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Daily 3632
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3632 PERIOD COVERED: DOYs 163-165 OBSERVATIONS SCHEDULED NIC1/NIC2/NIC3 9993 Cycle 12 NICMOS dark current, shading profile, and read noise monitoring program The purpose of this proposal is to monitor the dark current, read noise, and shading profile for all three NICMOS detectors throughout the duration of Cycle 12. This proposal is an essentially unchanged continuation of PID 9636 which cover the duration of Cycle 11. ACS/WFC 9902 The Evolution of the Host Galaxies of Radio-Quiet Quasars Study of the host galaxies and environments of high redshift AGN is proving a valuable probe of current theories of how galaxies form and evolve. Results from our NICMOS imaging program have indicated that the hosts of z ~ 2 -- 3 faint radio-quiet quasars {RQQ} have luminosities only around local L*, making them similar to Lyman-break field galaxies at the same redshifts, and to the low-z hosts RQQ hosts. This is roughly consistent with theoretical predictions of Kauffmann & Haehnelt {2000} for the hierarchical buildup of galaxy hosts and their relation to their resident supermassive black holes. The luminosity of the AGN in these RQQ is key to understanding this relationship, however, and we are making a comprehensive archival HST imaging study of the hosts of RQQs from low to high z at a range of nuclear luminosities. At intermediate z, however, there are no studies of the hosts of RQQs in the faint luminosity range that represents the bulk of the quasar population. In the present proposal, we request imaging at the same rest-wavelengths as our high-z sample of the hosts of 10 similarly luminous RQQs at z ~ 0.9. These data will fill in an important part of the parameter space defined by quasar luminosity and redshift. Combined with existing HST data they will allow us to trace the evolution of the hosts of RQQ and that of the relationship between quasar luminosity and host galaxy luminosity. STIS/CCD/MA1 9893 The field structure of the most strongly magnetized white dwarf PG1031+234 With a maximum field strength of 1 GG PG1031+234 has the strongest magnetic field found in any white dwarf. Since magnetic fields generated on earth are limited to a few MG, this star is an important cosmic laboratory to test the atomic data calculated for field strengths which are similar to those in recycled millisecond pulsars. Our aim is to take phase resolved FUV spectra covering the rotational {spin} period of 204 minutes. The variation of the position and shape of the Lyman alpha components is very important for a detailed mapping of magnetic field topology, which is believed - according to an analysis of the optical data - to consist of a general dipole field with a polar field strength of 500 MG and a magnetic spot with a field reaching 1 GG. Moreover, we will search for the forbidden 1s0 - 2s0 transition of hydrogen which would indicate the additional presence of an electric field, and, for quasi-molecular features of hydrogen which would provide constraints on the detailed temperature structure of the atmosphere. It is also important to redetermine the effective temperature with time resolved UV data, since an inconsistency between the analysis of IUE spectrum {Teff aprox. 25000 K}, integrated over one full rotational period, and the optical spectrum {15000 K} exists which is also reflected in a large uncertainty of the mass determination. 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. NIC/NIC3 9865 The NICMOS Parallel Observing Program We propose to continue managing the NICMOS pure parallel program. Based on our experience, we are well prepared to make optimal use of the parallel opportunities. The improved sensitivity and efficiency of our observations will substantially increase the number of line-emitting galaxies detected. As our previous work has demonstrated, the most frequently detected line is Halpha at 0.7z1.9, which provides an excellent measure of current star formation rate. We will also detect star-forming and active galaxies in other redshift ranges using other emission lines. The grism observations will produce by far the best available Halpha luminosity functions over the crucial--but poorly observed--redshift range where galaxies appear to have assembled most of their stellar mass. This key process of galaxy evolution needs to be studied with IR data; we found that observations at shorter wavelengths appear to have missed a large fraction of the star-formation in galaxies, due to dust reddening. We will also obtain deep F110W and F160W images, to examine the space densities and morphologies of faint red galaxies. In addition to carrying out the public parallels, we will make the fully reduced and calibrated images and spectra available on-line, with some ground-based data for the deepest parallel fields included. NIC2 9856 A near-IR imaging survey of submm galaxies with spectroscopic redshifts Submillimeter {submm} surveys with SCUBA have identified a population of obscured star-forming and active galaxies at high redshift. Our recent spectroscopic campaigns with the Keck-10m telescope have uncovered redshifts for 37 SCUBA galaxies. The wide redshift range of the radio identified submm population {z=1-4} implies that many varieties of sources driven by different physical processes may be selected in a submm survey. We propose to use HST-NICMOS, ACS to obtain 2-filter images of a sample of 15 SCUBA galaxies with redshifts spanning z=0.8-3.5. Our goal is to understand what physical process {major mergers?} drive their strong evolution and great luminosities, and what the implications are for galaxy evolution models. STIS/CCD 9854 Anomalous Flux Ratios in Quadruple Gravitationally Lensed QSOs We propose to observe eight {8} gravitationally lensed systems which exhibit quadruple images of the background high redshift quasars. Models invoking a smooth potential fit the observed image positions accurately, in most cases better than 5 milliarcseconds. But the same models dramatically fail to predict the observed flux ratios. These anomalous flux ratios can be attributed to micro- or milli-lensing in the massive lensing halo. In this proposal, we will isolate the source of the anomalous flux ratios by using the superior resolution of HST/STIS to obtain spectrophotometric data and compare the emission line flux ratio of the QSOs to the continuum flux ratios. Due to the much larger size of the broad emission line regions, the flux ratios in the emission lines should only be affected by milli-lensing if the sub-halos are comparable or larger in projected size than the source region. That is, flux ratios observed in the QSO continuum are sensitive to substructure on all scales {both micro- and milli-lensing}, while the broad emission lines are insensitive to micro-lensing due to the larger physical size of the source emission region. This sample of eight quasars will provide the definitive evidence to distinguish between possible sources causing the observed anomalous flux ratios. 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/HRC/WFC 9781 Galaxy Evolution in Action : The Detailed Morphology of Post-Starburst Galaxy If galaxies evolve morphologically, then some should be in transition between late and early types. One proposed evolutionary mechanism is a galaxy-galaxy merger, but evolved merger products are difficult to find. Fortunately, spectroscopic surveys have now uncovered large numbers of E+A galaxies, a class of objects whose post-starburst spectra, current lack of HI gas, and pressure-supported kinematics suggest that they are the missing panel that connects the "Toomre sequence" of merging spirals with normal ellipticals and S0s. Our first HST observations of five of these galaxies are intriguing. We find a considerable range of tidally disturbed morphologies, an "E+A" fundamental plane, significant differences among the color gradients within 1 kpc {~0.8''}, and populations of bright, blue globular clusters. These initial results are difficult to interpret, however, because they are drawn from a small sample of galaxies whose very blue overall colors may have selected a particular evolutionary path of E+As. Here we propose for ACS imaging of the remaining 15 E+As from the Las Campanas Redshift Survey to probe the full range of E+A properties. The proposed observations will allow us to 1} determine what fraction of the interactions that lead to E+As destroy all disk-like structures {and therefore necessarily lead to elliptical formation}, 2} measure the inner color gradients and constrain the spatial distribution of stars produced as gas sinks to the center during a merger, and 3} determine whether these interactions produce globular clusters in the required numbers to account for the increased specific frequency of clusters in early-type galaxies. ACS/WFC 9779 Giant Lya Halos Around High Redshift Radio Galaxies We propose to use the ACS + ramp filter to image the morphologies of several high redshift, giant Lya emission line halos associated with radio galaxies. High redshift radio galaxies are the likely precursors of the most massive elliptical galaxies known today. There is increasing evidence that they are forming in the centers of giant halos in overdense galaxy regions or `protoclusters'. The halos provide a unique diagnostic to study the formation of these massive galaxies and determine the importance of AGN/starburst feedback during this process. The capability of HST to resolve fine detail is essential for the interpretation of their complex morphologies. Our targets have also a number of Lya excess galaxies near the halos which fall within the field-of-view of the ACS + ramp filters. Our images will resolve these systems and we will investigate whether there is morphological evidence for starburst outflows. Starburst winds have been proposed as a source of heat and chemical enrichment for protoclusters, which may significantly affect their evolution. ACS/WFC/WFPC2 9774 Young Massive Clusters in Spiral Galaxies and the Connection with Open Clusters We propose to carry out a census of star clusters in the disks of the nearby spiral galaxies NGC 45, NGC 1313, NGC 4395, NGC 5236 and NGC 7793. Using ACS, we will identify much fainter and older star clusters than possible in previous ground-based surveys, or even in HST imaging of more distant galaxies. For the first time, we will directly explore the connection between young "massive'' {or "super''} star clusters {YMCs} and lower-mass "open'' clusters in different star forming environments. We will test the universality of the luminosity- and mass functions of stellar clusters and establish whether the presence of YMCs is a result of a top-heavy cluster luminosity function, or follows from generally richer cluster systems. Our target galaxies span a range of morphological properties, surface brightness and star formation rate. Some of them are known from ground-based studies to host large numbers of YMCs while others have more modest cluster populations. However, previous ground-based data were restricted to luminous clusters younger than about 500 Myr. Here we will extend the search to clusters formed throughout the entire lifetime of each galaxy and reach clusters with properties typical of the Milky Way open clusters. This will allow us to close the gap between studies of extragalactic and Galactic disk clusters. STIS/CCD/MA1 9736 Integrated Absorption- and Emission-Line Analysis of Nebulae Serious discrepancies have arisen in CNONe abundance determinations for galactic nebulae in the past ten years depending upon which type of emission lines are used in the analysis: forbidden vs. permitted lines. The cause of the discrepancies, which can exceed an order of magnitude for some PNe, has been studied intensively but is still unknown. Emission line abundances cannot be considered reliable until the nature of these contradictory results is understood. We have developed a technique for integrating absorption lines into emission analyses for diffuse nebulae that provides an independent check on the validity of emission-line analyses. It requires high resolution observations of UV resonance absorption produced by the nebular gas in imbedded or background stars together with optical spectra of the nebulae. We propose to obtain UV spectra of four PNe central stars with STIS that will provide data necessary to exploit the new technique of integrated abundance determination that combines both emission and absorption lines. ACS/HRC/WFC 9728 Tracing the History of Cosmic Expansion to z~2 with Type Ia Supernovae Type Ia supernovae {SNe Ia} provide the only direct evidence for an accelerating universe, an extraordinary result that needs the most rigorous test. The case for cosmic acceleration rests on the observation that SNe Ia at z = 0.5 are about 0.25 mag fainter than they would be in a universe without acceleration. A powerful and straightforward way to assess the reliability of the SN Ia measurement and the conceptual framework of its interpretation is to look for cosmic deceleration at z 1. This would be a clear signature of a mixed dark-matter and dark-energy universe. Systematic errors in the SNe Ia result attributed to grey dust or cosmic evolution of the SN Ia peak luminosity would not show this change of sign. We have obtained a toehold on this putative ``epoch of deceleration'' with SN 1997ff at z = 1.7, and 3 more at z 1 from our Cycle 11 program, all found and followed by HST. However, this is too important a test to rest on just a few objects, anyone of which could be subject to a lensed line-of-sight or misidentification. Here we propose to extend our measurement with observations of twelve SNe Ia in the range 1.0 z 1.5 or 6 such SNe Ia and 1 ultradistant SN Ia at z = 2, that will be discovered as a byproduct from proposed Treasury and DD programs. These objects will provide a much firmer foundation for a conclusion that touches on important questions of fundamental physics. 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. WFPC2 10079 Geometric distortion of F255W for WFPC2 Cycle 12 The goal of astrometric calibration of the HST WFPC2 is to obtain a coordinate system free of distortion down to the precision level of 1 mas. That precision is necessary for future astrometric work {e.g., on proper motions} involving a combination of the archival WFPC2 and recent ACS images. So far such a calibration has only been obtained for the wide bandpass F555W filter {Anderson and King, 2003}. Recently V. Kozhurina-Platais {ISR, 2003-002} has expanded the analysis of the geometric distortion of WFPC2 as a function of wavelength for two other broadband filters, {F814W and F300W}, and has also established the plate scale and skew parameters {non-perpendicularity of X and Y axes} for these filters. This study points to the importance of astrometric calibration at wavelengths shorter than ~400 nanometers. This proposal seeks observations in the FUV filter F255W of the Inner Calibration Field in the globular cluster omega Cen. It is expected that the amount of distortion in the F255W filter with respect to the F555W filter will be higher by 5% but this must be established from observations. A total of four astrometric calibrations in F255W {proposed here}, and F300W, F555, F814W {already completed} will allow us to interpolate such a calibration for any other filter from FUV to near infrared. WFPC2 10071 WFPC2 CYCLE 12 Supplemental Darks Part 3/3 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 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. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) None COMPLETED OPS REQs: None OPS NOTES EXECUTED: None SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 22 22 FGS REacq 20 20 FHST Update 37 37 LOSS of LOCK SIGNIFICANT EVENTS: SMS SA166O01 ends at a non-nominal time of 172/22:00Z to accommodate science visits across the nominal end boundary. |
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