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Daily 3634
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3634 PERIOD COVERED: DOY 167 OBSERVATIONS SCHEDULED 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 coronagraphic monitoring is required to assess the changing position of the spots. ACS/HRC 9703 Coronagraphic Search for Planets around Nearby Stars We will use the HRC coronagraph to search for planets, disks, and exo-zodiacal dust around nearby stars. We have selected the following stars: alpha Cen A and B, tau Ceti, and epsilon Eridani. The observations of each star will be taken at two or more epochs. The observations will be broken into a sequence of short exposures and taken at different roll angles to compensate for "telescope breathing" during the orbit. As a further precaution, the observations will be scheduled after the closest possible nearby pointing in order to minimize thermal changes in the OTA during the first orbit of observations. After matching phases, the PSFs from one star will be subtracted from the other star. ACS/HRC 9896 A Survey of Extinction Curves to Redshift z=1 The effects of dust are crucial to the study of galaxies {through models of galaxy evolution and star formation rates/histories}, cosmology {e.g., through its effects on SNe Ia fluxes}, and the interpretation of gamma-ray burst afterglows. However, classical methods for obtaining precise extinction curves cannot be applied outside the Local Group. Recently, we demonstrated that gravitational lenses can be used to measure extinction curves at intermediate redshifts with high accuracy. We propose a survey of the extinction curves in 6 lens galaxies known to contain dust, to study the evolution of dust properties in galaxies out to z=1. We will obtain multi-wavelength photometry {6 filters from 8140 A to 2550 A} of each system to {1} construct non-parametric extinction curves which overlap the 2175 A feature, {2} measure R{V} to a 2-sigma accuracy better than 0.5 for parametric models of Galactic dust, and {3} discriminate between Galactic and SMC extinction curves to better than 2-sigma accuracy. The compact angular size of the lens systems {1-2 arcsec} and the need for near-UV images means that HST is required to make the measurements. 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/HRC 9771 The local Hubble flow and the density field within 6 Mpc Great progress has been made recently in accurate distance measurements of nearby galaxies beyond the Local Group based on the luminosity of the tip of the red giant branch {TRGB}. Over the last three years, snapshot surveys with HST have provided us with the TRGB distances for more than a hundred nearby galaxies obtained with an accuracy of about 10%. The local velocity field within 5 Mpc exhibits a significant anisotropy which disagrees with a spherical Virgo-centric flow. The local Hubble flow is very cold, with 1-D rms deviations of ~30 km/s. Cosmological simulations with Cold Dark Matter can only realize such low dispersions with a combination of a low mean density of matter and a substantial component with negative pressure. There may be a constraint on the equation of state w=-p/rho. Our observations will concentrate on 116 galaxies whose expected distances lie within 4 - 6 Mpc, allowing us to trace a Dark Matter distribution in the Local Volume with twice the information currently available. The program is a good one for SNAP mode because the order and rate that the observations are made are not very important, as long as there is good completion over several years. 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. 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. NIC3 9878 The Age and Mass Function of the Intermediate Age Globular Cluster System of NGC 4365 We propose to obtain deep H-band photometry of the globular cluster system of the elliptical galaxy NGC 4365, which has previously been shown from shallow data to have a significant population of intermediate-age globular clusters. These data will allow us to constrain the luminosity and mass function of the intermediate-aged globular cluster system. This is a critical step in understanding the relationship between the young dense star cluster systems observed in galaxy mergers and starbursts, which have a power-law mass functions, and well known old, globular cluster systems, which have a lognormal mass functions. Specifically, the large intermediate-age cluster population in NGC 4365 provides the best case to test whether the power-law mass function of young systems evolves into a lognormal with the properties of old globular cluster systems. Dynamical models have long suggested such an evolution of a power-law mass function to a roughly log-normal one but there is no clear observational evidence yet in elliptical galaxies for steps along this process. Our proposed study of the intermediate-age cluster system of NGC 4365 will provide us with the fundamental information needed to conclusively establish the relationship between young and old globular cluster systems. 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. 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 10030 STIS/CCD Spectroscopic Sensitivity Monitor for Cycle 12 Monitor sensitivity of each CCD grating mode to detect any change due to contamination or other causes. STIS/CCD/MA1/MA2/WFPC2 9828 Young Massive Clusters in M33 Young Massive Clusters {YMC} appear to be abundantly forming in merging galaxies, but are not found in the Milky Way. They provide the opportunity to study the conditions necessary for the formation of massive, compact stellar systems, giving insight into conditions of the earliest epochs of galaxy formation, when ancient Globular Clusters {GC} formed, thus helping to constrain scenarios of galaxy formation and evolution. We propose STIS UV spectroscopy of three extremely young, UV-luminous clusters in the Local Group spiral galaxy M33, selected from our extensive survey with WFPC2 imaging. From multi-band integrated photometry we inferred age upper limits of 10 Myrs: UV spectra will provide precise ages, thus masses, for these objects from the earliest spectral types present, revealed by the strong spectral signatures, and from synthetic spectral modeling. We will be able to assess whether their mass overlap with GC masses, and whether such systems can survive internal dynamical evolution. These young, massive and compact objects provide a key link to the young cluster systems in mergers, and may be the only such counterparts accessible to detailed studies. 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. 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 9 9 FGS REacq 4 4 FHST Update 16 16 LOSS of LOCK SIGNIFICANT EVENTS: An additional series of FHST Rate Control and Intensity data collections (6 each) are scheduled during SMS SA166O01 on Days 168 through 170. These activities provide additional high-rate FHST data in support of the development of the T2G mode of the Two Gyro Science effort. Each of the 12 intervals involves a brief (10 - 15 minutes) transition to PN format and utilizes 4 TMDIAG slots. The 6 Intensity collections also involve the DIU Reader. Total time in PN format during the three days should be 170 minutes. All commanding is conducted on a non interference basis (NIB) with routine or contingency spacecraft activities. Periods of scheduled astrometry and other critical science with SMS SA166O01 is specifically avoided. See Ops Request for details. Intensity: FHST2 168/21:09:30 - 168/21:40:19Z FHST1 168/23:47:35 - 169/00:23:00Z FHST3 168/23:47:35 - 169/00:23:00Z |
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