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Daily 3584
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3584 PERIOD COVERED: DOYs 93-95 OBSERVATIONS SCHEDULED ACS/HRC 9987 Coronagraphic search for disks around nearby stars We will use the coronagraphic and imaging modes of the High Resolution camera to study of the role of circumstellar disks in planetary system formation over timescales of ~1-1000 Myr. Our targets comprise pre Main-Sequence {MS} and MS stars, selected by infrared excess, and targets selected from SIRTF surveys. Some targets, like Beta Pictoris have debris disks that have been detected at optical or near-IR wavelengths, while others have disks inferred from mid-IR or ISO observations. We will obtain multicolor images of each target's circumstellar environment for the purpose of {1} detecting and characterizing disk morphologies over all scales {including warps and regions of enhanced or depleted density}, and {2} seeking evidence of embedded planets. Direct and occulted images will be recorded for studying the disks within 2 arcseconds of these targets; the coronagraph will be used to image the outer regions of the disks. Together with existing infrared observations, we will provide constraints on the sizes, distribution, and composition of dust grains. FGS 9972 Calibrating the Mass-Luminosity Relation at the End of the Main Sequence We propose to use HST-FGS1R to calibrate the mass-luminosity relation {MLR} for stars less massive than 0.2 Msun, with special emphasis on objects near the stellar/brown dwarf border. Our goals are to determine M_V values to 0.05 magnitude, masses to 5 than double the number of objects with masses determined to be less than 0.20 Msun. This program uses the combination of HST-FGS3/FGS1R at optical wavelengths and ground-based infrared interferometry to examine nearby, subarcsecond binary systems. As a result of these measurements, we are deriving high quality luminosities and masses for the components in the observed systems, and characterizing their spectral energy distributions from 0.5 to 2.2 Mum. Several of the objects included have M 0.1 Msun, placing them at the very end of the stellar main sequence. Three of the targets are brown dwarf candidates, including the current low mass record holder, GJ 1245C, with a mass of 0.062 +/- 0.004 Msun. The payoff of this proposal is high because all 10 of the systems selected have already been resolved with HST- FGS3/FGS1R during Cycles 5--10 and contain most of the reddest objects for which masses can be determined. FGS 9880 The Masses of the O-type Binary 15 Monocerotis The O-type star 15 Mon {HD 47839} was recently discovered to be an astrometric and spectroscopic binary with a period of 25 years; it is the first known O-star system to bridge the observational gap between the period regimes normally probed by these techniques. An analysis of both the radial velocity curve and astrometric orbit yields the masses of the components and distance to the system. Continuing radial velocity and HST/FGS astrometric measurements will lead to a definitive orbit and yield key information about the masses of O-type stars. FGS TRANS mode measurements of separation, position angle, and magnitude difference {begun in Cycle 5} are needed to link existing speckle observations and anticipated observations with the CHARA Array optical interferometer. In addition, field astrometry measurements {FGS POS mode} will provide the proper motion, parallax, and the binary motion around the center of mass. The POS data will provide an accurate estimate of the mass ratio and an improved estimate of distance, and taken together with the spectroscopic and astrometric orbital data, we will obtain masses for both components accurate to a few percent. FGS 9879 An Astrometric Calibration of the Cepheid Period-Luminosity Relation We propose to measure the parallaxes of 10 Galactic Cepheid variables. When these parallaxes {with 1-sigma precisions of 10% or better} are added to our recent HST FGS parallax determination of delta Cep {Benedict et al 2002}, we anticipate determining the Period-Luminosity relation zero point with a 0.03 mag precision. In addition to permitting the test of assumptions that enter into other Cepheid distance determination techniques, this calibration will reintroduce Galactic Cepheids as a fundamental step in the extragalactic distance scale ladder. A Period-Luminosity relation derived from solar metallicity Cepheids can be applied directly to extragalactic solar metallicity Cepheids, removing the need to bridge with the Large Magellanic Cloud and its associated metallicity complications. WFPC2 9870 Low Mass Star Formation at Low Metallicity: Accretion Rates of Pre-Main Sequence Stars in the Large Magellanic Cloud As part of an ongoing effort to characterize the process of star formation at low metallicity, we propose to measure by means of U-band excess the current accretion rate for a homogenous sample of newly-born stars in NGC 1850, a young {5 Myr} stellar cluster in the LMC. Clearly, at this age most of the accretion has already taken place and its intensity is declining with respect to the earliest stages of formation. However, a comparison with Galactic Pre-Main Sequence stars of the same age immediately leads to assessing the relative strength of accretion when the metallicity is decreased by a factor of three. We have already analyzed the images available in the archive for these fields and we have determined the basic parameters {effective temperature and luminosity} for all of the stars down to a mass of ~0.9 Mo. To take the next step and determine the current accretion rate we only need WFPC2 imaging of NGC 1850 in the F336W passband. With three orbit worth of observations, we will reach m{F336W}~23 with an accuracy of 0.1 mag. In spite of their unique scientific potential, the data we apply for are relatively inexpensive to gather, as they are the last missing tile of a large dataset already available in the HST archive. ACS/HRC 9869 X-ray-Bright, Optically Normal Galaxies: The Hidden Truth Chandra has resolved most of the 2 keV X-ray background {XRB} into discrete sources. Ground-based optical studies of these sources have revealed a substantial population of apparently normal galaxies at modest redshift, not the Seyfert 2 galaxies predicted by models for the origin of the XRB. These objects have X-ray spectral properties and luminosities similar to Seyfert 2s, but emission lines are weak or absent in their starlight-dominated optical spectra, suggesting the emergence of a new class of obscured or gas-poor AGNs at moderate redshifts. However, most of the galaxies in question are distant enough that their angular sizes are comparable to the slit widths used in ground-based spectroscopic observations. Thus, it is possible that these "normal" galaxies are classical Seyfert 2s whose nuclear spectral features have been overwhelmed {"hidden"} by host galaxy light. The high angular resolution of HST/STIS offers a unique opportunity to isolate the nuclei of these objects spatially. STIS spectra of a small, carefully selected sample of optically "normal" X-ray galaxies will help clarify the origin of the XRB, which is vital for understanding the growth of supermassive black holes in galactic nuclei. ACS/WFC/WFC2 9857 A tailored survey of proplyds with the ACS While our specific understanding of the proto-planetary disks in Orion is increasing, our general knowledge of what promotes and hinders their birth and longevity is hampered by having good observations in only this one region. Observations of proplyds in other regions with different conditions of ultraviolet irradiation and age can provide more stringent tests of our present models. We have therefore designed an ACS/WFC and parallel WFC2 survey of open clusters embedded in H II regions that, with a small number of orbits, maximizes the probability of successfully finding proplyds there. Our observing strategy will additionally afford a quantitative study of the detected proplyds, as well as the derivation of a correlation between those characteristics and the clusters' stellar population. ACS gives us an unprecedented opportunity to kick start the mass discovery of proplyds in many environments, an obvious way in which progress can be made in this field. This small tailored survey, gives us an excellent chance to obtain a huge return at low cost. 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. 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. ACS/WFC/HRC 9771 The local Hubble flow and the density field within 6 Mpc Great progress has been made recently in accurate distance measurements of nearby galaxies beyond the Local Group based on the luminosity of the tip of the red giant branch {TRGB}. Over the last three years, snapshot surveys with HST have provided us with the TRGB distances for more than a hundred nearby galaxies obtained with an accuracy of about 10%. The local velocity field within 5 Mpc exhibits a significant anisotropy which disagrees with a spherical Virgo-centric flow. The local Hubble flow is very cold, with 1-D rms deviations of ~30 km/s. Cosmological simulations with Cold Dark Matter can only realize such low dispersions with a combination of a low mean density of matter and a substantial component with negative pressure. There may be a constraint on the equation of state w=-p/rho. Our observations will concentrate on 116 galaxies whose expected distances lie within 4 - 6 Mpc, allowing us to trace a Dark Matter distribution in the Local Volume with twice the information currently available. The program is a good one for SNAP mode because the order and rate that the observations are made are not very important, as long as there is good completion over several years. WFPC2 9740 CIII] Imagery of Planetary Nebulae and HII Regions -- A Snap Program We propose to undertake a SNAP program of WFPC2 imagery of several planetary nebulae and extragalactic HII regions with the F185W filter to study the spatial variation of the CIII] 1909 Angstrom emission lines across the nebulae. Much of our current knowledge of carbon abundances in planetary nebulae and HII regions are based on UV spectroscopic observations of this line yet there have not been any studies of its spatial variations in nebulae compared to several of the prominent optical lines {e.g. [OIII] 5007 Angstroms}. Such observations, coupled with photoionization modeling of the nebulae, will enable us to assess the utility of using the CIII] line in abundance calculations of C/O and C/H in nebulae and possibly permit improved empirical emission-line diagnostic techniques for ionization corrections to get the elemental carbon abundances from C++/O++ observations based on CIII]/[OIII] 1909/5007. We also plan to study the spatial variation of the CIII] 1909 Angstrom collisionally excited lines against the CII 4267 Angstrom permitted line in many of the nebulae using previous and planned ground-based longslit echelle spectroscopy coupled with the HST WFPC2 F185W imagery. ACS/WFC 9727 Exploration of the SN Ia Hubble Diagram at z 1.2 In the spirit of a Treasury proposal, we propose to organize, and deliver to the astronomical community, non-proprietary follow-up observations of ~10 Type Ia supernovae at 1z1.7 that are expected to be discovered in a Cycle 12 Treasury proposal. Together with the currently available sample, this would provide a Hubble diagram with over 20 SNe Ia in this redshift range, where it is possible to test the current cosmological model in the epoch of deceleration: If z ~ 0.5 SNe Ia are fainter due to evolution rather than an accelerating expansion, they should continue to get fainter at even higher redshifts. This size sample will show trends and outliers, and permit a more rigorous treatment of the asymmetric amplification distribution from gravitational lensing. This is a key redshift range for the studies of dark energy that will be done with future surveys {and future instruments now being designed}; this dataset will lay the ground-work for these studies by establishing the simple properties of the supernovae in this redshift range, including magnitudes, colors, and timescales. If considered more appropriate, this proposal could be treated as a part of a Treasury or Director's Discretionary program, since the data would be available to everybody immediately, and we would welcome others who would want to work with us on it. ACS/WFC 9722 Life in the fast lane: The dark-matter distribution in the most massive galaxy clusters in the Universe at z0.5 We propose two-filter ACS observations of a complete sample of 12 very X-ray luminous galaxy clusters at 0.5z0.7 as a cornerstone of a comprehensive multi-wavelength study of the properties of the most massive clusters in the universe. Our sample includes the famous systems Cl0016+16 and MS0451-03; all other clusters are new discoveries from the MACS survey. Being the counterparts of the best-studied systems at lower and higher redshift and comprising ALL massive clusters at 0.5z0.7 observable from Mauna Kea this sample will become the ultimate reference for cluster studies at z0.5. HST's unique capabilities will allow us to: 1} measure accurately the clusters' dark matter distribution on scales from tens to more than 500/h_50 kpc from observations of strong and weak gravitational lensing, 2} use galaxy-galaxy lensing to measure the shape, extent, and mass content of the dark-matter halos of both cluster and field galaxies, and 3} study the color morphology of mergers and the star formation history of galaxies in a high-density environment. The proposed observations are complemented by Chandra observations of all our targets {all 12 awarded, 11 executed to date} which provide independent constraints on the dark matter and gas distribution in the cluster cores, as well a by extensive groundbased observations of weak lensing on yet larger scales, galaxy dynamics, and the SZ effect. 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. 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. ACS/WFC 9575 Default {Archival} Pure Parallel Program. The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels in POMS. 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/ NIC1/NIC2/NIC3 8792 NICMOS Post-SAA calibration - CR Persistence Part 3 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. S/C 10097 NICMOS Temperature Setpoint Darks NICMOS darks at different temperatures are needed to calibrate the software tool used to create synthetic darks. Synthetic darks are used during calibration. The temperatures of the NICMOS detectors will be adjusted by +0.5 to -1.0 K from the nominal operating temperature. Darks in each camera will be obtained at each of the temperature settings. At the end of the Proposal the NCS nominal setpoint temperature for the NICMOS detectors will be increased by 0.07 K for the cool season {routine seasonal adjustment}. STIS/CCD 10096 STIS Pure Parallel Imaging Program: Cycle 12 This is the default archival pure parallel program for STIS during cycle 12. STIS/CCD 10085 STIS Pure Parallel Imaging Program: Cycle 12 This is the default archival pure parallel program for STIS during cycle 12. WFPC2 10084 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 10073 Earth Flats This proposal monitors flatfield stability. This proposal obtains sequences of Earth streak flats to construct high quality flat fields for the WFPC2 filter set. These flat fields will allow mapping of the OTA illumination pattern and will be used in conjunction with previous internal and external flats to generate new pipeline superflats. These Earth flats will complement the Earth flat data obtained during cycles 4-11. WFPC2 10070 WFPC2 CYCLE 12 Supplemental Darks Part 2/3 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 10060 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/HRC 10050 ACS Earth Flats High signal sky flats will be obtained by observing the bright Earth with the HRC and WFC. These observations will be used to verify the accuracy of the flats currently used by the pipeline and will provide a comparison with flats derived via other techniques: L-flats from stellar observations, sky flats from stacked GO observations, and internal flats using the calibration lamps. Weekly coronographic monitoring is required to assess the changing position of the spots. STIS/CCD 10026 STIS Sparse Field CTE test-internal {Cycle 12} CTE measurements are made using the "internal sparse field test", along the parallel axis. The "POS=" optional parameter, introduced during cycle 11, is used to provide off-center MSM positionings of some slits. All exposures are internals. STIS/CCD 10020 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/CCD 10018 CCD Dark Monitor-Part 2 Monitor the darks for the STIS CCD. WFPC2/ACS/HRC/WFC 10013 Focus Monitor The focus of HST is measured from WFPC2/PC and ACS/HRC images of stars. Multiple exposures are taken in parallel over an orbit to determine the influence of breathing on the derived mean focus. Observations are taken of clusters with suitable orientations to ensure stars appear in all fields. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) None COMPLETED OPS REQs: 17107-1 Battery 2 Capacity Test Script @ 093/14:39:09z OPS NOTES EXECUTED: NONE SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 32 32 FGS REacq 11 11 FHST Update 40 40 LOSS of LOCK SIGNIFICANT EVENTS: Battery 2 has sufficiently recovered from discharge to 15 Volts and Voltage, pressure, and load share are in family with the other batteries. Placed Battery 2 in FSW 6-battery system @ 093/14:30Z. The SOC 1 safing test was successfully modified to represent a 6-battery system and the BM SOC was reset to 313 A-h. Battery 2, K2 SPA Trim Relay (+AA) was unmasked and the proper charge optimization scheme was reinstated (OR 17107-1). The EPS is now in its nominal configuration in both FSW and hardware. EPS SEs continued to monitor the system for two orbits. The current integrated capacity for Battery 2 (as measured through the 5.1 Ohm resistor) is 54.78 A-h. This battery was last tested in May 2003 and yielded a capacity of 58.9 A-h. STIS MAMA 1 Fold Test (Proposal 10035) using HITM2 Lamp, 096/10:00Z - 10:52Z and MAMA 2 Fold Test using HITM1 Lamp, 096/11:02Z - 11:53Z via SMS. |
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