HUBBLE SPACE TELESCOPE DAILY REPORT # 3177 PERIOD COVERED: DOY 224 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. WF/PC-2 8935 Cycle 10 Standard Darks. calibration of the CCD dark current rate, and to monitor and characterize the evolution of hot pixels. Over an extended period these data will also provide a monitor of radiation damage to the CCDs. 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. WF/PC-2 8939 Cycle 10 Internal Monitor. The WF/PC-2 was used to calibrate the internal monitor, to be run weekly to monitor the health of the cameras. GO 9172 Molecular Hydrogen in the Damped LyAlpha Absorber of Q1331+170 We wish to search for the Lyman and Werner absorption lines of molecular hydrogen {rest LambdaLambda = 1104 to 911 Angstrom} associated with the well-studied damped LyAlpha and 21-cm absorber at z=1.776 in Q1331+170. The rare detection of C I absorption in this system make this a promising candidate for a search. After detecting H_2, we plan to measure the relative population in the individual rotation states. The J = 0, 1, 2, 3 states will yield the kinetic temperature of the gas, while the weak J = 4 and higher states will measure {or limit} the local UV radiation field and hydrogen density. The detection of C I^* has been used to measure the cosmic microwave background temperature at z=1.776, and test the validity of the Big Bang model. The observed population of the fine structure levels of C I can be explained entirely by the expected CMB radiation, with surprisingly strong limits on local sources of excitation. The H_2 spectrum will enable us to check this result, by allowing us to make an independent estimate of the rate of UV and collisional pumping of the C I^* levels. 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. NICMOS 9321 Dark current, shading profile, and read noise monitoring program The purpose of this proposal is to monitor the detector dark current, read noise, and shading profile for all three NICMOS cameras from the onset of normal NCS operations throughout the start of Cycle 11. SNAP 9356 SNAPSHOT survey of the Planetary Nebulae population of the Galactic Bulge The spectacular structures seen in HST images of planetary nebulae {PNe} are generally accepted as originating from hydrodynamical interactions between stellar winds: the interacting-stellar wind model {ISW}. Traditionally, the shaping is thought to occur after the star becomes hot enough to ionize the PN. But recent HST images indicate that the shaping may occur earlier, and the newer GISW model puts the shaping during the pre-planetary nebula evolution. The relative importance of both models is not known: GISW shaping will account for some fraction of PNe, but estimates range from 15--100 during the PN phase, especially for the youngest PNe. We here propose an HST SNAPshot survey of compact PNe in the Galactic Bulge, to test these predictions. The Bulge provides the only PNe population for which progenitor masses are known and nebular ages can be measured. In support of these HST measurements we have already measured velocity fields and emission line fluxes. The survey will give an unbiassed sampling of morphologies, and allow evolutionary sequences to be determined to test the ISW versus the GISW model. By-products of the survey will be the determination of nebular masses, diameters and filling factors. We will also obtain the White Dwarf mass distribution in the Bulge, and the initial-final mass function for low-mass stars. GO 9428 SINS: The Supernova Intensive Study-- Cycle 11 Supernovae create the chemical history of the Universe, energize the interstellar gas, form the spine of the extragalactic distance scale, and provide the only direct evidence for an accelerating universe. SINS is a program to study supernovae, near and far. HST is the perfect match in field and scale for spatially-resolved observations of SN 1987A. There, a violent encounter between the fast-moving debris and the stationary inner ring is well underway. Monitoring this interaction will help solve the riddles of stellar evolution posed by the enigmatic three-ring system of SN 1987A. Our UV observations of Ly-Alpha emission reveal a remarkable reverse shock that provides a unique laboratory for studying fast shocks and a powerful tool for dissecting the structure of the vanished star. For more distant events, we propose Target-of-Opportunity observations. In addition to one bright new supernova in Cycle 11 discovered by any search at any time, we propose to discover two supernovae for study in the ultraviolet at times specified in advance, using the Lick Observatory Supernova Search. SINS will study the historic SN 1987A, explore UV emission from supernovae, and press late-time observations of supernovae into uncharted territory of infrared catastrophes, light echos, and stellar remnants. WFPC2 9436 Proper Motions of Bulge Stars at b=-6: The Shape of the Potential in the Central kpc of the Galaxy We propose to measure proper motions in a bulge field at l, b=0,-6, near the globular cluster NGC 6558. Suitable first- epoch data exist {from 1997}. These data will allow us to calculate the vertical potential gradient in the bulge region, and hence the flattening of the potential in the central regions of the potential - a crucial piece of information for deciding measuring the central density of the dark halo of the Galaxy. Central halo densities currently constitute one of the most discrepant predictions of structure formation theories. In addition, the proper motions will allow us to make a kinematic separation between bulge, disk and globular cluster stars. The resulting cleaned colour-magnitude diagrams allow the bulge main sequence turnoff to be viewed cleanly, and compared with lower-latitude regions. Thus age and metallicity gradients in the bulge can be measured. ACS 9472 A Snapshot Survey for Gravitational Lenses among z >= 4.0 Quasars Over the last few years, the Sloan Digital Sky Survey has revolutionized the study of high-redshift quasars by discovering over 200 objects with redshift greater than 4.0, more than doubling the number known in this redshift interval. The sample includes eight of the ten highest redshift quasars known. We propose a snapshot imaging survey of a well-defined sample of 250 z > 4.0 quasars in order to find objects which are gravitationally lensed. Lensing models including magnification bias predict that at least 4% of quasars in a flux-limited sample at z > 4 will be multiply lensed. Therefore this survey should find of order 10 lensed quasars at high redshift; only one gravitationally lensed quasar is currently known at z > 4. This survey will provide by far the best sample to date of high-redshift gravitational lenses. The observed fraction of lenses can put strong constraints on cosmological models, in particular on the cosmological constant Lambda. In addition, magnification bias can significantly bias estimates of the luminosity function of quasars and the evolution thereof; this work will constrain how important an effect this is, and thereby give us a better understanding of the evolution of quasars and black holes at early epochs, as well as constrain models for black hole formation. ACS 9480 Cosmic Shear With ACS Pure Parallels 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/WFPC2 9488 Cosmic Shear - with ACS Pure Parallel Observations The ACS, with greater sensitivity and sky coverage, will extend our ability to measure the weak gravitational lensing of galaxy images caused by the large scale distribution of dark matter. We propose to use the ACS in pure parallel {non- proprietary} mode, following the guidelines of the ACS Default Pure Parallel Program. Using the HST Medium Deep Survey WFPC2 database we have measured cosmic shear at arc-min angular scales. The MDS image parameters, in particular the galaxy orientations and axis ratios, are such that any residual corrections due to errors in the PSF or jitter are much smaller than the measured signal. This situation is in stark contrast with ground-based observations. We have also developed a statistical analysis procedure to derive unbiased estimates of cosmic shear from a large number of fields, each of which has a very small number of galaxies. We have therefore set the stage for measurements with the ACS at fainter apparent magnitudes and smaller, 10 arc-second scales corresponding to larger cosmological distances. We will adapt existing MDS WFPC2 maximum likelihood galaxy image analysis algorithms to work with the ACS. The analysis would also yield an online database similar to that in archive.stsci.edu/mds/ 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/WFC 9584 ACS Default {Archival} Pure Parallel Program II. The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels. WFPC2 9591 Cycle 11 WFPC2 CTE Characterization Monitor CTE changes during Cycle 11; test whether 2X2 binning affects CTE {may be relevant for ACS}; and perform a high S/N long-vs-short test in an uncrowded field. WFPC2 9596 WFPC2 CYCLE 11 INTERNAL MONITOR This calibration proposal is the Cycle 11 routine internal monitor for WFPC2, to be run weekly to monitor the health of the cameras. A variety of internal exposures are obtained in order to provide a monitor of the integrity of the CCD camera electronics in both bays {gain 7 and gain 15}, a test for quantum efficiency in the CCDs, and a monitor for possible buildup of contaminants on the CCD windows. 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. ACS/HRC 9691 Resolution of the Source Star for a Candidate Planetary Gravitational Microlensing Event deviation from the normal single-lens microlensing light curve on July 4.65-5.28, 2002 UT. This light curve deviation may be due to either a planetary or stellar companion orbiting the lens star, and the deviation is very well characterized since the event was observed continuously by telescopes at 6 different longitudes. The source star for this microlensing event is very likely to be unresolved in ground-based images when it is not magnified by microlensing, and our observations are intended to determine the properties of the lens star. We request UBVI images both during and after the microlensing event in order to get accurate measurements of the color of the lensed source star and any stars that are not resolved from it, such as the lens star. Note: Observations taken for proposal 9691 maybe degraded because the Fine Guidance Sensors could not acquire the guide stars at August 12, 2002 09:09 FLIGHT OPERATIONS SUMMARY: HSTARS (For details see http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf) 8761 - GSACQ (1,3,3) results in fine lock backup (1,0,1) @ 224/0909z. GSacq (1,3,3) scheduled at 224/09:09:19 - 09:16:42 which began during ZOE period, (mid-night shift) resulted to FL/BU at AOS using FGS#1 (1,0,1). Unable to determine FGS Modes and Flag Bit Changes, until ETR Dump at 225/19:20:48 Z. The MAP at 225/09:16:56 Z showed Vehicle Axis Errors: V1=17.989, V2=-2.962, V3=1.640 (arcsec).Subsequent REACQ'S at 225/10:05:24, 225/11:41:36 using the same guide star ID# resulted in FL/BU using FSG#1 (1,0,1). Under investigation. COMPLETED OPS REQs: None OPS NOTES EXECUTED: None SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 8 8 FGS REacq 7 7 FHST Update 12 12 LOSS of LOCK Operations Notes: None SIGNIFICANT EVENTS: Continued CCS Release 4.0.1 - IP Packet Filter Mode activities 224/09:00Z - 225/09:00Z using CCS "B" String. Successfully executed three NSSC-1 load uplinks, one 486 load uplink, eleven science data playbacks, ephemeris build and uplink, and several Mode 2 - Mode 1 changes. 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 D06100R2. 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.