#1
|
|||
|
|||
Daily Report #4151
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 4151 PERIOD COVERED: UT July 7,8,9, 2006 (DOY 188,189,190) OBSERVATIONS SCHEDULED NIC1/NIC2/NIC3 8794 NICMOS Post-SAA calibration - CR Persistence Part 5 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. ACS/WFC/HRC 11005 Funcional test - MEB2 switch This is a functional test to be executed after the switch to MEB2. NIC2 10906 The Fundamental Plane of Massive Gas-Rich Mergers: II. The QUEST QSOs We propose deep NICMOS H-band imaging of a carefully selected sample of 23 local QSOs. This program is the last critical element of a comprehensive investigation of the most luminous mergers in the nearby universe, the ultraluminous infrared galaxies {ULIRGs} and the quasars. This effort is called QUEST: Quasar / ULIRG Evolutionary STudy. The high-resolution HST images of the QUEST QSOs will complement an identical set of images on the ULIRG sample obtained during Cycle 12, an extensive set of ground-based data that include long-slit NIR spectra from a Large VLT Program, and a large set of mid-infrared spectra from a Cycle 1 medium-size program with Spitzer. This unique dataset will allow us to derive with unprecedented precision structual, kinematic, and activity parameters for a large unbiased sample of objects spanning the entire ULIRG/QSO luminosity function. These data will refine the fundamental plane of massive gas-rich mergers and enable us to answer the following quesitons: {1} Do ultraluminous mergers form elliptical galaxies, and in particular, giant ellipticals? {2} Do ULIRGs evolve into optical bright QSOs? The results from this detailed study of massive mergers in the local universe will be relevant to understanding the basic physical processes involved in creating massive early-type host on the one hand, and growing/feeding embedded massive black holes on the other, in major galaxy mergers. This is an important question since 50% of cosmic star formation at high-z and most of the big BHs appear to be formed in this process. NIC1 10879 A search for planetary-mass companions to the nearest L dwarfs - completing the survey We propose to extend the most sensitive survey yet undertaken for very low-mass companions to ultracool dwarfs. We will use NICMOS to complete imaging of an all-sky sample of 87 L dwarfs in 80 systems within 20 parsecs of the Sun. The combination of infrared imaging and proximity allows us to search for companions with mass ratios q0.25 at separations exceeding ~3 AU, while probing companions with q0.5 at ~1.5 AU separation. This resolution is crucial, since no ultracool binaries are known in the field with separations exceeding 15 AU. Fifty L dwarfs from the 20-parsec sample have high- resolution imaging, primarily through our Cycle 13 HST proposal which identified six new binaries, including an L/T system. Here, we propose to target the remaining 30 dwarfs ACS/WFC 10824 Measuring the Shape and Orientation of the Galactic Dark-Matter Halo using Hypervelocity Stars We propose to obtain high-resolution images of five hypervelocity stars in the Galactic halo in order to establish the first-epoch astrometric frame for them, as a part of a long-term program to measure precise proper motions. The origin of these recently discovered stars, all with positive radial velocities above 540 km/s, is consistent only with being ejected from the deep potential well of the massive black hole at the Galactic center. The deviations of their space motions from purely radial trajectories probe the departures from spherical symmetry of the Galactic potential, mainly due to the triaxiality of the dark-matter halo. Reconstructing the full three-dimensional space motion of the hypervelocity stars, through astrometric proper motions, provides a unique opportunity to measure the shape and orientation of the dark halo. The hypervelocity stars allow measurement of the potential up to 75 kpc from the center, independently of and at larger distances than are afforded by tidal streams of satellite galaxies such as the Sagittarius dSph galaxy. HVS3 may be associated with the LMC, rather then the Galactic center, and would therefore present a case for a supermassive black hole at the center of the LMC. We request one orbit with ACS/WFC for each of the five hypervelocity stars to establish their current positions relative to background galaxies. We will request a repeated observation of these stars in Cycle 17, which will conclusively measure the astrometric proper motions. ACS/WFC 10775 An ACS Survey of Galactic Globular Clusters We propose to conduct an ACS/WFC imaging survey of Galactic globular clusters. We will construct the most extensive and deepest set of photometry and astrometry to-date for these systems reaching a main sequence mass of ~0.2 solar mass with S/N = 10. We will combine these data with archival WFPC2 and STIS images to determine proper motions for the stars in our fields. The resultant cleaned cluster CMDs will allow us to study a variety of scientific questions. These include [but are not limited to] 1} the determination of cluster ages and distances 2} the construction of main sequence mass functions and the issue of mass segregation 3} the internal motions and dynamical evolution of globular clusters, and 4} absolute cluster motions, orbits, and the Milky Way gravitational potential. We anticipate that the unique resource provided by the proposed treasury archive will play a central role in the field of globular cluster studies for decades, with a stature comparable to that of the Hubble Deep Field for high redshift studies. ACS/WFC 10760 Black Hole X-ray Novae in M31 We have been carring out a Chandra {GO+GTO} and HST {GO} program to find Black Hole X-ray Nova {BHXN} and their optical counterparts in M31 for several years. To date we have found 2 dozen BHXN and 3 HST optical counterparts for these BHXN. Our results suggest a rather high ratio of BH to neutron star {NS} binaries, or a high duty cycle for the BHXN. We propose to continue this program, with the goal of determining the orbital period distribution and duty cycles of these BHXN. Current results yield 3 orbital periods and 2 upper limits. Our proposed observations will ~double the total number of periods and therefore yield sufficient numbers to make a first approximation of the orbital period distribution. The orbital period distribution is the fundamental observable parameter any binary stellar evolution models must match, and the duty cycle is very poorly known but directly influences the binary lifetime. M31 is the only galaxy in which this extra-galactic study of BHXN is feasible. ACS/HRC/WFC 10758 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 May, 31 2006- Oct, 1- 2006. The first half of the program has a different proposal number: 10729. ACS/WFC 10753 An Astrometric Calibration Field Near the Ecliptic Pole This program will obtain deep ACS astrometry of a Large Magellanic Cloud star field lying within the planned continuous viewing zone of the James Webb Space Telescope, which extends to a 5 degree radius from the Ecliptic pole. To allow a full astrometric solution to be calculated, controlling for distortions within ACS that may be time variable over periods of months to years, we will observe our target field at two distinct roll angles separated by approximately 90 degrees. To help control for large scale distortions, we will "chop" the observations in at least one roll angle, using offsets of order one third the ACS field of view. ACS/WFC 10742 Ramp Filter and Grism Zeroth Order Wavelengths A calibration of ramp filters on the ACS is obtained through crossing the ramp filters with the G800L grism in observations of the standard star GD 153. The standard star is also observed through the F606W filter and each ramp crossed with a wide-band filter to measure any filter-wedge offset from the standard grism calibration produced by crossing a ramp with the grism. The ramp filters chosen for this first calibration are those which have been used most extensively by observers during the past ACS cycles and can be usefully crossed with the G800L grism. ACS/HRC/WFC 10737 CCD Stability Monitor This program will verify that the low frequency flat fielding, the photometry, and the geometric distortion are stable in time and across the field of view of the CCD detectors. A moderately crowded stellar field in the cluster 47 Tuc is observed every three months with the HRC {at the cluster core} and WFC {6' West of the cluster core} using the full suite of broad and narrow band imaging filters. The positions and magnitudes of objects will be used to monitor local and large scale variations in the plate scale and the sensitivity of the detectors and to derive an independent measure of the detector CTE. An additional orbit is required to compare WFC observations taken at gain 1 with those taken at the new default gain 2. ACS/WFC 10730 External CTE Monitor Monitor CTE in Cycle 14 for WFC and HRC ACS/WFC 10630 The Fine Structure of Elliptical Galaxies in Voids Elliptical galaxies constitute a remarkably homogeneous class of objects with a tight color- magnitude relation and a well-defined Fundamental Plane. In spite of their bland and symmetrical morphology, they are characterized by a wealth of structural features {such as nuclear disks, dust lanes, shells, blue cores, etc.} which contain important clues to their formation history. Little is known about how and if these sub-structures vary as a function of environment; in fact, due to the morphology density relation, our knowledge of ellipticals is strongly biased towards overdense regions such as clusters. But what of the fine structure of ellipticals in voids? According to theoretical predictions, void galaxies should have different merger histories than those in clusters, which may imply that their fine structure also differs. We address these issues using the exquisite angular resolution of HST/ACS to resolve sub-structures in the most accurately classified sample, to date, of truly isolated ellipticals, identified using the 2dFGRS. ACS/WFC 10629 Are Field OB Stars Alone? This SNAP program offers an inexpensive, simple program to search for low-mass companions of field OB stars. Do field OB stars exist in true isolation, as suggested by a recent Galactic study, or are they the tip of the iceberg on a small cluster of low-mass stars as predicted by the cluster mass function and stellar IMF? Short ACS/WFC V and I observations proposed here may easily resolve this issue for field OB stars in the Small Magellanic Cloud. Truly isolated OB stars represent a theoretical challenge and variation from clusters, in mode of star formation, and have important consequences for our understanding of the field stellar population in galaxies. Small clusters around the field OB stars, on the other hand, may confirm the universality of the stellar clustering law and IMF. ACS/WFC 10567 Securing the Faint-End Galaxy Luminosity Function with Surface Brightness Fluctuation Distances The history of the formation of galaxies must leave an imprint in the properties of the mass function of collapsed objects and in it's observational manifestation the luminosity function. At present the faint end of the luminosity function of galaxies is poorly known. Accurate knowledge of the luminosity function over the full range of galaxy clustering scales would provide serious constraints on both initial cosmological conditions and modulating astrophysical processes. Wide field imaging surveys with large groundbased telescopes now provide the capability to identify dwarf galaxy candidates to very faint levels. However distances to these candidates are needed to overcome the omnipresent problem of group membership uncertainties and to establish the intrinsic properties of the faint end of the luminosity function. Single orbit observations with HST ACS can provide adequate distances via the surface brightness fluctuation method for targets in this program, resulting in the best definition ever of the luminosity function to M_R=-11 in a specific environment. ACS/HRC 10542 Charting the Sparkling Star Formation in NGC346 New, stunning V, I images of the youngest and most massive star forming region NGC 346, in the Small Magellanic Cloud, have been recently obtained with the HST/ACS. They reveal a myriad of small compact clusters: some are still embedded in dust, possibly connected by gas and dust filaments. We also discover a rich population of pre-main sequence low mass stars {~3 -0.6 Mo} mainly distributed in the body of NGC 346 and in these compact clusters, which formed with the central cluster {~5My ago}, but have not reached the main sequence yet. The immediate question that emerges is: how did star formation occur in this region? Is there evidence for an age spread among these clusters, that could be indicative of sequential star formation? We are, therefore, requesting an immediate follow up investigation with the ACS/HRC to perform a comprehensive UV/U study of the ten largest clusters identified in the NGC 346 region, with the objective of determining, in combination with the already available deep V, I data, their mass function, their upper mass cut-off, whether mass segregation is present, whether there are age variations, and what is the impact of the stellar feedback, with the final aim to establish how star formation has occured and progressed in this low metallicity environment. NIC2/ACS/WFC/WFPC 10532 2 Kinematics and morphology of the most massive field disk galaxies at z1 We propose to obtain 1 orbit NIC-2 images of a sample of the 15 most massive galaxies found at $1 z 1.3$. These were culled from over 20, 000 Keck spectra collected as part of DEEP and are unique among high redshift massive galaxy samples in being kinematically selected. We intend to test whether these potentially very young galaxies are likely precursors to massive local disks, assuming no further merging. NIC-2 images provide rest-frame optical morphologies that will show whether they are normal disky systems or instead more disturbed looking objects with multiple subcomponents, mergers, peculiar structure, etc. NIC-2 provides near-IR resolutions sufficient to enable measurements of bulges and disks subcomponents. The near-IR will fill a critical gap in the broad-band SED photometry of the galaxy and its subcomponents to estimate mean stellar ages and stellar masses and to assess whether old stellar bulges and disks are in place at that time. Finally, this sample will yield the first statistically significant results on the $z 1$ evolution of the Tully-Fisher relation for massive galaxies. In addition, we propose parallel observations with ACS WFC {V and I bands} and WFPC2 {I-band}. These will target up to 700 galaxies at redshifts 0.7 ... 1.2 for which the DEEP2 survey has obtained precision redshifts and high-resolution kinematic data. The added HST morphology and color information will allow a variety of detailed studies on dynamical, structural, and photometric evolution of galaxies. ACS/HRC 10516 Host Galaxies of Reverberation-Mapped AGNs We propose to obtain unsaturated ACS high-resolution images of four reverberation- mapped active galactic nuclei in order to remove the point-like nuclear light from each image, thus yielding a "nucleus-free" image of the host galaxy. This will allow investigation of host galaxy properties: our particular interest is determination of the host-galaxy starlight contribution to the reverberation-mapping observations. This is necessary {1} for accurate determination of the relationship between the AGN nuclear continuum flux and the size of the broad Balmer-line emitting regions of AGNs, which is important because this relationship is used in estimating black hole masses for large samples of QSOs, and {2} for accurate determination of the bolometric luminosity of the AGN proper. In a Cycle 12 SNAP program, we obtained images of 14 of the 36 reverberation-mapped AGNs for this purpose. This additional request is to complete this program through observations of the four important remaining sources. NIC3/ACS/WFC 10504 Characterizing the Sources Responsible for Cosmic Reionization Our group has demonstrated the role that massive clusters, acting as powerful cosmic lenses, can play in constraining the abundance and properties of low-luminosity star- forming sources beyond z~6; such sources are thought to be responsible for ending cosmic reionization. The large magnification possible in the critical regions of well- constrained clusters brings sources into view that lie at or beyond the limits of conventional exposures such as the UDF, as well as those in imaging surveys being undertaken with IRAC onboard Spitzer. We have shown that the combination of HST and Spitzer is particularly effective in delivering the physical properties of these distant sources, constraining their mass, age and past star formation history. Indirectly, we therefore gain a valuable glimpse to yet earlier epochs. Recognizing the result {and limitations} of the UDF exposure, we propose a systematic search through 6 lensing clusters with ACS and NICMOS for further z~6-7 sources in conjunction with existing deep IRAC data. Our survey will mitigate cosmic variance and extend the search both to lower luminosities and, by virtue of the NICMOS/IRAC combination, to higher redshift. The goal is to count and characterize representative sources at z~6-10 and to delineate the redshift range of activity for the planning of future observations. 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: #10346 REacq(2,1,2 ) failed due to search radius limit exceeded @ 188/1219z The REacq(2,1,2)scheduled at 188/12:15:09 failed at 12:19:58 due to search radius limit exceeded on FGS 2. OBAD2 at 12:10:03 showed errors of V1=68.13, V2=37.63, V3=57.97, RSS=97.05. ESD a05 (FGS Coarse Track failed - Search Radius Limit exceeded) was received. Observations affected : ACS 19, ACS 20, NIC 43 #10347 OBAD Failed Identification (ESB 1902) @ 188/2320z At 188/23:20:04 OBAD1 using FHST-1 and FHST-2 failed. One 486 ESB message 1902 (OBAD Failed Identification) was received. OBAD1 had (RSS) value of 130325.87 arcseconds. OBAD success flag (mnemonic GCHACL09) returned to the "no success" state(a value of 1). OBAD2 at 188/23:30:39 was successful with (RSS) value of 28540.30 arcseconds. #10348 REacq(1,3,3) Failed to RGA Control @ 188/2334z The REacq(1,3,3) scheduled at 188/23:34:59 - 23:43:04 failed to RGA Hold due to uncorrected attitude error per Ref HSTAR# 10347. There were no FGSs indication flags. Prior GSacq using same star id was successful. Possible Observations affected: ACS 38 thru 41. #10349 GSAcq (2,1,2) failed due to search radius limit exceeded @ 190/0631z GSAcq (2,1,2) scheduled @ 190/06:28:12-06:35:45 failed due to search radius limit exceeded on FGS 1. Received one 486 ESB message a05 (Exceeded SRL). OBAD #1: V1 -1811.83, V2 1880.49, V3 -2874.30, RSS 3883.37. OBAD #2: V1 -0.53, V2 5.56, V3 7.14, RSS 9.06. At AOS (190/07:39:10) OBAD MAP scheduled @ 07:15:32 showed the following: V1 -55.71, V2 2400.79, V3 -29.66, RSS 2401.62. REAcq 2,1,2 scheduled at 190/08:03:38 failed to RGA hold due to stop flag on FGS-1. Possible observations effected: ACS 101-131. OBAD MAP @ 08:51:27 = V1 -389.08, V2 4988.63, V3 -3.54, RSS 5003.78 COMPLETED OPS REQUEST: #17543-2 Dump OBAD tables after failed OBAD (Generic) @ 188/2326z COMPLETED OPS NOTES: (None) SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 23 22 190/0631z (HSTAR 10349) FGS REacq 30 27 188/1215z (HSTAR 10346) 188/2334z (HSTAR 10348) 190/0803z (HSTAR 10349) OBAD with Maneuver 76 75 188/2320z (HSTAR 10347) SIGNIFICANT EVENTS: (None) |
Thread Tools | |
Display Modes | |
|
|
Similar Threads | ||||
Thread | Thread Starter | Forum | Replies | Last Post |
COMEDY CENTRAL -- Man First Steps on the Moon -- NASA Hoax????? | Ed Conrad | Astronomy Misc | 21 | July 7th 06 03:20 AM |
HOMO IGNORAMUS -- New Fossil Discovered -- It Has a Petrified Brain) | Ed Conrad | Astronomy Misc | 1 | June 14th 06 05:36 AM |
Who Says CROP CIRCLES are Man Made? | Ed Conrad | Astronomy Misc | 0 | May 25th 06 05:35 AM |
Even More on BILLY MEIER & EXTRATERRESTRIALS -- Major Media Conspiracy Against Truth ----- Just like 911 Govt Hoax & Man as Old as Coal ----- | Ed Conrad | Amateur Astronomy | 1 | May 11th 06 07:02 PM |