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