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Daily 3620
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3620 PERIOD COVERED: DOY 146 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/HRC/WFC 9763 Calibrating the Black Hole Mass Scale for Quasars We propose to obtain ACS/WFC imaging of all 17 low-redshift quasars that have black hole masses measured from reverberation mapping. This is a key sample since all secondary methods to estimate black hole mass in quasars depend on this local reverberation-mapped sample for their calibration. The best external check on reverberation mapping is whether it gives results that are consistent with the black hole mass- host galaxy correlations of nearby galaxies. For local Seyfert galaxies the reverberation masses appear consistent with the M-sigma correlation, but it is not known whether this also holds true for quasars because the stellar velocity dispersions of quasar hosts are virtually impossible to measure. We will use the ACS data to measure accurate bulge parameters {luminosity and effective radius} for the host galaxies of the reverberation-mapped quasars. From the fundamental plane or the Faber-Jackson relation, we can estimate the host galaxy velocity dispersion and test whether the reverberation masses follow the M-sigma relation even for objects with quasar luminosities. This is a crucial test if we are to trust the reverberation masses as the lowest rung on a "distance ladder" of black hole mass estimators for quasars, so that quasars can be used to trace the cosmological growth history of black holes. {Note added in Phase II: the TAC awarded us 8 orbits to observe 7 quasars and a PSF star.} ACS/WFC/HRC 9905 The Host Galaxies of Type II Quasars Type II quasars are the luminous analogues of Type II Seyferts; the central engines are presumably heavily obscured by dust. We have defined a sample of 9 highly luminous Type II quasar candidates with 0.24 z 0.40 from the spectroscopic data of the Sloan Digital Sky Survey, which have high equivalent width, narrow emission-line spectra characteristic of a nonthermal continuum. We estimate that the obscured AGN in these objects have optical luminosities of order 10^{12} solar luminosities. We propose to image this sample in rest-frame U, B and V, to determine the morphology and color of the host galaxies, and look for recent star formation. We will also probe the extended environments of these objects, to determine whether they are undergoing interactions with close companions, and whether they live in appreciably clustered environments. GO 9367 Unique Opportunities to Search for the Optical Counterparts to High-Z Damped LyAlpha Systems The galaxies responsible for damped LyAlpha absorption in QSO spectra are difficult to observe against the strong background QSO emission. We propose to detect even low luminosity galaxies associated with QSO absorption line systems out to redshifts as high as z = 1.8 by observing them in the shadow cast by an even higher redshift damped LyAlpha absorber. As a result the galaxy will be observed free of contamination by the background AGN and of the uncertainties which arise when image processing techniques are required to remove the AGN emission. We propose two approaches. In the first we will attempt to detect a z = 1.8634 system seen in the optical spectrum of a high-z BL Lac object in the shadow of two higher-redshift systems seen in the same optical spectrum. In the second only the higher redshift shadowing LyAlpha system is seen in the optical spectrum and the presence of the lower- redshift systems at z = 0.713 and z = 1.0466 are inferred from the presence of strong MgII, SiII and FeII absorption lines. 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. NICMOS/STIS CCD 9405 The Origin of Gamma-Ray Bursts The rapid and accurate localization of gamma-ray bursts {GRBs} promised by a working HETE-2 during the coming year may well revolutionize our ability to study these enigmatic, highly luminous transients. We propose a program of HST and Chandra observations to capitalize on this extraordinary opportunity. We will perform some of the most stringent tests yet of the standard model, in which GRBs represent collimated relativistic outflows from collapsing massive stars. NICMOS imaging and STIS CCD spectroscopy will detect broad atomic features of supernovae underlying GRB optical transients, at luminosities more than three times fainter than SN 1998bw. UV, optical, and X-ray spectroscopy will be used to study the local ISM around the GRB. Chandra spectroscopy will investigate whether the GRB X-ray lines are from metals freshly ripped from the stellar core by the GRB. HST and CTIO infra-red imaging of the GRBs and their hosts will be used to determine whether `dark' bursts are the product of unusually strong local extinction; imaging studies may for the first time locate the hosts of `short' GRBs. Our early polarimetry and late-time broadband imaging will further test physical models of the relativistic blast wave that produces the bright GRB afterglow, and will provide unique insight into the influence of the GRB environment on the afterglow. 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/MA1 9754 Intergalactic O VI absorption at redshift 0.004 Simulations of the formation of large-scale structure in the universe predict that at the present time a large fraction of the baryons in the intergalactic medium {IGM} is in a warm/hot phase, with T=10^5-10^7 K. The warm phase has been detected with HST in absorption through the OVI 1031.926, 1037.671 doublet at redshifts ~0.15-0.3. In a sample of 100 extra-galactic objects observed with FUSE, we find 12 detections of OVI at redshifts z=0.0008-0.004 {v=250 to 1200 km/s}. Many of these occur within 400 kpc and 50 km/s of a nearby galaxy, making it much easier to understand the relation between the OVI absorbers and galaxies. Our sample allows a comparison of the properties of nearby vs more distant OVI absorbers. However, modeling the physical conditions in the gas requires measurements of HI, OVI, CIV, NV and CIII. High velocity resolution is required to resolve the HI, CIV and NV lines in order to discriminate between collisional and photoionization. We propose to obtain improved HI data, as well as the CIV and NV measurements for two absorbers at z0.004. One appears to represent collisional ionization {Mrk 876}, while the other probably represents a case of a photoionized system {Ton S180}. Understanding the ionization of the warm IGM is essential for determining elemental abundance and the baryonic content of the gas. WFPC2 10067 WFPC2 Cycle 12 Decontaminations and Associated Observations This proposal is for the monthly WFPC2 decons. Also included are instrument monitors tied to decons: photometric stability check, focus monitor, pre- and post-decon internals {bias, intflats, kspots, & darks}, UV throughput check, VISFLAT sweep, and internal UV flat check. 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.) None COMPLETED OPS REQs: None OPS NOTES EXECUTED: None SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 04 04 FGS REacq 11 11 FHST Update 07 07 LOSS of LOCK SIGNIFICANT EVENTS: Successfully completed first series of OBAD/Rate Control data collections, Sections A through H @ 146/01:50Z (OR 17169 with attached OBAD Data Collection procedure). Additional OBAD data collection periods are necessary for further analysis of the process in support of future TGS efforts. OBAD data collection series scheduled as follows: 147/01:27:00 - 147/02:07:10 (PN) 147/16:06:00 - 147/16:23:00 (PN) 147/23:49:00 - 148/00:25:00 (PN) These periods involve transition to PN format in order to capture FHST position and intensity data at a higher rate. All command relating to the OBAD data collection is on a NIB with routine spacecraft activities. See Ops Request 17169 with attached OBAD Data Collection script for details. A compliment of SA 3 strings is being kept offline to optimize the Battery Full Charge Rate. To ensure HST remains power positive as solar intensity continues to decline, EPS hardware and SSM486 FSW changes need to be made to bring the +D SPA (5 strings) back online and offline the +DD SPA (4 strings). |
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