HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3184<br /><br />PERIOD COVERED: DOY 233<br /><br />OBSERVATIONS SCHEDULED [see HSTARS below for possible observation problems]<br /><br />NICMOS 8790<br /><br />NICMOS Post-SAA calibration - CR Persistence Part 1.<br /><br />A new procedure proposed to alleviate the CR-persistence problem of NICMOS. Dark<br />frames will be obtained immediately upon exiting the SAA contour 23, and every<br />time a NICMOS exposure is scheduled within 50 minutes of coming out of the SAA.<br />The darks will be obtained in parallel in all three NICMOS Cameras. The POST-SAA<br />darks will be non-standard reference files available to users with a USEAFTER<br />date/time mark.<br /><br />STIS/CCD 8902<br /><br />Dark Monitor-Part 2.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to monitor the darks.<br /><br />STIS/CCD 8904<br /><br />Bias Monitor-Part 2.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to monitor the bias in<br />the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4 in order<br />to build up high-S/N superbiases and track the evolution of hot columns.<br /><br />STIS/MA1/MA2 8920<br /><br />Cycle 10 MAMA Dark Measurements.<br /><br />the MAMA detector dark noise, and is the primary means of checking on health of<br />the MAMA detectors systems through frequent monitoring of the background count<br />rate.<br /><br />WFPC2 8938<br /><br />WFPC2 CYCLE 9 SUPPLEMENTAL DARKS pt3/3.<br /><br />This dark calibration program obtains 3 dark frames every day to provide data<br />for monitoring and characterizing the evolution of hot pixels.<br /><br />STIS/CCD 9317<br /><br />Pure Parallel Imaging Program: Cycle 10.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to perform the default<br />archival pure parallel program for STIS during cycle 10.<br /><br />ACS/STIS 9451<br /><br />ACS Imaging and STIS Spectroscopy of Binary Brown Dwarfs<br /><br />We have compiled a sample of 9 spatially resolved binary brown dwarfs {18<br />objects}, and now propose ACS imaging and STIS spectroscopic follow-up<br />observations. While theoretical models on the interplay of chemical and physical<br />processes governing brown dwarf atmospheres have reached a high level of<br />sophistication, interpretation of observational data remains difficult. As brown<br />dwarfs never stabilize themselves on the hydrogen main sequence, there is always<br />an ambiguity between the temperature or luminosity of any brown dwarf and its<br />mass or age. The individual components of brown dwarf binaries, however, are<br />expected to be coeval and have the same underlying chemical composition. This<br />provides crucial constraints on any model, thus greatly reducing the number of<br />the free parameters. The aim is to obtain photometric and spectroscopic data to<br />probe the physical and chemical properties of the brown dwarf atmospheres, as<br />well as second epoch astrometric data to characterize th e orbital motion. The<br />study will provide important feedback on theoretical model atmospheres and<br />evolutionary tracks for brown dwarfs. As such, it will be an important step<br />towards a better understanding of objects with spectral properties intermediate<br />between those of giant planets and late-type stars.<br /><br />9455<br /><br />ACS 9480<br /><br />Cosmic Shear With ACS Pure Parallels<br /><br />Small distortions in the shapes of background galaxies by foreground mass<br />provide a powerful method of directly measuring the amount and distribution of<br />dark matter. Several groups have recently detected this weak lensing by<br />large-scale structure, also called cosmic shear. The high resolution and<br />sensitivity of HST/ACS provide a unique opportunity to measure cosmic shear<br />accurately on small scales. Using 260 parallel orbits in Sloan textiti {F775W}<br />we will measure for the first time: beginlistosetlength sep0cm setlengthemsep0cm<br />setlength opsep0cm em the cosmic shear variance on scales <0.7 arcmin, em the<br />skewness of the shear distribution, and em the magnification effect. endlist Our<br />measurements will determine the amplitude of the mass power spectrum<br />sigma_8Omega_m^0.5, with signal-to-noise {s/n} ~ 20, and the mass density<br />Omega_m with s/n=4. They will be done at small angular scales where non-linear<br />effects dominate the power spectrum, providing a test of the gravitational<br />instability paradigm for structure formation. Measurements on these scales are<br />not possible from the ground, because of the systematic effects induced by PSF<br />smearing from seeing. Having many independent lines of sight reduces the<br />uncertainty due to cosmic variance, making parallel observations ideal.<br /><br />9483<br /><br />NICMOS 9484<br /><br />The NICMOS Parallel Observing Program<br /><br />We propose to manage the default set of pure parallels with NICMOS. Our<br />experience with both our GO NICMOS parallel program and the public parallel<br />NICMOS programs in cycle 7 prepared us to make optimal use of the parallel<br />opportunities. The NICMOS G141 grism remains the most powerful survey tool for<br />HAlpha emission-line galaxies at cosmologically interesting redshifts. It is<br />particularly well suited to addressing two key uncertainties regarding the<br />global history of star formation: the peak rate of star formation in the<br />relatively unexplored but critical 1<= z <= 2 epoch, and the amount of star<br />formation missing from UV continuum-based estimates due to high extinction. Our<br />proposed deep G141 exposures will increase the sample of known HAlpha emission-<br />line objects at z ~ 1.3 by roughly an order of magnitude. We will also obtain a<br />mix of F110W and F160W images along random sight-lines to examine the space<br />density and morphologies of the reddest galaxies. The nature of the extremely<br />red galaxies remains unclear and our program of imaging and grism spectroscopy<br />provides unique information<br /><br />regarding both the incidence of obscured star bursts and the build up of stellar<br />mass at intermediate redshifts. In addition to carrying out the parallel program<br />we will populate a public database with calibrated spectra and images, and<br />provide limited ground- based optical and near-IR data for the deepest parallel<br />fields.<br /><br />GO 9493<br /><br />Revealing the nature of low luminosity radio-galaxies with imaging polarimetry<br /><br />HST imaging of low luminosity FR I radio-galaxies allowed us to isolate for the<br />first time their optical nuclear emission from that of the host galaxy. Fluxes<br />of these unresolved nuclear sources strongly correlate with those of the radio-<br />cores, suggesting a common non-thermal origin. The picture which emerges is that<br />these radio-galaxies differ in many fundamental aspects from the other classes<br />of AGN as they might be lacking the substantial BLR, thermal disk emission and<br />torii, usually associated to active nuclei, probably reflecting a fundamentally<br />different accretion mode. On the other hand, these results support the<br />identification of FR I as the misoriented population of BL Lac objects. It is<br />crucial at this stage to firmly establish the synchrotron origin of these<br />nuclear sources. A simple and direct test can be performed by measuring their<br />polarization. In case of synchrotron emission we expect to detect significant<br />nuclear polarization, as routinely measured in BL Lac objects, at level of 3 -<br />20 We thus propose to obtain imaging polarimetry of a sample formed by the 9<br />nearest FR I radio- galaxies.<br /><br />STIS 9505<br /><br />The Evolution of Molecular Clouds.<br /><br />The combined STIS, FUSE and ground-based results will yield information needed<br />to understand the role of ablation in the evolution of the central clouds.<br /><br />ACS/CAL 9558<br /><br />ACS weekly Test<br /><br />This program consists of basic tests to monitor, the read noise, the development<br />of hot pixels and test for any source of noise in ACS CCD detectors. This<br />programme will be executed once a day for the entire lifetime of ACS.<br /><br />ACS 9564<br /><br />ACS Cycle 11: UV Earth Flats<br /><br />This proposal will obtain sequences of UV flats by observing the bright Earth.<br />The HRC UV filters were chosen for modes which were not obtained in the lab.<br />Since the UV transmission is likely to vary as a function of position on the<br />Pol_UV filters and on the coronograph, and since this behavior is currently<br />unconstrained by measurement, a good estimate for the missing UV flats cannot be<br />made. Although POL_UV and CORON transmissions change little at long wavelengths,<br />the UV transmission may change by amounts larger than can be estimated in the<br />absence of actual UV transmission measurements<br /><br />ACS 9669<br /><br />ACS coronagraph stability and vignetting<br /><br />This is a two-part activity for the purposes of {1} monitoring the positions ACS<br />coronagraph's occulting spots and the "Fastie Finger, " and {2} determining the<br />vignetting effects and the ability to flat field images of both point and<br />extended sources near the edges of the spots and finger.<br /><br />WFPC2 9676<br /><br />POMS Test Proposal: WFII parallel archive proposal<br /><br />This is the generic target version of the WFPC2 Archival Pure Parallel program.<br />The program will be used to take parallel images of random areas of the sky,<br />following the recommendations of the 2002 Parallels Working Group.<br /><br />POMS 9677<br /><br />POMS Test Proposal: WFII backup parallel archive proposal<br /><br />This is a POMS test proposal designed to simulate scientific plans. FLIGHT<br />OPERATIONS SUMMARY:<br /><br />HSTARS [For details see ]http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf]<br /><br />HSTARS: None<br /><br />COMPLETED OPS REQs:<br />16833-1 - Battery 1 Capacity Test Script @ 233/1240z [Steps 21-41 completed].<br /><br />OPS NOTES EXECUTED:<br />1030-0 CCC 5 Level Ground Limits for Battery 1 Recovery @ 233/2045z<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 7 7<br />FGS REacq 6 6<br />FHST Update 15 15<br />LOSS of LOCK<br /><br />Operations Notes: None<br /><br />SIGNIFICANT EVENTS:<br /><br />Successfully completed Battery 1 reconditioning with no issue during<br />discharge. After ~ 14.5 hours of discharge, the target low Voltage<br />was reached and the reconditioning resistor was autonomously turned<br />off by 486 FSW @ 233/12:34Z [OR16833-1]. EPS hardware reconfiguration<br />was completed during the following orbit night period, with the<br />reconnection of Solar Array Section 1 to Battery 1 completed @ 233/12:49Z.<br />Trickle charge was achieved in 45 minutes during the first orbit day pass<br />following configuration back to a 6-battery hardware system.<br /><br />NBL 02.3 [COS, ASCS, SSRF, SLIC COPE - Reilly, Walheim, Newman], Day<br />4 of 5, 7 am - 5 pm @ JSC NBL.<br /><br />HST On-Orbit Checkout of real-time WSC interface scheduled daily<br />231 - 238 with GDOC, STOCC Ops [SIMOR], HITT, and CCS using CCS "G"<br />String with CCS Release 4.0.1 and PRD O06100Q1. The purpose of this<br />testing is to verify CCS Release 4.0.1 [IP] capability to interface<br />through the IP Packet Filters to WSC for real-time telemetry and commands.