From: "Jacques van Oene" Newsgroups: sci.space.news Subject: HST Daily Report #3372 Date: Tue, 3 Jun 2003 18:49:57 +0200 Organization: Jet Propulsion Laboratory - Pasadena CA Approved: sci-space-news@zagami.jpl.nasa.gov Message-ID: <006301c329f0$2a8ed740$d1cd5dd5@chello.nl> charset="iso-8859-1" Content-Transfer-Encoding: 7bit X-Trace: nntp1.jpl.nasa.gov 1054658962 4220 137.78.16.91 (3 Jun 2003 16:49:22 GMT) X-Complaints-To: news@newsfeed.jpl.nasa.gov NNTP-Posting-Date: 3 Jun 2003 16:49:22 GMT X-Priority: 3 X-MSMail-Priority: Normal X-Mailer: Microsoft Outlook Express 5.00.2615.200 X-MIMEOLE: Produced By Microsoft MimeOLE V5.00.2615.200 Originator: daemon@zagami.jpl.nasa.gov Xref: newsread1.funet.fi sci.space.news:13621 HUBBLE SPACE TELESCOPE DAILY REPORT # 3372 PERIOD COVERED: DOY 148 OBSERVATIONS SCHEDULED NICMOS 8791 NICMOS Post-SAA calibration - CR Persistence Part 2 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. The keyword 'USEAFTER=date/time' will also be added to the header of each POST-SAA DARK frame. The keyword must be populated with the time, in addition to the date, because HST crosses the SAA ~8 times per day so each POST-SAA DARK will need to have the appropriate time specified, for users to identify the ones they need. Both the raw and processed images will be archived as POST-SAA DARKSs. Generally we expect that all NICMOS science/calibration observations started within 50 minutes of leaving an SAA will need such maps to remove the CR persistence from the science images. Each observation will need its own CRMAP, as different SAA passages leave different imprints on the NICMOS detectors. STIS/CCD/MA1 9357 Towards a global understanding of accretion physics --, Clues from an UV spectroscopic survey of cataclysmic variables Accretion inflows and outflows are fundamental phenomena in a wide variety of astrophysical environments, such as Young Stellar Objects, galactic binaries, and AGN. Observationally, cataclysmic variables {CVs} are particularly well suited for the study of accretion processes. We propose to carry out a STIS UV spectroscopic snapshot survey of CVs that fully exploits the diagnostic potential of these objects for our understanding of accretion physics. This survey will provide an homogenous database of accretion disc and wind outflow spectra covering a wide range of mass transfer rates and binary inclinations. We will analyze these spectra with state-of-the-art accretion disc model spectra {SYNDISK}, testing our current knowledge of the accretion disc structure, and, thereby, providing new insight into the so far not well understood process of viscous dissipation. We will use our parameterized wind model PYTHON for the analysis of the radiation driven accretion disc wind spectra, assessing the fundamental question whether the mass loss rate correlates with the disc luminosity. In addition, our survey data will identify a number of systems in which the white dwarf significantly contributes to the UV flux, permitting an analysis of the impact of mass accretion on the evolution of these compact stars. This survey will at least double, if not triple, the number of high-quality accretion disc / wind outflow / accreting white dwarf spectra, and we waive our proprietary rights to permit a timely use of this database. GO 9367 Unique Opportunities to Search for the Optical Counterparts to High-Z Damped LyAlpha Systems The galaxies responsible for damped LyAlpha absorption in QSO spectra are difficult to observe against the strong background QSO emission. We propose to detect even low luminosity galaxies associated with QSO absorption line systems out to redshifts as high as z = 1.8 by observing them in the shadow cast by an even higher redshift damped LyAlpha absorber. As a result the galaxy will be observed free of contamination by the background AGN and of the uncertainties which arise when image processing techniques are required to remove the AGN emission. We propose two approaches. In the first we will attempt to detect a z = 1.8634 system seen in the optical spectrum of a high-z BL Lac object in the shadow of two higher-redshift systems seen in the same optical spectrum. In the second only the higher redshift shadowing LyAlpha system is seen in the optical spectrum and the presence of the lower- redshift systems at z = 0.713 and z = 1.0466 are inferred from the presence of strong MgII, SiII and FeII absorption lines. NICMOS 9375 The Host Galaxies of Time Delay Lenses: , An Independent Route to the Hubble Constant Because of its importance in setting the distance scale, the time scale and in estimating cosmological parameters from the CMB, astronomy needs an estimate of the Hubble constant independent of the local distance scale and its systematic problems. This can be achieved using gravitational lenses with time delay measurements given enough constraints on the gravitational potential of the lens. We will use deep NICMOS observations of the lensed quasar host galaxies in 7 gravitational lenses with time delay measurements to obtain the necessary constraints, determine the dark matter distribution and estimate H_0. Analysis of the existing images and the well-developed theory for analyzing Einstein ring images of host galaxies suggest the new data will break the familiar degeneracies between lens mass distributions and the Hubble constant. We also request 30 ksec Chandra ACIS images for each of the 2 systems lacking them {B1608+656 and B1600+434} to measure the mass in nearby or surrounding groups and clusters. ACS/HRC 9391 High-Resolution Imaging of Pluto's Surface We will collect a series of observations with the ACS/HRC from which we will derive a two-color global map of Pluto's surface. We will image Pluto at F435W and F555W, wavelengths that have been extensively studied from the ground over the past 50 years. The maps will provide albedos with accurate error determinations down to 52 degrees South latitude. These observations will provide a second epoch of HST mapping of the active surface of Pluto as it continues to recede from the Sun and will provide an important context for other detailed studies of Pluto. ACS 9476 Galaxy Evolution in the Richest Clusters at z=0.8: the EDisCS Cluster Sample The study of distant cluster galaxies requires two key ingredients: {1} deep high-resolution imaging, to constrain galaxy structure; and {2} 8m-class spectroscopy, to measure stellar content, star-formation rates, dynamics, and cluster membership. We will reach both conditions with the addition of HST/ACS imaging to our suite of VLT {36 nights} and NTT {20 nights} observations of 10 confirmed clusters at z~0.8, drawn from the ESO Distant Cluster Survey {EDisCS}. The proposed HST/ACS data will complement our existing optical/IR imaging and spectroscopy with quantitative measures of cluster galaxy morphologies {i.e. sizes and shapes, bulge-disk decompositions, asymmetry parameters}, and with measurements of cluster masses via weak lensing. Major advantages unique to the EDisCS project include: {i} uniform selection of clusters; {ii} large enough sample sizes to characterize the substantial cluster-to-cluster variation in galaxy populations; {iii} large quantities of high quality data from 8m telescopes; {iv} uniform measurements of morphologies, spectroscopic and photometric redshifts, SEDs, star-formation/AGN activities, and internal kinematics; {v} optical selection of clusters to complement the X-ray selection of almost all high-z clusters in the ACS GTO programs; {vi} forefront numerical simulations designed specifically to allow physical interpretation of observed differences between the high-z and local clusters. 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 9482 ACS Pure Parallel Lyman-Alpha Emission Survey {APPLES} Ly-alpha line emission is an efficient tool for identifying young galaxies at high redshift, because it is strong in galaxies with young stars and little or no dust --- properties expected in galaxies undergoing their first burst of star- formation. Slitless spectroscopy with the ACS Wide-Field Camera and G800L grism allows an unmatched search efficiency for such objects over the uninterrupted range 4 <~ z <~ 7. We propose the ACS Pure Parallel Ly-alpha Emission Survey {``APPLES''}, to exploit this unique HST capability and so obtain the largest and most uniform sample of high redshift Ly-alpha emitters yet. Parallel observations will allow this survey to be conducted with minimal impact on HST resources, and we will place reduced images and extracted spectra in the public domain within three months of observation. We aim to find ~ 1000 Ly-alpha emitters, 5 times the biggest current sample of Ly-alpha emitters. This unprecedented sample will provide robust statistics on the populations and evolution of Ly-alpha emitters between redshifts 4--7; a robust measurement of the reionization redshift completely independent of the Gunn-Peterson trough; spatial clustering information for Ly-alpha emitters which would let us probe their bias function and hence halo mass as a function of redshift; many galaxies at redshift exceeding 6; and lower redshift serendipitous discoveries. 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/ WFPC2 9595 WFPC2 CYCLE 11 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 9604 STIS CCD Performance Monitor This activity measures the baseline performance and commandability of the CCD subsystem. Only primary amplifier D is used. Bias and Flat Field exposures are taken in order to measure bias level, read noise, CTE, and gain. Numerous bias frames are taken to permit construction of "superbias" frames in which the effects of read noise have been rendered negligible. Full frame and binned observations are made, with binning factors of 2 x 1, 1 x 2, 2 x 2, 4 x 1, and 4 x 2. Dark images are taken in 2x2 binning mode; 1x1 binning darks are being taken in the nominal CCD Dark Monitor. Bias frames are taken in subarray readouts to check the bias level for ACQ and ACQ/PEAK observations. All exposures are internals. STIS 9606 CCD Dark Monitor-Part 2 Monitor the darks for the STIS CCD. STIS 9608 CCD Bias Monitor - Part 2 Monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4, to build up high-S/N superbiases and track the evolution of hot columns. STIS 9615 Cycle 11 MAMA Dark Monitor This test performs the routine monitoring of the MAMA detector dark noise. This proposal will provide the primary means of checking on health of the MAMA detectors systems through frequent monitoring of the background count rate. The purpose is to look for evidence of change in dark indicative of detector problem developing. NICMOS 9636 Cycle 11 NICMOS dark current, shading profile, and read noise monitoring program The purpose of this proposal is to monitor the dark current, read noise, and shading profile for all three NICMOS detectors throughout the duration of Cycle 11. This proposal is a continuation of PID 9321 which covers the period between the end of SMOV3B and the onset of Cycle 11. ACS 9674 CCD Daily Monitor 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. NICMOS 9693 NICMOS Coronagraphic Performance Assessment This test defines a coherent program designed to quantitatively measure and map out the diffractive and scattered energy rejection of occulted targets to improve the target/background contrast ratios by use of the NICMOS coronagraph. The performance levels of system will be assessed while exploring the observational parameter spaces and execution strategies which undoubtedly will be proposed for use in HST Cycle 11. This test is constructed in four parts with different, but complementary, Taken together they will provide critical information needed to re-evaluate the coronagraphic systemic performance from which flight {and possibly ground} S/W updates, and advisories to observers defining Phase 2 proposals will be issued. STIS 9708 STIS Pure Parallel Imaging Program: Cycle 11 This is the default archival pure parallel program for STIS during cycle 11. WFPC2 9709 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. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) HSTAR 9046: GS Acquisition (2,3,2) @ 148/09:40:13Z failed to RGA control during ZOE due to SRLE on primary FGS 2. Under investigation. COMPLETED OPS REQs:NONE OPS NOTES EXECUTED: 1114-0 Change Limits MAMA2 Threshold Voltage @ 148/23:16z SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 09 08 See Hstar # 9046 FGS REacq 07 07 FHST Update 18 18 LOSS of LOCK SIGNIFICANT EVENTS: HST FSW 2.3c Ops Acceptance Test Part 2 of 2 scheduled 148/10:00Z - 149/01:00Z with GDOC, HITT, SE, and VEST using CCS "B" and "C" Strings with CCS Release 4.0.2.2 and PRD O06100R1T. The purpose of the testing is to verify installation and back out procedures for the RAM version of FSW 2.3c and EEPROM installation procedure work in an operational scenario. ---- Jacques :-) Editor: www.spacepatches.info ------------------------------------------------------