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Daily 3605
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3605 PERIOD COVERED: DOY 125 OBSERVATIONS SCHEDULED ACS 9476 Galaxy Evolution in the Richest Clusters at z=0.8: the EDisCS Cluster Sample The study of distant cluster galaxies requires two key ingredients: {1} deep high-resolution imaging, to constrain galaxy structure; and {2} 8m-class spectroscopy, to measure stellar content, star-formation rates, dynamics, and cluster membership. We will reach both conditions with the addition of HST/ACS imaging to our suite of VLT {36 nights} and NTT {20 nights} observations of 10 confirmed clusters at z~0.8, drawn from the ESO Distant Cluster Survey {EDisCS}. The proposed HST/ACS data will complement our existing optical/IR imaging and spectroscopy with quantitative measures of cluster galaxy morphologies {i.e. sizes and shapes, bulge-disk decompositions, asymmetry parameters}, and with measurements of cluster masses via weak lensing. Major advantages unique to the EDisCS project include: {i} uniform selection of clusters; {ii} large enough sample sizes to characterize the substantial cluster-to-cluster variation in galaxy populations; {iii} large quantities of high quality data from 8m telescopes; {iv} uniform measurements of morphologies, spectroscopic and photometric redshifts, SEDs, star-formation/AGN activities, and internal kinematics; {v} optical selection of clusters to complement the X-ray selection of almost all high-z clusters in the ACS GTO programs; {vi} forefront numerical simulations designed specifically to allow physical interpretation of observed differences between the high-z and local clusters. ACS/HRC 9746 Binary systems in the Kuiper Belt The properties of the orbits of Kuiper belt object {KBO} satellites hold keys to fundamental insight into masses and densities of KBOs, the interaction history of the early solar system, the internal structure of distant ice-rock bodies, and even the genesis of the Pluto-Charon binary. Within the past 18 months, 9 KBO satellite systems have been discovered, allowing for the first time the possibility of characterizing a sample of KBO satellite orbital properties. We propose HRC observations to determine satellite orbits in the 6 best cases. We have carefully devised a strategy for each of these 6 systems to make maximum use of ground-based observations, previous HST observations, and the smallest possible number of new HST observations. Our proposed observations will efficiently provide highly reliable orbital solutions which are critical to achieving the scientific promise available from the study of these systems. Our strategy relies heavily on extensive Monte Carlo simulations to define optimal times of observing such that each new point obtained gives maximum leverage for refining the orbital solution. We find that with this strategy we can provide mass solutions for all 6 systems to an accuracy of better than 10% using only 25 new HST observations. This highly efficient program provides extreme scientific output with optimal use of scarce resources. 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 9766 The Globular Cluster Systems of Spiral Galaxies along the Hubble Sequence While the globular cluster {GC} systems of ellipticals and ongoing mergers have been relatively well-studied with HST, very little is known about the GC systems of spirals besides the Milky Way and M31. To constrain GC/galaxy formation models, especially where spirals are the merger progenitors of ellipticals, it is crucial to understand their GC properties. We propose to obtain ACS images of three edge-on spirals, spanning the Hubble sequence, with Keck spectroscopic follow-up. This will effectively double the number of well-studied spiral systems. We will detect 100-200 GCs per galaxy, sufficient to reveal GC subpopulations, their relative numbers, radial trends, and dependences on Hubble type {e.g., a bulge vs. disk origin for red GCs}. For half of our GCs we will be able to measure individual sizes. By providing a much-needed comparative benchmark, these data will allow researchers to better exploit the large existing HST database of GCs in E/S0 galaxies. 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. There is no other instrument on or off the earth that can consistently deliver HST FGS level of precision for critical parallaxes. 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. 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 9723 Deep NICMOS imaging We have obtained ultra-deep Js, H, Ks imaging of the Hubble Deep Field South WFPC2 field with the VLT, in order to study high redshift galaxies. The Ks-band data are the deepest obtained to date in any field. We find that the population of Ks selected galaxies at z=2-4 in HDF-South differs in two important aspects from previous studies in HDF-North. First, we find several galaxies which are large and apparently regular in the rest-frame optical, with more complex rest- frame UV morphologies. These objects resemble large disk galaxies in the local Universe. Second, we have identified a population of galaxies with red J-K colors that are extremely faint in the rest-frame UV. The galaxies have ages of 0.5-2 Gyr and are highly clustered, and may be progenitors of nearby bulges and early-type galaxies. We propose to obtain a deep mosaic with the NICMOS/NIC3 camera in the H band, covering the WFPC2 field. The increased depth and spatial resolution of the NICMOS mosaic would allow us to determine the restframe optical morphologies of a large sample of high redshift galaxies, in order to study the relative distributions of young and old stars, to decompose the galaxies in bulges and disks, to measure scale lengths, and to model the stellar populations of the sub-components. The lack of large U- dropouts and red galaxies in HDF-North, and the need for larger samples call for the proposed imaging of HDF-South. We waive all prioprietary rights. 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 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. 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: NONE OPS NOTES EXECUTED: 1234-0 TDW Cross-support tracking (T77 CODE) @ 125/18:00z 1234-0 TDW Cross-support tracking (T77 CODE) @ 126/04:21z SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 07 07 FGS REacq 08 08 FHST Update 14 14 LOSS of LOCK SIGNIFICANT EVENTS: None |
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