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DAILY REPORT #3898
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT #3898 PERIOD COVERED: UT July 08-10, 2005 (DOY 189-191) OBSERVATIONS SCHEDULED NIC1/NIC2/NIC3 8793 NICMOS Post-SAA calibration - CR Persistence Part 4 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. FGS 10614 Internal Structure and Figures of Binary Asteroids The goal of this proposal is to obtain very important information on the internal structure of a number of asteroids, and insight on the gravitational reaccumulation-process after a catastrophic disruptive collision. High resolutions observations with the HST/FGS interferometer are proposed to obtain high precision data for the topographic shape and size of a number of selected asteroids. Here we focus on objects with satellites, hence with known masses, so that the bulk density and porosity will be derived in the most accurate manner. This will yield plausible estimates on the internal properties of the objects, test wether they are close or not to figures of equilibrium {in terms of shape and adimensional rotational frequency}, and provide estimates of their relative density. The HST/FGS in interferometric mode is an ideal facility to carry out this program. ACS/HRC 10435 Merger-Induced Populations in Early-Type Galaxy Cores Hierarchical formation models predict that early-type galaxies are built up over an extended period from mergers of smaller systems, a process which should leave long- lived signatures in their light profiles and stellar population colors. Merger events should have continued up to relatively recent times {the last 1-5 Gyr}, and many ellipticals and S0 bulges should therefore show evidence of multiple, discrete, intermediate-age populations. Although there is substantial observational support for a dissipational merger origin for some early-type galaxies, most do not exhibit the expected anomalies in either their light profiles or color distributions. However, existing searches {mainly in the V and I bands} have not probed very deeply. Here we propose high resolution, broad-band, near-ultraviolet {2500-3400 A} imaging of the cores of bright early-type galaxies. This is the most sensitive probe available for the detection of spatially-segregated, multiple population components with ages in the range 1-5 Gyr. Our sample consists of dust- and AGN-free systems with both normal and mildly anomalous central light profiles. There is very little existing information on the near-UV structure of early-type galaxies, and our program would effectively explore new terrain. NIC1/NIC2 10410 Anisotropy and obscuration in the near-nuclear regions of powerful radio galaxies Despite the success of the orientation-based unified schemes for powerful radio sources, we are still far from understanding the distribution of obscuring material in the near-nuclear regions of such sources, and how this distribution evolves with radio power. Following on from our highly successful Cycle 7 pilot observations of Cygnus A, we propose a near-IR polarimetric survey of a complete sample of powerful radio galaxies in order map the near-nuclear illumination cones, and investigate the distribution of obscuring material on a 0.1 to 1kpc scale. In particular, the observations will allow us to test the "receding torus model'' which predicts that the opening angles of the illumination cones are smaller in low redshift/low power radio galaxies than in their high redshift/high power counterparts.We will also investigate whether AGN- and jet-driven outflows have a substantial effect on distribution of obscuring material by "hollowing out'' the quasar illumination cones in the more powerful sources. Finally, by using our polarization maps to search for signs of intrinsic anisotropy in the near-IR continuum within the cones, we will investigate the geometry of the near-IR continuum emitting regions close to the quasar nuclei. These observations are not only crucial for our understanding of radio source unification, but also provide key information about the effects of AGN-induced outflows on the ISM of the host galaxies. ACS/HRC/WFC/NIC2 10399 Accurate and Robust Calibration of the Extragalactic Distance Scale with the Maser Galaxy NGC4258 II The extragalactic distance scale {EDS} is defined by a comparison of Cepheid Period- Luminosity {PL} relations for nearby galaxies and the LMC, whose uncertain distance is thereby the SOLE anchor. Studies of masers orbiting the central black hole in NGC4258 have provided the most accurate extragalactic distance ever {7.2+/-0.5 Mpc}, and new radio data and analysis techniques will reduce the uncertainty to 3.5% {0.07 mag} by 2005. Since this distance is well determined and based on geometric arguments, NGC4258 can provide a much needed new anchor for the EDS. Ultimately, the combination of an independent measurement of H0 and measurements of CMB fluctuations {e.g., WMAP} can be used to directly constrain cosmological parameters including the equation of state of dark energy. In our Cycle 12 proposal, we defined a program spanning two cycles. The Cycle 12 portion was accepted. We have acquired WFC images and are constructing well sampled PL relations in 3 colors {BVI}. The purpose of the Cycle 13 observations is to address systematic sources of error and is crucial for the success of the entire program. To disentangle the effects of reddening and metallicity, and to characterize the effects of blending, we require 50 orbits to obtain H-band photometry {NICMOS/NIC2} and high resolution images {ACS/HRC}. ACS/WFC/WFPC2/NIC 10395 3 Environmental drivers of galaxy evolution: an HST survey of dwarf galaxy morphologies in the Abell Galaxies in dense environments are subject to numerous physical processes that leave a lasting impact, yet studies of galaxy evolution to date have been limited to the most luminous galaxies -- those least sensitive to environmental influence. We propose to explore the environmental drivers of DWARF galaxy evolution: with a mosaic of 9x9 ACS pointings in F606W we will determine morphologies for ~1200 galaxies down to M_V=-14 in the A901/902 supercluster, spanning 3x3 Mpc at z=0.16. The deep ACS data will allow us to probe their surface brightness profiles, shapes, sizes, asymmetry and fine structure such as tidal features. With the addition of extensive existing multi- wavelength data, we will probe the dependence of these important parameters on dark matter content {from weak lensing maps}, the hot intercluster medium {from deep XMM- Newton imaging}, and local galaxy density {from hyper-accurate COMBO-17 photometric redshifts with delta z=0.02 to m_R=24}, thus disentangling the various environmental processes shaping dwarf galaxy evolution. Furthermore, the 8000+ background galaxies at 0.2z1.0 will be of enormous scientific benefit for additional studies of weak lensing, AGN host galaxies, the morphology-density relation, and the merger rate as a function of redshift. ACS/WFC/WFPC2 10394 Deep imaging of newly discovered globular clusters in the outer halo of M31 Globular clusters {GCs} are fossil relics with which we can investigate the processes of galaxy formation and growth. We have recently discovered a sample of GCs, as part of a very wide area CCD survey of M31. These clusters span a range in projected galactocentric distance of 20 - 80 kpc, more than double the radii of the previous most remote known GC. Here we apply for deep ACS images of 13 GCs, which will allow us to study their stellar populations, line-of-sight distances and structural parameters. These will be used to: a} Investigate the merger history of M31, through an examination of variations in the RGB and HB morphologies, particularly to obtain metallicities and check for the presence of any second parameter effect in the HB. d} Determine, in conjuction with ground-based spectroscopy, the dynamical mass of M31 at large radius, providing a direct probe of the mass distribution of its dark halo. ACS/HRC/WFC 10389 ACS CCDs daily monitor - Cycle 13 - Part 2 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 program will be for the entire lifetime of ACS. NIC1/NIC2/NIC3 10381 Photometric Stability This NICMOS calibration proposal carries out photometric monitoring observations during Cycle 13. The format of the program is identical to that of the Cycle 12 program 9995 ACS/WFC/HRC 10378 ACS Polarimetry Calibration Observations are made of the Boomerang Nebula {highly polarized reflection nebula} to calibrate the ACS polarizers. ACS/HRC 10377 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 coronagraphic monitoring is required to assess the changing position of the spots. ACS/HRC/NIC2 10244 Coronagraphic imaging of Eta Corvus: a newly discovered debris disk at 18 pc Debris disks are one of the final stages in the evolution of planetary systems. High resolution imaging of debris disks has been instrumental to our understanding of the status of planet formation in these systems. The detection of clumps and asymmetries has even led to the detection of unseen planets. However, just six resolved disks exist in the literature. Eta Crv is now the seventh debris disk confirmed with imaging, and was discovered in a recent sub-mm survey of nearby stars. Its proximity {18 pc} and similarity to Beta Pic, one of the "big four" Vega-type disks, makes it an excellent candidate for a high resolution coronagraphic study of its disk structure. Modeling of this structure at many wavelengths will set hard constraints on its unseen planetary system and the distribution of particles from micron to kilometer in size, thus significantly extending our understanding of the planet formation processes in debris disks ACS/WFC 10154 Morphology of z ~ 7-10 galaxies viewed through gravitational telescopes The aim of these observations is to obtain deep z/ACS and H/NICMOS images in the core of two lensing clusters, A1835 and AC114, where a few z ~ 7-10 galaxy candidates have been selected from our ultra-deep JHK imaging program with Isaac/VLT. Spectroscopic observations have allowed to confirm 2 of these candidates thanks to the detection of faint emission lines identified as Lyman alpha at z=7.2 and 10. Our HST project is focused on two main goals: {1} the morphological confirmation of galaxy candidates lying near critical lines, and {2} the determination of the physical scales involved in star-forming regions at z ~ 7-10. These goals should have important implications on our present knowledge of the galaxy formation process in the early Universe. ACS/WFC 10101 The Region of the Hydrogen-Burning Limit in Omega Centauri and 47 Tucanae We propose a photometric study of the lower main sequences of Omega Cen and 47 Tuc, down to the region of the H-burning limit, which the deeper faintness limit of ACS will allow us to reach. For the faintest stars, proper-motion separation of cluster from field is essential; hence we include Cycle 13 observations. The resulting color-- magnitude diagrams {CMDs} and luminosity functions {LFs} will allow study of stars in a mass regime and metallicity that have never been accessible before, and will serve as an important check on theories of the structure of low-mass stars. These are the 2nd- epoch observations. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) HSTARS: #9880 - SAVED FGS ERROR NULL BIAS (QSFGENB0) @ 189/1919z During successful GSacq(1,2,1) of 189/19:14:25, a measuremnet was made of the V1 (roll) error during sequential update. This measured value of the error -1073.130 a-s "Err Null Bias (QSFGENB0)" was saved in the telemetry parameter "Saved FGS Error Null Bias (QSFGENB0)" at 189/19:19:08. #9881 - GSacq(1,3,1) results in finelock backup (1,0,1) scan step lmt exc on FGS-3 @ 189/2054z The GSacq(1,3,1) scheduled at 189/20:50:22 - 20:58:24 Z resulted in finelock backup (1,0,1) using FGS-1, due to scan step limit exceeded on FGS-3 during acquisition walkdown. The Secondary FGS has the same star id (0547900910) as HSTAR 9871. #9882 - GSacq(1,2,1) results in finelock backup (1,0,1) scan step lmt exc on FGS-2 @ 189/2230z The GSacq(1,2,1) scheduled at 189/22:26:15 - 22:34:17 Z resulted in finelock backup (1,0,1) using FGS-1, due to scan step limit exceeded on FGS-2 duirng acquisition walkdown. The Secondary FGS has the same star id (0547900910) as HSTAR 9871. #9883 - GSAcq (2,1,1) Failed to RGA Control, due to search radius limit exceeded on FGS-1 @ 190/1016z The GSACQ(2,1,1) scheduled at 190/10:11:10 - 190/10:18:32 Failed to RGA Control due to search radius limit exceeded on both FGS1 and FGS2. #9886 - GSACQ(1,2,1) fine lock backup, scan step limit exceeded on FGS-1 @ 190/1917z GSACQ(1,2,1) at 190/19:13:24 ended in fine lock backup on FGS 2 due to scan step limit exceeded twice on FGS 1 at 19:17:20 and 19:19:01. #9887 - GSACQ(1,2,1) fine lock backup (2,0,2), scan step limit exceeded on FGS 1 @ 190/2225z GSACQ(1,2,1)@190/22:25:57 resulted in fine lock backup(2,0,2)on FGS 2 due to scan step limit exceeded twice on FGS 1 at 22:29:10 and 22:30:52. COMPLETED OPS REQUEST: #17464-0 - Genslew for proposal 10330 - slot 8 @ 189/1725z #17465-0 - Genslew for proposal 10330 - slot 11 @ 189/1727z #17466-1 - Real Time Map @ 190/1342z #17467-1 - ARU/PRT @ 190/1424z #17468-0 - Real Time Map @ 190/1523z COMPLETED OPS NOTES: (None) SCHEDULED SUCCESSFUL FGS Gsacq 25 24 FGS Reacq 19 16 FHST Update 36 36 SIGNIFICANT EVENTS: (None) |
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