HUBBLE SPACE TELESCOPE DAILY REPORT # 3180 PERIOD COVERED: DOY 227 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/MA1/MA2 9036 An Ultraviolet Spectroscopic Survey of Star-Forming Galaxies in the Local Universe. The Space Telescope Imaging Spectrograph (CCD, MA1 and MA2) was used to perform a comprehensive STIS ultraviolet spectroscopic survey of star-forming galaxies in the local universe. The sample covers a broad range of morphologies, chemical composition, and luminosity. The observations will provide spectral coverage between 1200 and 3100 Angstrom, at a resolution of 100 to 200 kms and S/N of about 30. The data set will allow the proposers to document and quantify the effects of massive stars on the interstellar medium and to infer implications for the evolution of the host galaxies. Note: Proposal 9036 maybe degraded because the Fine Guidance Sensors could only acquire a single guide star at August 15, 2002 22:56 STIS/CCD 9317 Pure Parallel Imaging Program: Cycle 10. program for STIS during cycle 10. FGS 9348 The Distances to AM CVn stars We propose to determine the parallaxes and proper motions of the five brightest of the seven known AM CVn systems using the HST Fine Guidance Sensors. AM CVn systems are binaries where mass is transferred from a completely hydrogen-deficient, degenerate mass donor to a white dwarf primary through a helium accretion disk. A better understanding of these systems is crucial for a number of reasons:, to study the late stages of binary evolution, to study the effect of chemical composition on the physics of accretion discs; , o to estimate their contribution to the Supernovae Ia rate and , to estimate their contribution to the gravitational radiation background. All these studies rely critically on a determination of the distances to the currently known systems. With brightnesses in the range 13~ 24, V >~ 25.5}. Recent near-IR observations with the CTIO/OSIRIS and VLT-UT1/ISAAC revealed four objects within about 2'' radius circle around the X-ray position. One of these objects -- which is 0arcs6 from the X-ray source position -- is a plausible candidate for the IR counterpart of the X-ray source. To verify this hypothesis and understand the nature of the X-ray source, we propose deep imaging with NICMOS. An IR counterpart, variable at the X-ray period, and with brightness and broad-band spectrum consistent with a stellar object, would identify the source as an accreting binary with a subluminous companion. This would be the first discovery of a binary system inside a young SNR. Alternatively, a faint counterpart with a peculiar spectrum would indicate the presence of a long-hypothesized residual disk leftover after the supernova explosion. 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. 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. 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. WFPC2 9634 POMS Test Proposal: WFII targeted parallel archive proposal The parallel opportunities available with WFPC2 in the neighborhood of bright galaxies are treated in a slightly different way from the normal pure parallels. Local Group galaxies offer the opportunity for a closer look at young stellar populations. Narrow-band images in F656N can be used both to identify young stars via their emission lines, and to map the gas distribution in star-forming regions. Thus, the filter F656N is added to the four standard filters. Near more distant galaxies, up to about 10 Mpc, we can map the population of globular clusters; for this purpose, F300W is less useful, and only F450W, F606W, and F814W will be used. ACS 9650 CCD Hot Pixel Annealing Hot pixel annealing will be performed once every 4 weeks. The CCD TECs will be turned off and heaters will be activated to bring the WFC detector temperature to about +10C. The HRC temperature will reach about 30C.This state will be held for approximately 24 hours, after which the heaters are turned off, the TECs turned on, and the CCDs returned to normal operating condition. To assess the effectiveness of this procedure, a bias and two dark images will be taken before and after the annealing procedure for both WFC and HRC. WFPC2 9676 POMS Test Proposal: WFII parallel archive proposal 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) HSTAR 8763 G STRING NOT UPDATING THE TDM DATA FILE. Recycled G-string during ZOE as per FOT (Joe Cooper) requested due the SAC software problem which was the TDM data file has not been updating for the last 24 hours. George Gibson (RT) has been notified the problem. Under investigation. HSTAR 8764 GSACQ (3,2,3) FL backup, scan step limit exceeded on FGS2 @ 227/2301z. GSacq(3,2,3) at 22:56:35 resulted in fine lock back-up on FGS 3 with scan step limit exceeded on FGS 2. Two subsequent REACQ's also failed to FL backup. Under investigation. Observations affected: WFPC 166 to 173, STIS 109 to 114, ACS 91 to 97, NICMOS 90. COMPLETED OPS REQs: None OPS NOTES EXECUTED: 1027-2 - Reset MCE1 Limits @227/1800z SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 6 6 FGS REacq 9 9 FHST Update 15 15 LOSS of LOCK Operations Notes: 1. FOT conducted operations from Bld#23 227/0930z - 228/0100z due to AT&T work. 2. Target of Opportunity SMS SA224M01_F Signed Off and 1st 486 load uplinked @228/0900z SIGNIFICANT EVENTS: HST On-Orbit Checkout of real-time WSC interface scheduled daily 224 - 231 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.