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Daily #4033
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT #4033 PERIOD COVERED: UT January 20,21,22, 2006 (DOY 020,021,022) OBSERVATIONS SCHEDULED 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 10772 WF4 Anomaly Characterization A anomaly has been found in images from the WF4 CCD in WFPC2. The WF4 CCD bias level appears to have become unstable, resulting in sporadic images with either low or zero bias level. Calibration images will be obtained to further characterize the anomaly. ACS/HRC 10752 Cycle 14 Focus Monitor The focus of HST is measured primarily with ACS/HRC over full CVZ orbits to obtain accurate mean focus values via a well sampled breathing curve. Coma and astigmatism are also determined from the same data in order to further understand orbital effects on image quality and optical alignments. To monitor the stability of ACS to WFPC2 relative focii, we've carried over from previous focus monitor programs parallel observations taken with the two cameras at suitable orientations of previously observed targets, and interspersed them with the HRC CVZ visits. ACS/HRC 10738 Earth Flats 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 in the pipeline and to monitor any changes. Weekly coronagraphic monitoring is required to assess the changing position of the spots. ACS/HRC/WFC 10729 ACS CCDs daily monitor This program consists of a set of basic tests to monitor, the read noise, the development of hot pixels and test for any source of noise in ACS CCD detectors. The files, biases and dark will be used to create reference files for science calibration. This programme will be for the entire lifetime of ACS. Changes from cycle 13:- The default gain for WFC is 2 e-/DN. As before bias frames will be collected for both gain 1 and gain 2. Dark frames are acquired using the default gain {2}. This program cover the period Oct, 2 2005- May, 29-2006. The second half of the program has a different proposal number: 10758. ACS/WFC 10626 A Snapshot Survey of Brightest Cluster Galaxies and Strong Lensing to z = 0.9 We propose an ACS/WFC snapshot survey of the cores of 150 rich galaxy clusters at 0.3 z 0.9 from the Red Sequence Cluster Survey {RCS}. An examination of the galaxian light in the brightest cluster galaxies, coupled with a statistical analysis of the strong-lensing properties of the sample, will allow us to contrain the evolution of both the baryonic and dark mass in cluster cores, over an unprecedented redshift range and sample size. In detail, we will use the high- resolution ACS images to measure the metric {10 kpc/h} luminosity and morphological disturbances around the brightest clusters galaxies, in order to calibrate their accretion history in comparison to recent detailed simulations of structure formation in cluster cores. These images will also yield a well-defined sample of arcs formed by strong lensing by these clusters; the frequency and detailed distribution {size, multiplicity, redshifts} of these strong lens systems sets strong constraints on the total mass content {and its structure} in the centers of the clusters. These data will also be invaluable in the study of the morphological evolution and properties of cluster galaxies over a significant redshift range. These analyses will be supported by extensive ongoing optical and near-infrared imaging, and optical spectroscopy at Magellan, VLT and Gemini telescopes, as well as host of smaller facilities. ACS/WFC 10624 Solving the Mystery of the Short-Hard Gamma-Ray Bursts Eight years after the afterglow detections that revolutionized studies of the long-soft gamma-ray bursts, not even one afterglow of a short-hard GRB has been seen, and the nature of these events has become one of the most important problems in GRB research. The Swift satellite, expected to be in full operation throughout Cycle 14, will report few-arcsecond localizations for short-hard bursts in minutes, enabling prompt, deep optical afterglow searches for the first time. Discovery and observation of the first short-hard optical afterglows will answer most of the critical questions about these events: What are their distances and energies? Do they occur in distant galaxies, and if so, in which regions of those galaxies? Are they the result of collimated or quasi-spherical explosions? In combination with an extensive rapid-response ground-based campaign, we propose to make the critical high-sensitivity HST TOO observations that will allow us to answer these questions. If theorists are correct in attributing the short-hard bursts to binary neutron star coalescence events, then they will serve as signposts to the primary targeted source population for ground-based gravitational-wave detectors, and short-hard burst studies will have a vital role to play in guiding those observations. ACS/WFC/WFPC2 10594 The Formation of Spiral Spheroids and Their Globular Cluster Systems The assembly history of spiral galaxies remains one of the most pressing questions in astrophysics today. In particular, we do not have a clear picture of the formation mechanism for bulges of spiral galaxies. Are bulges of spirals simply "small ellipticals", formed via rapid dissipative collapse during the early universe? Or is bulge building through secular evolution of inner disk stars a more common mechanism? Is there any dependence on bulge mass? A powerful yet relatively simple way to probe these fundamental questions is by studying the properties of globular cluster {GC} systems of spirals. Specifically, bulge formation via secular evolution is expected not to form GCs, whereas bulge formation via dissipative collapse is. We therefore propose to obtain ACS/WFC imaging as well as ground-based, wide-field imaging of five edge-on Sa spirals which cover a factor ~15 in luminosity/mass, and for which spectroscopic follow-up is feasible. This constitutes the first luminosity-selected sample of early-type spirals, which will allow us to directly probe the dependence of GC properties on the bulge luminosity. We will detect a minimum of ~100-200 GCs per galaxy in the ACS images, sufficient to reveal GC subpopulations, their relative numbers, sizes, and radial distributions. This study will more than double the number of well-studied early-type spiral systems. ACS/WFC 10592 An ACS Survey of a Complete Sample of Luminous Infrared Galaxies in the Local Universe At luminosities above 10^11.4 L_sun, the space density of far-infrared selected galaxies exceeds that of optically selected galaxies. These `luminous infrared galaxies' {LIRGs} are primarily interacting or merging disk galaxies undergoing enhanced star formation and Active Galactic Nuclei {AGN} activity, possibly triggered as the objects transform into massive S0 and elliptical merger remnants. We propose ACS/WFC imaging of a complete sample of 88 L_IR 10^11.4 L_sun luminous infrared galaxies in the IRAS Revised Bright Galaxy Sample {RBGS: i.e., 60 micron flux density 5.24 Jy}. This sample is ideal not only in its completeness and sample size, but also in the proximity and brightness of the galaxies. The superb sensitivity, resolution, and field of view of ACS/WFC on HST enables a unique opportunity to study the detailed structure of galaxies that sample all stages of the merger process. Imaging will be done with the F439W and F814W filters {B and I-band} to examine as a function of both luminosity and merger state {i} the evidence at optical wavelengths of star formation and AGN activity and the manner in which instabilities {bars and bridges} in the galaxies may funnel material to these active regions, {ii} the relationship between star formation and AGN activity, and {iii} the structural properties {AGN, bulge, and disk components} and fundamental parameters {effective radius and surface brightness} of LIRGs and their similarity with putative evolutionary byproducts {elliptical, S0 and classical AGN host galaxies}. This HST survey will also bridge the wavelength gap between a Spitzer imaging survey {covering seven bands in the 3.6-160 micron range} and a GALEX UV imaging survey of these galaxies, but will resolve complexes of star clusters and multiple nuclei at resolutions well beyond the capabilities of either Spitzer or GALEX. The combined datasets will result in the most comprehensive multiwavelength study of interacting and merging galaxies to date. ACS/WFC 10588 The Host Galaxies of Post-Starburst Quasars We propose to use ACS to conduct a snapshot imaging survey of post-starburst quasars now being discovered in signficant numbers by the Sloan Digital Sky Survey. Post-starburst quasars are broad-lined AGN that also possess Balmer jumps and high-n Balmer absorption lines indicative of luminous stellar populations on order of 100 Myr old. These objects, representing a few percent of the z 0.5 quasar population, may be an evolutionary stage in the transition of ultraluminous infrared galaxies into normal quasars, or a type of galaxy interaction that triggers both star formation and nuclear activity. These sources may also illustrate how black hole mass/bulge mass correlations arise. Ground-based imaging of individual poststarburst quasars has revealed merger remnants, binary systems, and single point sources. Our ACS snapshots will enable us to determine morphologies and binary structure on sub-arcsecond scales {surely present in the sample}, as well as basic host galaxy properties. We will be looking for relationships among morphology, particularly separation of double nuclei, the starburst age, the quasar black hole mass and accretion rate, that will lead to an understanding of the triggering activity and mutual evolution. This project will bring quantitative data and statistics to the previously fuzzy and anecdotal topic of the "AGN-starburst connection" and help test the idea that post-starburst quasars are an early evolutionary stage of normal quasars. ACS/WFC 10587 Measuring the Mass Dependence of Early-Type Galaxy Structure We propose two-color ACS-WFC Snapshot observations of a sample of 118 candidate early- type gravitational lens galaxies. Our lens-candidate sample is selected to yield {in combination with earlier results} an approximately uniform final distribution of 40 early-type strong lenses across a wide range of masses, with velocity dispersions {a dynamical proxy for mass} ranging from 125 to 300 km/s. The proposed program will deliver the first significant sample of low-mass gravitational lenses. All of our candidates have known lens and source redshifts from Sloan Digital Sky Survey data, and all are bright enough to permit detailed photometric and stellar- dynamical observation. We will constrain the luminous and dark-matter mass profiles of confirmed lenses using lensed-image geometry and lens-galaxy structural/photometric measurements from HST imaging in combination with dynamical measurements from spatially resolved ground-based follow-up spectroscopy. Hence we will determine, in unprecedented detail, the dependence of early-type galaxy mass structure and mass-to-light ratio upon galaxy mass. These results will allow us to directly test theoretical predictions for halo concentration and star-formation efficiency as a function of mass and for the existence of a cuspy inner dark- matter component, and will illuminate the structural explanation behind the fundamental plane of early-type galaxies. The lens-candidate selection and confirmation strategy that we propose has been proven successful for high-mass galaxies by our Cycle 13 Snapshot program {10174}. The program that we propose here will produce a complementary and unprecedented lens sample spanning a wide range of lens-galaxy masses. ACS/WFC 10579 ULX counterparts: the key to finding intermediate-mass black holes The origin and formation mechanism for supermassive black holes {SMBHs} found in the centres of most, if not all, galaxies remains one of the outstanding questions in astrophysics. Most scenarios involve the presence of massive black holes in the early universe, formed by the collapse of primordial Population III stars. It is predicted that a relic of this population could still be present in galactic halos in the current epoch, possessing masses from a few hundred times solar mass upwards. However, to date no CONCLUSIVE evidence for such a class of "intermediate-mass" black holes has been found. The most likely current candidates are the ultraluminous X-ray sources {ULXs}, which show tantalising evidence for IMBHs {e.g. the extreme X-ray luminosities and low disk temperatures expected from accreting IMBHs}. We propose to address this issue by identifying optical counterparts for six of the nearest ULXs. We will use this programme as a pathfinder for future radial velocity measurements, which will allow the orbital parameters and hence the first undisputed mass constraints for these systems to be determined. ACS/HRC/WFC 10570 Hosts of Quasars with Opaque Partial Covering A few quasars are known to exhibit associated absorption lines with opaque partial covering. These are the lines which are clearly saturated but not completely dark, so that these absorbing clouds are opaquely and partially covering the quasar light. In some cases, ionization parameter and density arguments indicate that the absorbers are on kpc scale. This implies that at least in some cases, the residual, unabsorbed optical {rest-UV} continuum component originates from ~kpc scales, rather than microscopic scales {such as ~100 Schwarzschild radii}. This could be a superluminous host galaxy or starbursting core, and could be resolved by HST. We address the nature of these opaquely and partially covered quasars with a simple and robust ACS imaging. ACS/WFC 10562 Validating a dark galaxy VIRGOHI21 is an object detected in the Virgo Cluster HI survey of Davies et al {2004}, with a velocity width typical of a disc galaxy {220 km/s} but which does not appear to have an optical counterpart down to a surface brightness level of 27.5 B mag/sq. arcsec. Altogether, it is the best ever candidate for a Dark Galaxy. We propose to image this object with the ACS through the F814W filter for 9 orbits to see if this object contains a population of individually very faint stars which would be missed by ground-based telescopes. ACS/HRC 10556 Neutral Gas at Redshift z=0.5 Damped Lyman-alpha systems {DLAs} are used to track the bulk of the neutral hydrogen gas in the Universe. Prior to HST UV spectroscopy, they could only be studied from the ground at redshifts z1.65. However, HST has now permitted us to discover 41 DLAs at z1.65 in our previous surveys. Followup studies of these systems are providing a wealth of information about the evolution of the neutral gas phase component of the Universe. But one problem is that these 41 low-redshift systems are spread over a wide range of redshifts spanning nearly 70% of the age of the Universe. Consequently, past surveys for low-redshift DLAs have not been able to offer very good precision in any small redshift regime. Here we propose an ACS-HRC- PR200L spectroscopic survey in the redshift interval z=[0.37, 0.7] which we estimate will permit us to discover another 41 DLAs. This will not only allow us to double the number of low-redshift DLAs, but it will also provide a relatively high-precision regime in the low-redshift Universe that can be used to anchor evolutionary studies. Fortunately DLAs have high absorption equivalent width, so ACS-HRC-PR200L has high-enough resoultion to perform this proposed MgII-selected DLA survey. ACS/WFC 10543 Microlensing in M87 and the Virgo Cluster Resolving the nature of dark matter is an urgent problem. The results of the MACHO survey of the Milky Way dark halo toward the LMC indicate that a significant fraction of the halo consists of stellar mass objects. The VATT/Columbia survey of M31 finds a similar lens fraction in the M31 dark halo. We propose a series of observations with ACS that will provide the most thorough search for microlensing toward M87, the central elliptical galaxy of the Virgo cluster. This program is optimized for lenses in the mass range from 0.01 to 1.0 solar masses. By comparing with archival data, we can detect lenses as massive as 100 solar masses, such as the remnants of the first stars. These observations will have at least 15 times more sensitivity to microlensing than any previous survey, e.g. using WFPC2. This is due to the factor of 2 larger area, factor of more than 4 more sensitivity in the I-band, superior pixel scale and longer baseline of observations. Based on the halo microlensing results in the Milky Way and M31, we might expect that galaxy collisions and stripping would populate the overall cluster halo with a large number of stellar mass objects. This program would determine definitively if such objects compose the cluster dark matter at the level seen in the Milky Way. A negative result would indicate that such objects do not populate the intracluster medium, and may indicate that galaxy harassment is not as vigorous as expected. We can measure the level of events due to the M87 halo: this would be the best exploration to date of such a lens population in an elliptical galaxy. Star-star lensing should also be detectable. About 20 erupting classical novae will be seen, allowing to determine the definitive nova rate for this giant elliptical galaxy. We will determine if our recent HST detection of an M87 globular cluster nova was a fluke, or indicative of a 100x higher rate of incidence of cataclysmic variables and nova eruptions in globulars than previously believed. We will examine the populations of variable stars, and will be able to cleanly separate them from microlensing. ACS/WFC 10528 Ram Pressure Stripping and Dense Cloud Ablation in the Virgo Spiral NGC 4402 We propose to image in BVI with HST ACS the highly inclined Virgo cluster spiral galaxy NGC 4402, which is an outstanding example of a galaxy undergoing stripping of its ISM by an ICM-ISM interaction. Ground-based images at 0.5" resolution appear to show active dust stripping, triggered star formation, and ablation of dense molecular clouds by the ICM wind. The near side of NGC 4402 contains the leading edge of interaction, giving us a relatively unobscured view of the processes which occur as the ICM wind impacts the ISM. High resolution HST B-I images of dust in NGC 4402 can reveal the fate of giant molecular clouds during a stripping event, including whether clouds above some size get left behind as the rest of the ISM is stripped from around them, how decoupled clouds become ablated by the ICM wind, and how the survival time varies with cloud mass. We will identify and estimate the ages of stars and star clusters in the stripped outer disk and halo, and from the spatial distributions of the younger objects, constrain the stripping history of the galaxy. Its proximity, orientation, stage of evolution, and direction of travel through the ICM make NGC 4402 an outstanding subject for a detailed HST study of ICM-ISM stripping. An in-depth study of this galaxy will provide new insight into the physical processes of ISM-ICM interactions and give us greater understanding of cluster galaxy evolution, both in Virgo and at higher redshifts. ACS/WFC 10523 The Halo Shape and Metallicity of Massive Spiral Galaxies We propose to resolve the stellar populations of the halos of seven nearby, massive disk galaxies using a SNAP survey with WFC/ACS. These observations will provide star counts and color-magnitude diagrams 2-3 magnitudes below the tip of the Red Giant Branch along the two principal axes and one intermediate axis of each galaxy. We will measure the metallicity distribution functions and stellar density profiles from star counts down to very low average surface brightnesses, equivalent to ~31 V-mag per square arcsec. This proposal will create a unique sampling of galaxy halo properties, as our targets cover a range in galaxy mass, luminosity, inclination, and morphology. As function of these galaxy properties this survey will provide:- the first systematic measurement of radial light profiles and axial ratios of the diffuse stellar halos and outer disks of spiral galaxies- a comprehensive analysis of halo metallicity distributions as function of galaxy type and position within the galaxy- an unprecedented study of the stellar metallicity and age distribution in the outer disk regions where the disk truncations occur- the first comparative study of globular clusters and their field stellar populations We will use these fossil records of the galaxy assembly process to test halo formation models within the hierarchical galaxy formation scheme. ACS/WFC 10494 Imaging the mass structure of distant lens galaxies The surface brightness distribution of extended gravitationally lensed arcs and Einstein rings contains super-resolved information about the lensed object, and, more excitingly, about the smooth and clumpy mass distribution of the lens galaxies. The source and lens information can non-parametrically be separated, resulting in a direct "gravitational-mass image" of the inner mass-distribution of cosmologically-distant galaxies {Koopmans 2005}. With this goal in mind, we propose deep HST ACS-F555W/F814W and NICMOS-F160W imaging of 15 gravitational-lens systems with spatially resolved lensed sources, selected from the 17 new lens systems discovered by the Sloan Lens ACS Survey {Bolton et al. 2004}. Each system has been selected from the SDSS and confirmed in a time-efficient HST-ACS snapshot program {cycle-13}; they show highly-magnified arcs or Einstein rings, lensed by a massive early-type lens galaxy. High- fidelity multi-color HST images are required {not delivered by the 420-sec snapshot images} to isolate these lensed images {properly cleaned, dithered and extinction-corrected} from the lens galaxy surface brightness distribution, and apply our "gravitational-mass imaging" technique. The sample of galaxy mass distributions - determined through this method from the arcs and Einstein ring HST images - will be studied to: {i} measure the smooth mass distribution of the lens galaxies {Dark and luminous mass are separated using the HST images and the stellar M/L values derived from a joint stellar-dynamical analysis of each system}; {ii} quantify statistically and individually the incidence of mass-substructure {with or without obvious luminous counter- parts such as dwarf galaxies}. Since dark-matter substructure should be considerably more prevalent at higher redshift, both results provide a direct test of this prediction of the CDM hierarchical structure-formation model. ACS/HRC 10396 Star Clusters, Stellar Populations, and the Evolution of the Small Magellanic Cloud As the closest star forming dwarf galaxy, the SMC is the preferred location for detailed studies of this extremely common class of objects. We therefore propose to use the capabilities of ACS, which provide an improvement by an order of magnitude over what is possible with ground- based optical imaging surveys that are limited by confusion anddepth, to measure key stellar population parameters in the SMC from VI color-magnitude diagrams. Our program focuses on regions where crowding makes HST essential and includes 7 star clusters and 7 field star locations. We will measure accurate ages of the clusters, test stellar evolution models, gain fiducial stellar sequences to use in fitting the field stars, check the form of the IMF, and substantially extend the study of RR Lyrae variables in the key NGC121 SMC globular cluster. The field pointings will allow us to reconstruct the star formation history, look for enhanced star formation that is expected when the SMC interacts with the LMC and/or Milky Way, and compare its main sequence luminosity {and mass} functions with those of the Milky Way, LMC, and UMi dwarf spheroidal. This proposal is part of a coordinated HST and ground-based study of the stellar history and star formation processes in the SMC. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) HSTARS: 10092 - GSAcq (2,3,2) failed due to Search Radius Limit Exceeded @ 020/1441z During ZOE GSacq(2,3,2) scheduled at 020/14:41:37 failed due to search radius limit exceeded on FGS 3. A ESB a07 (FGS Coarse Track Failed - timeout waiting for data valid ) was received. The OBADS were during ZOE. At AOS 020/15:02.28 we were in FN format because of Astrometry. 10093 - GSAcq (2,1,2) results in FLBU (2,0,2) due to Scan Step Limit Exceeded on FGS 1 @ 021/0806z GSAcq (2,1,2) scheduled @ 021/08:06:45 results in FLBU (2,0,2)on FGS 2 due to Scan Step Limit Exceeded on FGS 1. OBAD 1: V1 797.90, V2 3859.79, V3 357.03, RSS 3957.54 OBAD 2: V1 -3.62, V2 -5.54, V3 -10.29, RSS 12.23 OBAD MAP: V1 -1.16, V2, -4.49, V3 -12.51, RSS 13.34 10094 - GSAcq (1,3,3) failed due to Search Radius Limit Exceeded on FGS 1 @ 022/0536z GSAcq (1,3,3) scheduled @ 022/05:36:34 failed due to search radius limit exceeded on FGS 1. ESB 1805 (x2) received @ 022/05:34:38. ESB 486 "a05" (Exceeded SRL) was received @ 022/05:41:38. Transitioned to M2G as a result of GSAcq failure. OBAD 1: V1 -150.97, V2 -2124.95, V3 -306.91, RSS 2152.30 OBAD 2: V1 1.82, V2 -9.78, V3 21.83, RSS 23.99 10098 - REAcq (2,1,2) Failed @ 023/0618z At 023/06:20:19 Transitioned to M2G, @ 023/06:26:43 transitioned to T2G. Contacted PCS/SE who advised to perform Real-Time OBAD. OBAD performed @ 023/06:56:26 and showed errors of: V1 -10.83, V2 -779.38, V3 -8.93, RSS 779.50 COMPLETED OPS REQUEST: 17620-0 - Temporary Elevation of VTFE While in Taper Charge @ 020/1507z 17633-0 - Modify ROC TC Elapse Timer Limit for Taper Charge @ 020/1825z 17631-2 - VTFE Adjustment During Taper Charge (Options 3) @ 020/2303z 17634-0 - Real-Time OBAD @ 023/0656z COMPLETED OPS NOTES: (None) SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 23 21 020/1441z (HSTAR 10092) 022/0536z (HSTAR 10094) FGS REacq 19 18 023/0618z (HSTAR 10098) OBAD with Maneuver 71 71 SIGNIFICANT EVENTS: Taper Charge 2-Orbit High VT Flash Report: On DOY 2006/020 at 15:06 GMT, the 2-Orbit High VT was successfully executed via Ops Request 17620. A pressure based SOC increase of ~12 AH and battery temperature increase of +3 degC (battery 5 experienced the warmest temperature at 2.83 degC. ) were observed. The system reached charge cut-off each orbit and the EPS FSW performed nominally during the 2 orbits at the higher VTFE. In addition, Ops Request 17633 was successfully executed at 18:24 GMT to modify the ROC Safing Test Trickle Charge Elapse Timer Limit from 22392 seconds to 25800 seconds. The VTFE was set back to K1L4-100mv as planned at 2006/20 23:02 following the 2-orbit high VT boost. The system was monitored for one orbit and nominal performance was observed with the benchmark reset threshold satisfied and the maximum system SOC equal to 246Ah. |
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