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Daily 3593
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3593 PERIOD COVERED: DOY 106 OBSERVATIONS SCHEDULED 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/WFC 9765 The Dusty ISM Substructure in Nearby Spiral Galaxies We propose an ACS V&I imaging snapshot survey of all nearby edge-on spiral galaxies in order to measure the small scale structures in their dust extinction down to the 10pc scale. Dust and molecular gas are tightly coupled and therefore HST high resolution reddening maps can reveal information about the cold ISM phase on a scale inaccessible from the ground by any other means. We have recently discovered a sudden change in dust lane properties using ground-based data; all galaxies with rotation speeds in access of 120km/s show dust lanes, but none of the slower rotators does. This transition may be caused by a sudden change in the state of the multiphase ISM, and HST resolution imaging is needed to fully quantify this effect. Analysis will consist of full radiative transfer modeling of dust extinction with realistic, fractal like substructure and power spectrum analysis of the structure from the global to the 10pc scale. By observing a sample of galaxies with a range in structural parameters we can quantify how the cold ISM structure changes as function of radius, rotation speed, local surface density, et cetera. This information is duly needed with SIRTF soon providing a wealth of information on dust absorption, but lacking the resolution to determine the small scale distribution of the dust. ACS/WFC/WFPC2 9822 The COSMOS 2-Degree ACS Survey We will undertake a 2 square degree imaging survey {Cosmic Evolution Survey -- COSMOS} with ACS in the I {F814W} band of the VIMOS equatorial field. This wide field survey is essential to understand the interplay between Large Scale Structure {LSS} evolution and the formation of galaxies, dark matter and AGNs and is the one region of parameter space completely unexplored at present by HST. The equatorial field was selected for its accessibility to all ground-based telescopes and low IR background and because it will eventually contain ~100, 000 galaxy spectra from the VLT-VIMOS instrument. The imaging will detect over 2 million objects with I 27 mag {AB, 10 sigma}, over 35, 000 Lyman Break Galaxies {LBGs} and extremely red galaxies out to z ~ 5. COSMOS is the only HST project specifically designed to probe the formation and evolution of structures ranging from galaxies up to Coma-size clusters in the epoch of peak galaxy, AGN, star and cluster formation {z ~0.5 to 3}. The size of the largest structures necessitate the 2 degree field. Our team is committed to the assembly of several public ancillary datasets including the optical spectra, deep XMM and VLA imaging, ground-based optical/IR imaging, UV imaging from GALEX and IR data from SIRTF. Combining the full-spectrum multiwavelength imaging and spectroscopic coverage with ACS sub-kpc resolution, COSMOS will be Hubble's ultimate legacy for understanding the evolution of both the visible and dark universe. 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. FGS 9961 The Masses and Luminosities of Population II Stars Very little is currently known concerning the mass-luminosity relation {MLR} of Population II stars. However, with the advent of the Hipparcos Catalogue, improved distances to many spectroscopic binaries known to be Pop II systems are now available. After surveying the literature and making reasonable estimates of the secondary masses, we find 13 systems whose minimum separation should be larger than the resolution limit of FGS1. Because of the expected magnitude differences and separations, it is not possible to resolve the systems from the ground. We therefore propose FGS observations of the sample. In combination with the known spectroscopic orbits and Hipparcos distances, these observations will yield up to 26 precise stellar mass determinations of metal-poor stars, if all systems are resolved and the relative orbits are determined. A combination of FGS data and ground-based observations will lead to component luminosities and effective temperatures. This program will allow for a significantly better understanding of the Pop II main sequence, which in turn will lead to better ages and distances of the galactic globular clusters, and a Pop II MLR will be constructed for the first time. 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. 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. 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. NIC2 9845 NICMOS Confirmation of a Young Planetary-Mass Companion We have recently discovered a strong candidate for a planetary-mass {~10 Mjup} companion to a young Sun-like star, based on near-IR imaging and spectroscopy with the Keck and Subaru adaptive optics {AO} systems. While the ground-based data strongly suggest that the candidate has a very low effective temperature, and hence a very low mass, they are not definitive. We propose to obtain NICMOS coronagraphy to measure the companion's 1.9um water-band absorption. This feature is a distinct signature of very cool objects and is unobservable from the ground. The combined ground-based and space-based data set will determine whether the companion has a very low temperature, and hence if it is the lowest mass companion found to date by direct imaging. NIC3 9999 The COSMOS 2-Degree ACS Survey NICMOS Parallels The COSMOS 2-Degree ACS Survey NICMOS Parallels. This program is a companion to program 9822. STIS 9783 The Ages of Nuclear Star Clusters in Early-type Spiral Galaxies We propose to obtain STIS G430L spectra of the previously identified nuclear star cluster in a sample of 16 spiral galaxies of early to intermediate Hubble type. HST's spatial resolution is required to separate the nuclear cluster from the underlying galaxy bulge. Analysis of the spectra with population synthesis methods will reveal the cluster ages. We will use the age distribution to constrain the duty cycle of nuclear cluster formation. Comparison of the results to those for a larger sample of nuclear clusters in late-type, bulgeless galaxies will allow us to investigate possible differences between the formation mechanisms of nuclear clusters in early and late Hubble types. Such differences might be expected because galaxy bulges show a dichotomy: in late Hubble types, the surface brightness profiles are best described by an exponential, while they follow a de Vaucouleurs law in earlier types. Although the reason for this dichotomy is still unknown, it is plausible that galaxy bulges have different formation mechanisms at the two ends of the Hubble sequence. We know that {1} nuclear cluster formation is linked to the funneling of gas towards the nucleus via gravitational torques from stellar bars, {2} a nuclear mass concentration can make bars unstable, and {3} unstable bars can form bulges. Therefore, the age distribution of nuclear star clusters contains important clues to the evolution of galaxy centers and promises new insight into the origin of the Hubble sequence. STIS/CCD 10018 CCD Dark Monitor-Part 2 Monitor the darks for the STIS CCD. 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 10024 STIS CCD Imaging Flats C12 Investigate flat-field stability over a bimonthly period. STIS/CCD/MA1 9724 Towards a global understanding of accretion physics - Clues from an UV spectroscopic survey of cataclysmic variables Accretion inflows and outflows are fundamental phenomena in a wide variety of astrophysical environments, such as Young Stellar Objects, galactic binaries, and AGN. Observationally, cataclysmic variables {CVs} are particularly well suited for the study of accretion processes. We are currently carrying out a Cycle 11 STIS UV spectroscopic snapshot survey of CVs to fully exploit the diagnostic potential of these objects for our understanding of accretion physics. While the data obtained so far are of excellent quality, the number of targets that will be observed in Cycle 11 is too small for a statistically significant analysis {only 19 objects out of our 149 accepted Cycle 11 snapshot targets have been observed at the time of writing}. We propose here to extend this survey into Cycle 12, building a homogenous database of accretion disc and wind outflow spectra covering a wide range of mass transfer rates and binary inclinations. We will analyze these spectra with state-of-the-art accretion disc model spectra {SYNDISK}, testing our current knowledge of the accretion disc structure, and, thereby, providing new insight into the so far not well understood process of viscous dissipation. We will use our parameterised wind model PYTHON for the analysis of the radiation driven accretion disc wind spectra, assessing the fundamental question whether the mass loss rate correlates with the disc luminosity. In addition, our survey data will identify a number of systems in which the white dwarf significantly contributes to the UV flux, permitting an analysis of the impact of mass accretion on the evolution of these compact stars. This survey will triple the number of currently available high-quality accretion disc / wind outflow / accreting white dwarf spectra, and we waive our proprietary rights to permit a timely use of this database. STIS/MA1 9790 Separating Activity and Accretion in T Tauri Stars Due to their unique evolutionary state, the naked {non-accreting} T Tauri stars {NTTS} are the only real proxies for what the underlying magnetically active star of a classical TTS {CTTS} system looks like. Comparative analysis then allows us to separate stellar properties from accretion properties in CTTS. In addition, the late-type NTTS are excellent candidates for studying rotation-activity relationships in fully convective stars and probing the properties of turbulent dynamos. With the limited data currently available, NTTS appear to be very magnetically active stars with higher than expected H-alpha/X-ray flux ratios but lower transition region fluxes relative to other active stars. However, the data are very incomplete. We will use HST-STIS observations of transition region line fluxes on 11 fully convective NTTS to establish the level and structure of dynamo generated emission in these young stars. In principal, these far ultraviolet emission lines are sensitive diagnostics of mass accretion onto CTTS, since accretion shocks on the stellar surface should produce substantial emission measure at 10^5 - 10^6 K. However, it is imperative that we first understand the emissions from NTTS before we can use these lines to study accretion onto CTTS. 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. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) None COMPLETED OPS REQs: 17124-0 - FSW 2.5B EEPROM Installation @ 106/1332z 17122-0 - FSW 2.5B On-Orbit Verification (thru step E) @ 106/2126z OPS NOTES EXECUTED: None SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 9 9 FGS REacq 5 5 FHST Update 18 18 LOSS of LOCK SIGNIFICANT EVENTS: Successfully completed installation of FSW 2.5b EEPROM (OR 17124 with attached script) The FSW 2.5b EEPROM load was completed @ 106/12:11:30Z, post-installation EEPROM memory dump was completed @ 106/13:13:40Z and subsequently verified by FSW. FSW 2.5b on-orbit verification continued following the EEPRO installation (OR 17122). PN format was successfully acquired from 106/16:56Z - 17:09Z to verify the 10 Hz. Magnetic Field model. The first FHST 1 OBAD with FHST in simultaneous Rate Control was successfully performed @ 106/19:39Z, mapping 4 stars. The second FHST 3 OBAD with FHST 1 in simultaneous Rate Control was successfully performed @ 106/21:15Z, mapping 6 stars. All FSW functions executed nominally, SAC is in the process of comparing the results of both OBADs to the FSW table dumps captured. Verification activities will resume at ~ 107/12:58Z with Rate Control monitoring periods on FHST 2. |
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