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Daily 3495
HUBBLE SPACE TELESCOPE
DAILY REPORT # 3495 PERIOD COVERED: DOYs 325-327 OBSERVATIONS SCHEDULED 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. FGS 9970 The Best Brown Dwarf Yet?: FGS Astrometry of the Companion to the Hyades Eclipsing Binary V471 Tau The analysis of over 30 yr of 161 eclipse timings of the Hyades eclipsing binary V471 Tauri shows the presence of a low mass tertiary companion. A third body was found from periodic variations in the observed arrival times of the eclipses - known as the ``light time'' effect. The light time effect occurs as the relative distance {and light travel time} changes as the eclipsing binary moves around the barycenter of the triple system. Our analysis yields an orbital period of P_3=30.5+/-1.6 yr, e_3=0.31+/-0.04, a semi-major axis of a_3=11.2+/-0.4 AU, and a tertiary mass M_3 sin i_3 =0.039+/- 0.004 Mo. For orbital inclinations 35 degrees the mass of the third body would be below the stable hydrogen burning limit of M~0.07 Mo and thus would be a brown dwarf. We propose HST/FGS observations of V471 Tau over the next 3 years {2 HST orbits/year} to determine its astrometric orbit. These HST observations, when combined with Hipparcos astrometry and the light time orbit, will unambiguously yield the orbital inclination and the mass of the third body. The identification of a brown dwarf in V471 Tau will provide the first direct dynamical mass determination of a brown dwarf with a known age {tau{Hyades}=625 Myr}, chemical composition, and distance. In a few years {near maximum elongation}, it should be feasible to obtain IR images and spectra of this object that will provide crucial tests of brown dwarf models. 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. NIC/NIC3 9865 The NICMOS Parallel Observing Program We propose to continue managing the NICMOS pure parallel program. Based on our experience, we are well prepared to make optimal use of the parallel opportunities. The improved sensitivity and efficiency of our observations will substantially increase the number of line-emitting galaxies detected. As our previous work has demonstrated, the most frequently detected line is Halpha at 0.7z1.9, which provides an excellent measure of current star formation rate. We will also detect star-forming and active galaxies in other redshift ranges using other emission lines. The grism observations will produce by far the best available Halpha luminosity functions over the crucial--but poorly observed--redshift range where galaxies appear to have assembled most of their stellar mass. This key process of galaxy evolution needs to be studied with IR data; we found that observations at shorter wavelengths appear to have missed a large fraction of the star-formation in galaxies, due to dust reddening. We will also obtain deep F110W and F160W images, to examine the space densities and morphologies of faint red galaxies. In addition to carrying out the public parallels, we will make the fully reduced and calibrated images and spectra available on-line, with some ground-based data for the deepest parallel fields included. STIS/CCD/MA1 9848 A SNAPSHOT Survey of Sharp-Lined Early B-Type Stars Although spectrum synthesis studies of the UV spectra of sharp-lined main sequence B stars provide us with some our best determinations of the abundances of the Fe group and neutron capture elements and the chemical evolution in our galaxy and the Magellanic Clouds, the HST archive is virtually devoid of high resolution spectra of the bright nearby B stars that have become to be regarded as abundance standards. For example, there are NO observations of HR 1886, iota Her, and tau Her, the sharpest-lined representatives {V sin i 5 km/s} of spectral classes B1 V, B3 IV-V and B5 IV, and only a few tiny spectral intervals of gamma Peg {B2 IV}. Information on the abundances of the Fe group is important for computing opacities for stellar evolution calculations and for determining astrophysical f-values. There are no suitable galactic standards in the HST database to compare with recent HST/STIS observations of B stars in the Magellanic Clouds and the likely future observations of similar objects in M31 and other nearby galaxies. To correct this deficiency, we propose SNAPSHOT observations with the STIS E140M and E230M gratings of 33 of the best bright abundance standards in nearby clusters and the galactic field. Using this data we will determine the abundances of the Fe group and heavy elements using the technique of spectrum synthesis with LTE and NLTE treatments. We waive the proprietary period. ACS 9831 Multiplicity among brown dwarfs in the Pleiades cluster We have compiled a sample of 32 confirmed brown dwarfs in the Pleiades cluster. We propose to observe this sample with HST/ACS in SNAPSHOT mode in order to search for very low mass multiple systems. Our goals a 1} to determine the occurrence and frequency of binary systems among substellar objects, which hold important clues to the formation and evolution mechanism{s} of ultracool and brown dwarfs, 2} to get an estimate of the Initial Mass Function {IMF} at very low masses, which is still unknown and very much needed to be corrected for binarity, 3} to compare the distribution of multiple systems in young open clusters and in the field. NIC3/ACS/HRC/WFC 9803 Deep NICMOS Images of the UDF The ACS Ultra Deep Field {UDF} images will greatly enhance the rich suite of deep multi-wavelength images in the Chandra Deep Field South {CDF--S}. We propose to complete the image set with deep near-IR NICMOS images at 1.1 and 1.6 microns over a significant fraction of the UDF, providing a critical link between the HST ACS and SIRTF observations. The timely addition of the near-IR images ensures that investigators will have images that span the spectrum from X-ray to far IR. In recognition of the value of the near IR images this proposal is submitted as a Treasury proposal with no proprietary period. The proposal team will deliver science quality images, mosaiced images covering 4.9 sq arc min, and a photometric catalog complete to an AB mag of 28.2 in both the F110W and F160W filters. The program also delivers a parallel extremely deep ACS field, 8' away, that reaches to within 0.6 mag of the UDF in the same filters as the UDF. The scientific program of the proposal team focuses on the star formation history of the universe, evolved galaxies at high redshift, galaxies at the epoch of reionization, and the redshift evolution of AGNs and ULIRGs. The HDF-N is currently the only field with spatially-coincident deep HST imaging in both the optical and near-IR. The small size of the HDF-N means that large scale structure is the dominant error in the results from the HDF-N. Providing observations in a field that is spatially uncorrelated is critically important. The UDF/CDF-S fulfills that goal. The depth of the UDF ACS imaging, and the wealth of Great Observatory and ground based observations in the CDF-S, make these NICMOS observations uniquely valuable. An extraordinarily rich array of science opportunities await the community from the NICMOS UDF data. ACS/HRC/WFC 9796 Observations of Intermediate Mass Black Hole Candidate Ultra-Luminous X-ray Sources Ultra-luminous X-ray {ULX} sources are off-nuclear point sources in nearby normal galaxies. Variability observed on the timescale of days, weeks, and years signals that ULXS are accreting sources, likely harboring black holes. However, the observed X-ray luminosity of these systems far exceeds the Eddington limit for a 10 Msun black hole; some ULXs may be intermediate mass black holes. The identification and study of optical counterparts with HST will be central to better understanding these objects. We propose to obtain deep U-B-V-I exposures of 4 extremely bright ULXs in nearby spirals: NGC 1313 X-1 and X-2, M81 X-9 {Holmberg II X-1}, and M74 X-1. Each has a 0.5'' Chandra position, and X-ray luminosity and spectral characteristics consistent with expectations for intermediate mass black holes. We will use the colors we obtain, the magnitudes we measure, and any source variability {also, correlated optical-X-ray variability from simultaneous Chandra snapshots} to constrain the nature of the donor stars and the black holes {10 Msun or 100-1000 Msun}, and the formation and evolution scenarios for each system. 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-diaram 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. ACS/HRC/WFC 9773 Ram Pressure Stripping in the Virgo Spiral NGC 4522 We propose to image in BVI with HST ACS/WFC the highly inclined Virgo cluster spiral galaxy NGC 4522, which is perhaps the nearest and clearest case of a galaxy whose interstellar medium {ISM} is being actively stripped by the pressure of the intracluster medium {ICM}. High resolution HST B-I mages of dust in the ISM will show important details of the interaction, such as what happens to giant molecular clouds in the interaction, how rapidly and cleanly disks are stripped, and whether star formation is triggered by ICM pressure. We will identify extraplanar star clusters which formed in the stripped gas, and from their ages and spatial distribution constrain the stripping history of NGC 4522. Only with the spatial resolution of HST can we map dust features down to the few pc scale of GMCs, and clearly identify stars clusters. In-depth study of this galaxy should provide new insight into the physical processes which occur in ICM-ISM interactions, and give us greater understanding of galaxy evolution in clusters of all types and at all redshifts. ACS/HRC/WFC 9770 Galaxy Evolution During Half the Age of the Universe: ACS imaging of rich galaxy clusters Detailed studies of nearby galaxies {z0.05} have shown that galaxies have very complex histories of formation and evolution involving mergers, bursts of star formation, and morphological changes. Even so, the global properties of the galaxies {radii, luminosities, rotation velocities, velocity dispersions, and absorption line strengths} follow a number of very tight {empirical} scaling relations, e.g. the Tully-Fisher relation and the Fundamental Plane. These relations place constraints on models for galaxy evolution. The results for nearby galaxies rely on high signal-to-noise spectroscopy and multi-color photometry. With the Gemini Telescopes and the Hubble Space Telescope {HST} it is possible to carry out similar detailed studies of galaxies at much larger redshifts, up to z~1.0, equivalent to half the age of the Universe. We have started a project using the scaling relations and aimed at studying the galaxy evolution over the last half of the age of the Universe. The project is based on a large database of spectroscopy and photometry of galaxies in 15 X-ray selected clusters of galaxies with redshifts between 0.15 and 1.0. Spectroscopic observations are being obtained using both Gemini Telescopes; we have observed 6 clusters so far, covering from z=0.18 to z=0.83. We propose to use HST/ACS to image the clusters and determine the morphologies and measure the sizes of the galaxies. At this time we ask for 26 orbits to image four of the clusters in our sample. ACS/HRC 9747 An Imaging Survey of the Statistical Frequency of Binaries Among Exceptionally-Young Dynamical Families in the Main Asteroid Belt We propose an ambitious SNAPSHOT program to determine the frequency of binaries among two very young asteroid families in the Main Belt, with potentially profound implications. These families {of C- and S-type} have recently been discovered {Nesvorny et al. 2002, Nature 417, 720}, through dynamical modeling, to have been formed at 5.8 MY and 8.3 MY ago in catastrophic impact events. This is the first time such precise and young ages have been assigned to a family. Main-belt binaries are almost certainly produced by collisions, and we would expect a young family to have a significantly higher frequency of binaries than the background, because they may not yet have been destroyed by impact or longer-term gravitational instabilities. In fact, one of the prime observables from such an event should be the propensity for satellites. This is the best way that new numerical models for binary production by collisions {motivated largely by our ground-based discoveries of satellites among larger asteroids}, can be validated and calibrated. HST is the only facility that can be used to search for binaries among such faint objects {V17.5}. We will also measure two control clusters, one being an "old" family, and the other a collection of background asteroids that do not have a family association, and further compare with our determined value for the frequency of large main-belt binaries {2%}. We request visits to 180 targets, using ACS/HRC. ACS/WFC 9744 HST Imaging of Gravitational Lenses Gravitational lenses offer unique opportunities to study cosmology, dark matter, galactic structure, galaxy evolution and quasar host galaxies. They are also the only sample of galaxies selected based on their mass rather than their luminosity or surface brightness. While gravitational lenses can be discovered with ground-based optical and radio observations, converting them into astrophysical tools requires HST. HST has demonstrated that it is the only telescope that can in each case precisely locate the lens galaxy, measure its luminosity, color and structure, and search for lensed images of the source host galaxy given the typical image separations of ~1''. We will obtain ACS/WFC V and I images and NICMOS H images of 21 new lenses never observed by HST and NICMOS H images of 16 lenses never observed by HST in the IR. As in previous cycles, we request that the data be made public immediately. WFPC2 9712 Pure Parallel Near-UV Observations with WFPC2 within High-Latitude ACS Survey Fields In anticipation of the allocation of ACS high-latitude imaging survey{s}, we request a modification of the default pure parallel program for those WFPC2 parallels that fall within the ACS survey field. Rather than duplicate the red bands which will be done much better with ACS, we propose to observe in the near-ultraviolet F300W filter. These data will enable study of the rest-frame ultraviolet morphology of galaxies at 0z1. We will determine the morphological k-correction, and the location of star formation within galaxies, using a sample that is likely to be nearly complete with multi-wavelength photometry and spectroscopic redshifts. The results can be used to interpret observations of higher redshift galaxies by ACS. 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. STIS/ACS/NICMOS 9430 The Role of Jets in Shaping Planetary Nebulae Recent CO observations of several planetary nebulae {PN} suggest that collimated outflows may play a crucial role in the early shaping of these objects. The idea that jets may be the primary driver of the early development of some PN represents a major shift in thinking about the evolution of these objects. In the past, the role of jets has been considered secondary to the interacting winds scenario, the standard model of PN formation. We propose to use the unique capabilities of HST to access the importance of collimated outflows in the development of the young PN PK166-06D1 {AFGL 618}. We have chosen PK166-06D1 for this study because it is in the early stages of PN formation - the time during which jets would have the greatest impact on PN development. We propose to use STIS, ACS, and NICMOS to characterize the collimated outflows present in PK166- 06D1. The goals of this study a 1} to characterize the interaction of the jets with the surrounding AGB shell by determining the physical conditions in the outflows and the interaction regions, 2} to determine the structure of the surrounding AGB shell using deep optical imaging, 3} to investigate the origin of the collimated outflows by examining the central regions of the nebula. We require both the stability and high spatial resolution capabilities of HST for this project because we will be investigating the detailed structure of compact regions { 1"}. 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. WFPC2 10082 POMS Test Proposal: WFII backup parallel archive proposal This is a POMS test proposal designed to simulate scientific plans WFPC2 10075 WFPC2 CYCLE 12 Intflat and Viflat Sweeps and Filter Rotation Anomaly Monitor Using intflat observations, this WFPC2 proposal is designed to monitor the pixel-to-pixel flatfield response and provide a linearity check. The intflat sequences, to be done once during the year, are similar to those from the Cycle 11 program 9597. The images will provide a backup database in the event of complete failure of the visflat lamp as well as allow monitoring of the gain ratios. The sweep is a complete set of internal flats, cycling through both shutter blades and both gains. The linearity test consists of a series of intflats in F555W, in each gain and each shutter. As in Cycle 11, we plan to continue to take extra visflat, intflat, and earthflat exposures to test the repeatability of filter wheel motions. WFPC2 10069 WFPC2 CYCLE 12 Supplemental Darks, Part 1/3 This dark calibration program obtains 3 dark frames every day to provide data for monitoring and characterizing the evolution of hot pixels. ACS/HRC/WFC 10042 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. STIS/CCD 10019 CCD Bias Monitor - Part 1 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/CCD 10017 CCD Dark Monitor-Part 1 Monitor the darks for the STIS CCD. STIS/CCD 10000 STIS Pure Parallel Imaging Program: Cycle 12 This is the default archival pure parallel program for STIS during cycle 12. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) HSTAR 9217: FHST Update failure and GS Acquisition (2,0,2) failed to Gyro control due to SRLE on FGS 2 @ 326/04:06:14Z. Prior GS Acquisition failure and Full Maneuver Updates (U2,3FM) failures @ 326/03:32:39Z and 326/03:35:24Z both due to FHST 1. FHST Map @ 326/04:53Z showed errors of 51.203, - 64.262, - 60.102. FHST Roll Delay U1,3RD @ 326/05:11:17Z failed due to FHST 1. Subsequent FHST Full Maneuver Updates @ 326/06:20:23Z and 326/06:23:08Z were successful with first update producing results of 21.644, 113.034, 49.638 after Type 2 slew. GS Acquisition @ 326/06:52:22Z was successful. Under investigation. COMPLETED OPS REQs: None OPS NOTES EXECUTED: None SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 15 15 FGS REacq 16 16 FHST Update 30 30 LOSS of LOCK SIGNIFICANT EVENTS: None |
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