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Daily 3888
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3888 PERIOD COVERED: UT June 23, 2005 (DOY 174) OBSERVATIONS SCHEDULED ACS/HRC 10391 Wavelength and Flux Calibration of the ACS prisms The wavelength calibration of the SBC {PR110L and PR130L} and HRC {PR200L} prisms will be established by observing a planetary nebula in the LMC and QSOs at carefully selected redshifts. Flux calibrations will be derived for each prism by observing white dwarf standards. ACS/WFC 10152 A Snapshot Survey of a Complete Sample of X-ray Luminous Galaxy Clusters from Redshift 0.3 to 0.7 We propose a public, uniform imaging survey of a well-studied, complete, and homogeneous sample of X-ray clusters. The sample of 73 clusters spans the redshift range between 0.3-0.7. The samples spans almost 2 orders of magnitude of X-ray luminosity, where half of the sample has X-ray luminosities greater than 10^44 erg/s {0.5- 2.0 keV}. These snapshots will be used to obtain a fair census of the the morphology of cluster galaxies in the cores of clusters, to detect radial and tangential arc candidates, to detect optical jet candidates, and to provide an approximate estimate of the shear signal of the clusters themselves, and potentially an assessment of the contribution of large scale structure to lensing shear. ACS/WFC 10416 Star Formation Driven Outflows in Actively Star Forming Edge-on Spiral Galaxies We will investigate the disk-halo interaction in four actively star forming edge-on spiral galaxies using the ACS. In recent years considerable progress has been achieved in testing the disk-halo interaction scenario which describes the large scale mass exchange of the ISM between disk and halo including the metal enrichment of the IGM, which is on galactic scales described by various theoretical models {e.g., galactic fountains, chimneys, superwinds}. The investigation of nearby edge-on spirals in this respect offers a particularly exciting perspective for a quantitative understanding of this feedback provided by star formation on the ISM. Feedback is the crucial ingredient in all models of galaxy formation and evolution. While commonly implemented in simple terms {global energy or metal injection}, further progress can only be achieved with a better understanding of the relevant physics. This requires high spatial resolution studies of nearby galaxies. Whereas groundbased observations are perfectly suited to study the overall morphology of the outflowing gas, they are inadequate to describe the structure on the smallest relevant scales. However, it is the small scale structure that constrains the microphysics to be applied in theoretical models of a multiphase medium. Galaxies spanning a wide range of star formation activity have to be investigated in order to test which processes for the gas ejection are at work. High spatial resolution studies, as can be achieved with the ACS onboard HST and yielding a spatial resolution of 3-7 parsecs for the four proposed target galaxies, will critically test the existing models for the feedback process. ACS/WFC/WFPC2/NIC3 10395 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. NIC1 10143 Ultracool companions to the nearest L dwarfs We propose to conduct the most sensitive survey to date for low mass companions to nearby L dwarfs. We will use NICMOS to image targets drawn from a volume-complete sample of 70 L dwarfs within 20 parsecs. The combination of infrared imaging and proximity will allow us to search for T dwarf companions at separations as small as 1.6 AU. This is crucial, since no ultracool binaries are currently known with separations exceeding 15 AU. Only 10 dwarfs in this sample have previous HST observations primarily at optical wavelengths. With the increased sensitivity of our survey, we will provide the most stringent test to date of brown dwarf models which envisage formation as ejected stellar embryos. In addition, our observations will be capable of detecting binaries with mass ratios as low as 0.3, and will therefore also test the apparent preference for equal-mass ultracool binaries. Finally, our observations offer the best prospect to date of detecting companions significantly cooler than the coolest t dwarf currently known. 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. NIC2 10147 Detecting the elusive low mass companion around epsilon Indi We propose coronagraphic NICMOS observations of the nearby {d = 3.6 pc} K5V star epsilon Indi {HD 209100} to search for the unknown companion which causes a low amplitude radial velocity {RV} trend in our 11 years of precise Doppler measurements. This RV data set places a lower limit of 4.5 AU for the orbital semimajor axis of this companion. Moreover, the fact that the RV trend is lacking any sign of curvature over this long time period clearly points towards a much larger orbital separation. Epsilon Indi also has a T dwarf {binary} companion at a separation of 1400 AU. However, these brown dwarf companions are too distant from the primary to induce the observed RV variation. It is also unlikely that this nearby star has an unknown stellar {M dwarf} companion. The RV signal is thus most probably caused by a yet unknown giant planetary or brown dwarf companion at a separation of more than 5 AU. Because epsilon Indi is so near to the Sun, it constitutes an ideal target for high contrast imaging with NICMOS in its coronagraphic mode. Indeed, NICMOS coronagraphy is capable of detecting objects down to 15 Jupiter masses at separations greater than 2.3 arcseconds {S/N=25} - precisely the separation and mass range indicated by our Doppler spectroscopy. Only 2 orbits of HST/NICMOS observations could directly image the coolest and lowest mass companion ever found around a solar-type star. NIC2 10176 Coronagraphic Survey for Giant Planets Around Nearby Young Stars A systematic imaging search for extra-solar Jovian planets is now possible thanks to recent progress in identifying "young stars near Earth". For most of the proposed young {~ 30 Myrs} and nearby {~ 60 pc} targets, we can detect a few Jupiter-mass planets as close as a few tens of AUs from the primary stars. This represents the first time that potential analogs of our solar system - that is planetary systems with giant planets having semi-major axes comparable to those of the four giant planets of the Solar System - come within the grasp of existing instrumentation. Our proposed targets have not been observed for planets with the Hubble Space Telescope previously. Considering the very successful earlier NICMOS observations of low mass brown dwarfs and planetary disks among members of the TW Hydrae Association, a fair fraction of our targets should also turn out to posses low mass brown dwarfs, giant planets, or dusty planetary disks because our targets are similar to {or even better than} the TW Hydrae stars in terms of youth and proximity to Earth. Should HST time be awarded and planetary mass candidates be found, proper motion follow-up of candidate planets will be done with ground-based AOs. LIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) HSTARS: (None) COMPLETED OPS REQUEST: (None) COMPLETED OPS NOTES: (None) SCHEDULED SUCCESSFUL FAILURE TIMES FGS Gsacq 15 15 FGS Reacq 04 04 FHST Update 17 17 LOSS of LOCK SIGNIFICANT EVENTS: |
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