide redshift range of the radio identified submm population {z=1-4} implies that many varieties of sources driven by different physical processes may be selected in a submm survey. We propose to use HST-NICMOS, ACS to obtain 2-filter images of a sample of 15 SCUBA galaxies with redshifts spanning z=0.8-3.5. Our goal is to understand what physical process {major mergers?} drive their strong evolution and great luminosities, and what the implications are for galaxy evolution models. 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. STIS/CCD 9885 Probing the High Redshift Universe with Quasar Emission Lines The quasar epoch is believed to be associated with the birth of the most massive galaxies, a time marked by rapid star formation and evolution. Quasar emission lines can reveal the chemical evolution and physical state of gas in the very center of these galaxies. Analysis of the observed line strengths, using tools that have recently become available, implies that the chemical composition of the emitting gas correlates with quasar luminosity in a way that is suggestive of the known galactic mass/luminosity/metallicity correlations. The emission lines can also reveal the form of the ionizing radiation field emitted by the central object. Understanding the evolution of the central powerhouse is important for black hole accretion physics and because its spectrum is likely to dominate the ionization of the IGM. There are many high-ionization permitted emission lines in the region below 1000A rest wavelength that can provide important new constraints on these measurements. Thus, there is a critical need for spectra over the full rest-wavelength range ~ 600A through the UV. Through a pilot Cycle 10 archival study, we have identified the QSO HE 1122-1648 as an optimal object for such a study. This QSO has a sufficiently high redshift {z = 2.4} so that we can see down to very short rest wavelengths {463A} in observed-wavelength regions where STIS has high sensitivity, and lies on a line of sight with an unusually low density of intervening Ly-alpha absorber clouds. A high-quality spectrum of this object will have implications for the ionization of the IGM and will leverage the unique UV capabilities of HST to complement the galaxy formation studies that NGST will do at higher redshift. WFPC2 10071 WFPC2 CYCLE 12 Supplemental Darks Part 3/3 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.) None COMPLETED OPS REQs: None OPS NOTES EXECUTED: None SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 7 7 FGS REacq 6 6 FHST Update 13 13 LOSS of LOCK SIGNIFICANT EVENTS: Successfully completed first group of Intensity data collections per Ops Request 17198. Sections A through D (of consolidated script) have been executed thus far. FHST Rate Control and FHST Intensity data collections continued. See Ops Request 17198 and 17199-1 for details. Set-up and execution of HST CCS Release 5.0.3.1 CT verification test scheduled 169/11:00Z - 19:00Z with GDOC, HITT, and SOC using CCS "H" String with CCS Release xxx (intentionally removed) and PRD xx. The purpose of this testing is to verify GSCA 793 Upgrade to PF-13 Spare. |
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