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Daily 3423
HUBBLE SPACE TELESCOPE DAILY REPORT****** # 3423 PERIOD COVERED: DOYs 220-222 OBSERVATIONS SCHEDULED ACS 9658 ACS Earth Flats This program will obtain sequences of flat field images by observing the bright Earth. Several UV filters from the interim calibration program {9564} require additional exposures to obtain the required illumination. A few UV filters from this program will be repeated to monitor for changes in the flat fields and to verify the interim results. Since no streaks are observed in the UV, the wavelength coverage is extended to longer wavelengths in order to explore the severity of streaks in the flats from clouds in the FOV. We have added exposures for the HRC in the visible filters to verify the results derived from the L-flat campaign and to explore the severity of streaks. We have also added exposures on WFC using the minimum exposure time and using filters which will not saturate the brightest WFC pixel by more than 10 times the full well. ACS 9760 ACS Imaging of the Gemini Deep Deep Survey Fields: Galaxy Assembly at z = 1.5 We are presently carrying out the deepest redshift survey ever undertaken {the Gemini Deep Deep Survey}. Spectra of extraordinary quality have been taken in order to obtain redshifts in the so-called "redshift desert" at 1z2. This redshift range corresponds to the epoch of peak galaxy formation. In this proposal we request 40 orbits of ACS imaging to determine the morphologies of 100-120 candidate early-type galaxies with known redshifts in our survey fields. We seek to determine if these systems are indeed elliptical galaxies and to link their morphological states to their spectroscopically determined ages, recent star-formation histories, and to the evolving global stellar mass function at the peak epoch of galaxy assembly. ACS 9787 ACS Monitoring of the Polarization of the Crab Nebula We propose to use the ACS to follow the changing polarization of relativistically moving wisps in the Crab Nebula. Making use of the known geometry of the wisps, these observations will allow us to fully characterize the radiation field from the wisps as a function of direction relative to the axis of the wisp. These observations will provide detailed information on such hard-to-measure properties as the pitch-angle distribution of the radiating particles, and will help to constrain models of the flow. More generally, these observations will add to the already rich observational legacy of HST on what is arguably the most important single object in astrophysics. 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 9675 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. ACS 9984 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/HRC 9853 A Search for Young Binary Brown Dwarfs: Constraining Formation Scenarios and Masses Through Multiplicity We propose to use the Advanced Camera for Surveys / High Resolution Camera to conduct a direct imaging multiplicity survey of 34 young brown dwarfs in the nearest regions of recent star formation, the T association Taurus-Auriga and the OB association Upper Scorpius. The determined multiplicity fraction, the separation distribution, and the mass ratio distribution will offer stringent observational constraints on proposed brown dwarf formation scenarios. Moreover, the small semi-major axes of known field and open cluster brown dwarf binaries suggest the exciting possibility of our identifying several very close binaries { 15 AU}. Continued monitoring of these systems would yield, on a decade timescale, the first dynamical mass estimates of T Tauri brown dwarfs. With masses intermediate between those of stars and planets, brown dwarfs offer our best hope of relating the reasonably well understood processes of star formation to the less well understood processes of planet formation. ACS/WFC 9788 A Narrow-band Snapshot Survey of Nearby Galaxies We propose to use ACS/WFC to conduct the first comprehensive HST narrow-band {H-alpha + [N II]} imaging survey of the central regions of nearby bulge-dominated disk {S0 to Sbc} galaxies. This survey will cover, at high angular resolution extending over a large field, an unprecedented number of galaxies representing many different environments. It will have important applications for many astrophysical problems of current interest, and it will be an invaluable addition to the HST legacy. The observations will be conducted in snapshot mode, drawing targets from a complete sample of 145 galaxies selected from the Palomar spectroscopic survey of nearby galaxies. Our group will use the data for two primary applications. First, we will search for nuclear emission-line disks suitable for future kinematic measurements with STIS, in order to better constrain the recently discovered relations between black hole mass and bulge properties. Preliminary imaging of the type proposed here must be done, sooner or later, if we are to make progress in this exciting new field. Second, we will investigate a number of issues related to extragalactic star formation. Specifically, we will systematically characterize the properties of H II regions and super star clusters on all galactic scales, from circumnuclear regions to the large-scale disk. ACS/WFC 9842 A Snapshot Search for Halo Very-Low-Mass Binaries We propose a snapshot search for binary M subdwarf stars. These nearby stars have high velocities and low metallicies that identify them as members of the old Galactic halo {Population II}. ACS imaging is requested to search for secondary companions. This supplements a previous snapshot program that only obtained 10 observations. The observed binary fraction will be compared to the disk M dwarf fraction to look for differences in star formation. It is likely that a system suitable for orbital mass determinations will be found. In this case, future HST observations could determine the first masses for very-low-mass, low-metallicity stars. ACS/WFC 9891 A snapshot survey of rich stellar clusters in the Large and Small Magellanic Clouds Rich stellar clusters are vital to a wide variety of astrophysical research, from stellar evolution studies to the formation and evolution of galaxies. In this context, it is important to understand how rich star clusters form and evolve. The cluster systems in the LMC and SMC are particularly important in achieving this, because they are the only systems which contain clusters at all stages of evolution while being close enough to be studied as fully resolved stellar populations - although in general this requires the capabilities of HST. We have recently investigated the structural evolution of LMC and SMC clusters using archival WFPC2 data, and demonstrated a dramatic trend in the sizes of these clusters with age. We have shown that this trend likely represents genuine structural evolution in these clusters, although it is not clear whether we are observing a dynamical process or the signature of changing formation conditions. This result has implications for all astronomical research involving massive stellar clusters. To develop this work further requires the extension of our two samples, so that they are statistically quantifiable. This will allow a number of key questions regarding the structural evolution trend to be answered. We propose a two-colour ACS/WFC SNAP survey of rich Magellanic Cloud clusters to achieve this aim. The unique resolution and sensitivity of ACS/WFC is required for success, because of the crowded nature of the targets. The SNAP data will have a large number of additional applications, both to globular cluster and Magellanic Cloud research. ACS/WFC 9902 The Evolution of the Host Galaxies of Radio-Quiet Quasars Study of the host galaxies and environments of high redshift AGN is proving a valuable probe of current theories of how galaxies form and evolve. Results from our NICMOS imaging program have indicated that the hosts of z ~ 2 -- 3 faint radio-quiet quasars {RQQ} have luminosities only around local L*, making them similar to Lyman-break field galaxies at the same redshifts, and to the low-z hosts RQQ hosts. This is roughly consistent with theoretical predictions of Kauffmann & Haehnelt {2000} for the hierarchical buildup of galaxy hosts and their relation to their resident supermassive black holes. The luminosity of the AGN in these RQQ is key to understanding this relationship, however, and we are making a comprehensive archival HST imaging study of the hosts of RQQs from low to high z at a range of nuclear luminosities. At intermediate z, however, there are no studies of the hosts of RQQs in the faint luminosity range that represents the bulk of the quasar population. In the present proposal, we request imaging at the same rest-wavelengths as our high-z sample of the hosts of 10 similarly luminous RQQs at z ~ 0.9. These data will fill in an important part of the parameter space defined by quasar luminosity and redshift. Combined with existing HST data they will allow us to trace the evolution of the hosts of RQQ and that of the relationship between quasar luminosity and host galaxy luminosity. ACS/WFC/HRC 9905 The Host Galaxies of Type II Quasars Type II quasars are the luminous analogues of Type II Seyferts; the central engines are presumably heavily obscured by dust. We have defined a sample of 9 highly luminous Type II quasar candidates with 0.24 z 0.40 from the spectroscopic data of the Sloan Digital Sky Survey, which have high equivalent width, narrow emission-line spectra characteristic of a nonthermal continuum. We estimate that the obscured AGN in these objects have optical luminosities of order 10^{12} solar luminosities. We propose to image this sample in rest-frame U, B and V, to determine the morphology and color of the host galaxies, and look for recent star formation. We will also probe the extended environments of these objects, to determine whether they are undergoing interactions with close companions, and whether they live in appreciably clustered environments. 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 9883 Parallaxes of Extreme Halo Subgiants: Calibrating Globular Cluster Distances and the Ages of the Oldest Stars The ages of the oldest stars are a key constraint on the evolution of our Galaxy, the history of star formation, and cosmological models. These ages are usually determined from globular clusters. However, it is alternatively possible to determine ages of extreme Population II subgiants in the solar neighborhood based on trigonometric parallaxes, without any recourse to clusters. This approach completely avoids the vexing issues of cluster distances, reddenings, and chemical compositions. There are 3 known nearby, extremely metal-deficient Pop II subgiants with Hipparcos parallax errors of 6-11% which are available for such age determinations. At present, based on the latest isochrones, the derived ages of these stars {HD 84937, HD 132475, and HD 140283} are all close to 14 Gyr, uncomfortably close to or higher than current estimates of the age of the universe. However, the errors in the Hipparcos parallaxes imply uncertainties of at least 2 Gyr in the ages of the 3 stars. We propose to measure parallaxes of these three Pop II subgiants using HST's Fine Guidance Sensor 1R. We expect to reduce the Hipparcos parallax error bars by factors of 5-6, providing the most stringent test yet of current theoretical stellar models of Pop II stars and pushing the age uncertainties to below 0.5 Gyr. These data will also provide a major new constraint on the distance scale of globular clusters, with wide implications for stellar evolution and the calibration of Pop II standard candles. HST 9382 A Large Targeted Survey for z 1.6 Damped Lyman Alpha Lines in SDSS QSO MgII-FeII Systems. We have searched the first public release of SDSS QSO spectra for low-z {z1.65} metal absorption lines and found over 200 large rest equivalent width MgII-FeII systems. Previously, we empirically showed that such systems are good tracers of large neutral gas columns, with ~50% being classical damped Lyman alpha {DLA} systems {N_HI=2*10^20 cm^-2}. Here we propose to follow up a well-defined subset of 79 of them to search for DLAs with 0.47z1.60. Only QSOs brighter than g'=19 were selected. The QSO emission and DLA absorption redshifts were constrained to virtually eliminate data loss due to intervening Lyman limit absorption. Consequently, we expect to discover ~40 new DLAs, which is a three-fold increase in this redshift interval. This will significantly improve our earlier low-z DLA statistical results on their incidence, cosmological mass density, and N_HI distribution. The results will also allow us to better quantify the empirical DLA -- metal-line correlation. With this improved understanding, the need for follow-up UV spectroscopy will lessen and, with the release of the final database of SDSS QSO spectra {an ~25-fold increase}, the number of low-z DLAs could be increased arbitrarily. Thus, the power of the large and statistically-sound SDSS database in combination with a proven technique for finding low-z DLAs will, over the next few years, essentially solve the problem of making an accurate determination of the cosmic evolution of the neutral gas component down to z~0.4. 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 9606 CCD Dark Monitor-Part 2 Monitor the darks for the STIS CCD. STIS 9855 Exploring Interstellar Krypton Abundance Variations at Kiloparsec Scales We propose to obtain high-resolution STIS echelle observations of the interstellar Kr I 1236 absorption toward eight stars situated in the Galactic disk beyond the Carina/Sagittarius or Perseus Arms. The measurement of interstellar krypton abundances is a relatively simple way to investigate elemental abundance variations in the Galaxy, since its dominant form is neutral and it is undepleted in the ISM. Furthermore, the intrinsic strengths of krypton's UV resonance lines combined with its low relative abundance to hydrogen produce weak, unsaturated features in typical Galactic sight lines. Previous GHRS and STIS measurements have demonstrated that Kr/H abundance ratios within the local spiral arm, the Orion Spur, are remarkably uniform; however, anomalously high krypton abundances have been measured for the only two sight lines extending also through gas outside the Orion Spur. This program is designed to determine whether these sight lines are isolated cases of enrichment, or if they are representative of large scale krypton abundance variations outside the local arm. Since krypton is undepleted in the ISM, these observations will also be relevant to the study of total elemental abundance and depletion variations for a variety of elements with resonance lines between 1170 and 1372 Angstroms. STIS 9633 STIS parallel archive proposal - Nearby Galaxies - Imaging and Spectroscopy Using parallel opportunities with STIS which were not allocated by the TAC, we propose to obtain deep STIS imagery with both the Clear {50CCD} and Long-Pass {F28X50LP} filters in order to make color-magnitude diagrams and luminosity functions for nearby galaxies. For local group galaxies, we also include G750L slitless spectroscopy to search for e.g., Carbon stars, late M giants and S-type stars. This survey will be useful to study the star formation histories, chemical evolution, and distances to these galaxies. These data will be placed immediately into the Hubble Data Archive. STIS 9708 STIS Pure Parallel Imaging Program: Cycle 11 This is the default archival pure parallel program for STIS during cycle 11. STIS 9786 The Next Generation Spectral Library We propose to continue the Cycle 10 snapshot program to produce a Next Generation Spectral Library of 600 stars for use in modeling the integrated light of galaxies and clusters. This program is using the low dispersion UV and optical gratings of STIS. The library will be roughly equally divided among four metallicities, very low {[Fe/H] lt -1.5}, low {[Fe/H] -1.5 to -0.5}, near-solar {[Fe/H] -0.3 to 0.1}, and super-solar {[Fe/H] gt 0.2}, well-sampling the entire HR-diagram in each bin. Such a library will surpass all extant compilations and have lasting archival value, well into the Next Generation Space Telescope era. Because of the universal utility and community-broad nature of this venture, we waive the entire proprietary period. STIS/CCD/MA1 9784 The rarest of sightlines: probing the metallicity of a DLA with a nearby Low Surface Brightness galaxy We seek to measure the gas-phase metallicity, dust content, and gas kinematics in the interstellar medium {ISM} of the Low Surface Brightness {LSB} galaxy SBS 1543+593, by observing absorption lines in the spectrum of the background QSO HS 1543+5921. The QSO shines directly through the center of the LSB galaxy, producing a damped Lyman-alpha {DLA} line. This is the lowest redshift DLA system known outside of the local group. Specifically, we wish to use the G140M grating of STIS to: a} determine the metallicity of the interstellar gas in the LSB galaxy by accurately measuring the column densities of neutral hydrogen and sulphur; and b} estimate the amount of dust present from a precise measure of the nickel column density. The grating settings chosen to accomplish these goals will also allow us to: c} characterize the kinematics of cool gas in the disk and halo of the LSB galaxy by observing the line profiles of strong low ionization species {Si II, O I, C I, C II, etc.}; and d} search for absorption from NV which may arise in any highly ionized component of the ISM due to accretion of intragroup gas onto the galaxy. STIS/CCD/MA1 9894 UV Spectroscopic Observations of Luminous Narrow-line Seyfert 1 Galaxies Narrow-line Seyfert 1 galaxies {NLS1s} have remarkably different properties than Active Galactic Nuclei with broad optical lines. The most promising explanation for this behavior is that NLS1s have a higher accretion rate relative to Eddington {L/M} than do broad-line Seyferts. Despite uniformity in optical line properties, detailed analysis reveals a divergence of the UV emission line properties that can be traced differences in the shape of the continuum. A link with similarly divergent X-ray properties suggests that there may be variations in L/M even among NLS1s. To test this scenario, we propose UV spectroscopic of two X-ray extreme NLS1s. These observations offer the opportunity to advance our understanding in the scatter in the relationship between line width and black hole mass, to understand physics of gas in AGN optical and UV emission-line regions, and to understand recently-discovered peculiar line-less high-z quasars that may be the early universe counterpart of luminous NLS1s. STIS/CCD/MA1 9876 Where is the Local Hot Gas? We wish to sample the absorption characteristics of 3 lines-of-sight in the local interstellar medium to establish the physical location of the production sites of the highly ionized absorption lines of CIV, SiIV and NV. Such lines are formed at gas temperatures of ~ 100, 000K and all have been widely observed throughout the Galaxy. However, evidence for the formation of any of these high ions within the hot gas of the Local Bubble {LB} remains inconclusive, supporting the similar lack of detections of the OVI ion {T ~ 300, 000K} within 100pc recently reported by the FUSE satellite. Using our recently gained information on the contours of the neutral boundary to the LB, we have selected 3 pairs of stars located just within, and just beyond the LB boundary. We shall test whether high ionization ions are formed either {a} beyond the LB boundary in more distant interstellar bubbles of hot gas, {b} at the conductive interface of the LB neutral boundary, or {c} at possible conductive interfaces between hot gas within the LB and the diffuse clouds embedded within it. Hopefully, these observations will enable theorists to better model the {anomalous} ionization state, pressure and chemical abundance of the local interstellar gas and will assist in the interpretation of data soon to be gained from the NASA CHIPS mission. WFPC2 9710 POMS Test Proposal: WFII backup parallel archive proposal This is a POMS test proposal designed to simulate scientific plans. 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. WFPC2 9458 Probing the Formation & Evolution of M31's Outer Disk and Halo The fossil record of galaxy formation and evolution is imprinted on the spatial distribution, ages and metallicities of galactic stellar populations. The observations proposed here build significantly upon our extensive ground-based and archival WFPC2 programs and aim to constrain the formation and evolution of our nearest large neighbor, M31. We propose deep imaging of 8 fields in the outer disk and halo, several of which have been identified from our panoramic ground-based CCD survey {covering ~ 26 square degrees} to possess significant stellar density and/or potential metallicity variations. Deep colour-magnitude diagrams reaching ~2-3 magnitudes below the horizontal branch will be constructed, allowing detailed characterization of the luminous evolved stellar populations via the red giant metallicity distribution, the luminous asymptotic giant branch, the horizontal branch morphology and the red clump, as well as the detection of a main-sequence that may be present from any younger component. Our primary goals are to: {i} quantify the stellar population variations associated with M31 halo substructure, including the newly- discovered giant stellar stream, and {ii} derive stringent constraints on the age and metallicity of stars in the far outer disk. These observations will directly address two key predictions of cold dark matter hierarchical galaxy formation models. 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. WFPC2 9589 WFPC2 Decontaminations and Associated Observations Pt. 1/3 This proposal is for the monthly WFPC2 decons. Also included are instrument monitors tied to decons: photometric stability check, focus monitor, pre- and post-decon internals {bias, intflats, kspots, & darks}, UV throughput check, VISFLAT sweep, and internal UV flat check. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) None COMPLETED OPS REQs: None OPS NOTES EXECUTED: None ************************ SCHEDULED**** SUCCESSFUL*** FAILURE TIMES FGS GSacq************ 22*********************** 22 FGS REacq************ 25*********************** 25 FHST Update********** 36*********************** 35**************** 221/1321z LOSS of LOCK SIGNIFICANT EVENTS: NCC cool down proceeding exceptionally well.* Physical response from the Cryocooler loop indicated surging ended @ approximately 220/05:55Z at a Turboalternator Inlet temperature of 85.9 K.* Four hours later, temperature dropped below 82 K allowing the FSW authority over the full range of compressor speed, up to 7300 rps.* All indications continue to point to a cool down significantly faster than during SMOV-3B. HST Command Timing testing scheduled 223/11:00Z - 20:00Z with GDOC, SOC, HITT, and CCS using CCS "B" String with CCS Release 4.0.2.2 and PRD D06300 and CCS "D" String with CCS Release 5.0.3 and PRD D06300S.* The purpose of this testing is to run comparison testing with CCS Release 5.0.3 on the "D" String and CCS Release 4.0.2.2 on the "C" String. |
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