HUBBLE SPACE TELESCOPE DAILY REPORT # 3181 PERIOD COVERED: DOYs 228 - 230 OBSERVATIONS SCHEDULED (see HSTARS below for possible observation problems) 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 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 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. ACS 9563 Preliminary ACS Sensitivity A spectrophotometric standard star is observed through a popular subset of filters of each camera to assess the sensitivity of the instrument. The star is placed at the centre of the aperture, and two images are taken through each filter. This programme is based on proposal 9020 designed for SMOV. There are three groups of visits, numbered respectively 1 through 3, 4 through 6 and 7 through 9. The three visits in each group must be executed about one month apart from one another, as indicated in the visit requirements. The first visit in each group {namely visits 1, 4 and 7} ought to be scheduled during the month of July 2002. During SMOV the standard star GD71 could be used, which is not visible during the Cycle 11 interim calibration period. We have selected GRW+705824 instead. The latter is a WD slightly brighter than GD71 in V but with very similar spectral properties. The exposure times with this object have been selected to reach, on average, SNR~350 in the central pixel for broad band filters. 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/HRC 9379 Near Ultraviolet Imaging of Seyfert Galaxies: Understanding the Starburst-AGN Connection We propose a near-UV snapshot survey of 101 Seyfert galaxies using ACS/HRC and the filter F330W, a configuration which is optimal to detect faint star forming regions around their nuclei. These images will complement optical and near-IR images available in the HST archive, thus providing a panchromatic atlas of the inner regions of active galaxies, which we will use to study the starburst-AGN connection. The main goals of this proposal are: {1} Determine the frequency of circumnuclear starbursts in Seyferts, down to levels which cannot be observed from the ground; {2} characterize the observational {fluxes, colors, structure, sizes} and intrinsic {luminosities, masses, ages, global star-formation rate} properties of these clusters; {3} derive the luminosity functions of young star clusters around the nucleus of Seyferts and compare these results with those from normal and starburst galaxies to determine their survival rate close to the AGN; {4} address questions about the relation between AGNs and starbursts, like the possible connection between the masses and luminosities of black holes and starbursts, and the implications for the evolution of the black holes and their host galaxy bulges. By adding UV images to the existing optical and near-IR ones, this project will create an extremely valuable database for astronomers with a broad range of scientific interests, from the properties of the AGN to the properties of their host galaxies. ACS/WFC 9584 ACS Default {Archival} Pure Parallel Program II. The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels. 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/ FGS 9347 FGS Astrometry of the Extrasolar Planet of Epsilon Eridani We propose observations with HST/FGS in Position Mode to determine the astrometric elements {perturbation orbit semimajor axis and inclination} of the candidate extra-solar planet around the K2 V star Epsilon Eridani that has been detected by Doppler spectroscopy. These observations will also permit us to determine the actual mass of the planet by providing the sin{i} factor which can not be determined with the radial velocity method. High precision radial velocity {RV} measurements spanning the years 1980.8--2000.0 for the nearby {3.22 pc} star Epsilon Eri show convincing variations with a period of ~ 7 yrs. These data represent a combination of six independent data sets taken with four different telescopes. A least squares orbital solution using robust estimation yields orbital parameters of period, P = 6.9 yrs, velocity K- amplitude = 19 m/s, eccentricity e = 0.6, projected companion mass M_B sin{i} = 0.83 M_Jupiter. An estimate of the inclination yields a perturbation semi-major axis, Alpha = 0arcs0022, easily within the reach of HST/FGS astrometry. NICMOS 9366 H_2 Imaging of Proto-Planetary Nebulae: Probing the Dynamics and Morphology H_2 emission provides an excellent probe of the physical conditions in planetary nebulae {PNs} and also in proto- planetary nebulae {PPNs}, objects in transition between the asymptotic giant branch {AGB} and PN phases. It is thought that the shaping of the PN occurs when a fast wind interacts with the remnant of the AGB progenitor during the PPN phase. The study of shock-excited H_2 in PPNs will allow us to study this process. We request HST/NICMOS H_2 and complementary K and H broad-band images of 13 PPNs with a range of spectral types of the central star. We presently have very high- resolution {~100, 000} H_2 spectra for 7 of these, which we will use with the high-resolution images to study the velocity structure of the fast wind. We will also explore the relationship between the presence of H_2 and a bipolar shape for the nebula, as has been found in PNs. However, the role of the equatorial torus is expected to be different in these two cases, and in the PPNs it is expected to collimate the wind rather than shield the molecules. Thus the H_2 in the PPNs is expected at the ends of the lobes rather than in the torus. Radiatively-excited H_2 emission appears to be common in PPNs with central stars of B spectral types; this appears to be a transitional stage in the evolution of the H_2 in the nebula which these images will help us to better understand. 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. 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. 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. SNAP/STIS 9434 A SNAPSHOT Survey of the Hot Interstellar Medium We propose to obtain SNAPSHOT STIS echelle observations of key tracers of hot interstellar gas {CIV, NV and SiIV} for selected FUSE Team OVI survey targets with known UV fluxes. By taking advantage of the SNAPSHOT observing mode we will efficiently obtain a large number of spectra suitable for the study of the highly ionized hot component of the interstellar medium {ISM}. Our goals are to explore the physical conditions in and distribution of such gas, as well as to explore the nature of the interfaces between the hot ISM and the other interstellar gas phases. Using inter--comparisons of the various ionic ratios for CIV, NV, OVI and SiIV, we will be able to discriminate between the various models for the production of the highly ionized gas in the Galactic ISM. The survey will also enable detailed studies of regions already known to contain hot gas through X-ray emission measurements {e.g., SNRs and radio loops}. The proposed SNAPSHOT observations will extend our previous Cycle 9 survey {which was compromised by the STIS side 1 failure}, and should roughly double the number of stars for which high quality STIS observations of the important hot gas tracers are available, enabling us to derive a truly global view of the hot ISM. STIS 8653 Collimation and Physical Conditions Within the HH 30 Protostellar Jet We propose to observe the protostellar jet HH 30 through a wide slit with STIS in order to determine the distance from the star that the jet becomes collimated, and to diagnose the density, temperature, shock structure, and ionization within the collimation region. The proposed observations will provide an image of the jet in each emission line across the entire optical spectrum with minimal contamination from the reflection nebula near the star, a marked improvement over existing narrowband images that cover only a few lines which emit over a limited range of densities and ionization states. Ratios of the new emission-line images will probe the physical conditions in the jet with HST spatial resolution and make it possible to observe the shape and location of any shocks in the flow, resolve the cooling layers behind these shocks, and trace the recombination of any ionized gas that emerges from the base of the jet. The proximity and brightness of HH 30 together with its favorable inclination angle make this an ideal object to study jet collimation. The new STIS spectra are precisely what are needed to test MHD models of jet collimation from accretion disks. Understanding how jets originate, become collimated, and form shocks has profound implications for the distribution of magnetic fields and angular momentum within accretion disks, which in turn control how stars and planets form. 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/CCD 8902 Dark Monitor-Part 2. The Space Telescope Imaging Spectrograph (CCD) was used to monitor the darks. 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. WF/PC-2 9254 Cycle 10 CTE Monitor. The WF/PC-2 was used to monitor CTE changes during cycle 10. WF/PC-2 9180 Gamma-ray Burst Progenitors: Probing Their Environment. The WF/PC-2 was used to perform a target of opportunity observation of gamma ray burster (GRB), GRB-011121. GRB astronomy is a field maturing at a phenomenal rate. Three important new observational and theoretical discoveries, formulated over the last twelve months, allow the proposer to address new, and in many cases, more sophisticated questions than could have been posed previously. These developments: the discovery of X-ray lines in GRB 991216; the observation that N_H as deduced from X-ray afterglow are one to two orders of magnitude larger than the dust extinction inferred from optical afterglow; and the growing realization that the afterglow emission may exhibit features of dust echoes, appear to offer unexpected and new diagnostics that will directly inform us about the progenitor, the circum-progenitor material and the immediate interstellar environs. 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. WFPC2/PC1 9663 Focus Monitoring The HST focus is monitored using WFPC2/PC1. In principle ACS/HRC should provide superior capability for monitoring the HST focus. Since most of the HST science will shift to ACS in Cycle 11 trending observations are continued with this program to establish the focus of WFPC2/PC1 {and hence HST} and ACS/HRC {and WFC to a lessor degree} using exposures over full orbits that are taken in parallel. With parallel exposures breathing cancels out for the relative camera offset. FLIGHT OPERATIONS SUMMARY: HSTARS (For details see http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf) 8765 - B String Coredataserver ISPNULL @228/0220z.CCS "B" String Core Data Server ISPNULL process count = 0%, flashing red @ 228/02:20Z. Under investigation. COMPLETED OPS REQs: None OPS NOTES EXECUTED: None SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 19 19 FGS REacq 26 26 FHST Update 39 39 LOSS of LOCK Operations Notes: None SIGNIFICANT EVENTS: 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. NBL 02.3 (Batteries, RSUs, WFC3 - Parazynski, Williams), 7 am - 5 pm, Day 1 of 5, @ JSC NBL.