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Daily 3603
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3603 PERIOD COVERED: DOYs 121-123 OBSERVATIONS SCHEDULED 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/CCD 9906 Volatile Abundances and the D/H Ratio in Long-Period Comets Comet NEAT {C/2001 Q4} is predicted to reach naked-eye visibility in the spring of 2004, under excellent conditions for observations with HST. Although predicting cometary magnitudes more than 1 year in advance is notoriously risky, C/NEAT seems likely to be exceptionally active, allowing us for the first time to perform sensitive measurements of the D/H and OD/OH ratios. Accurate measurements of the deuterium abundance in comets, which can vary in different species, are crucial for determining if comets retain a signature of their possible interstellar origin and if they supplied a significant fraction of the water on Earth. HST observations of C/NEAT will additionally provide accurate abundances for highly volatile ices in the nucleus, such as CO, CO2 {via Cameron band emission}, and S2, which also provide important insights on the comet's origin and evolution. This opportunity in cycle 12 is unique in the history of HST and is unlikely to be repeated during its remaining lifetime. 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. WFPC2 9870 Low Mass Star Formation at Low Metallicity: Accretion Rates of Pre-Main Sequence Stars in the Large Magellanic Cloud As part of an ongoing effort to characterize the process of star formation at low metallicity, we propose to measure by means of U-band excess the current accretion rate for a homogenous sample of newly-born stars in NGC 1850, a young {5 Myr} stellar cluster in the LMC. Clearly, at this age most of the accretion has already taken place and its intensity is declining with respect to the earliest stages of formation. However, a comparison with Galactic Pre-Main Sequence stars of the same age immediately leads to assessing the relative strength of accretion when the metallicity is decreased by a factor of three. We have already analyzed the images available in the archive for these fields and we have determined the basic parameters {effective temperature and luminosity} for all of the stars down to a mass of ~0.9 Mo. To take the next step and determine the current accretion rate we only need WFPC2 imaging of NGC 1850 in the F336W passband. With three orbit worth of observations, we will reach m{F336W}~23 with an accuracy of 0.1 mag. In spite of their unique scientific potential, the data we apply for are relatively inexpensive to gather, as they are the last missing tile of a large dataset already available in the HST archive. 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. 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. 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 9782 Measuring Black Hole Masses in Double Peaked Broad Lined AGNs To date there have been few black hole {BH} mass estimates for luminous broad line AGN, including those derived from reverberation mapping. In this context, objects with "double-peaked" broad lines are particularly important because the line emission is believed to arise in a relativistically rotating accretion disk. If this model is correct, then the BH mass can be determined directly from periodic variations in the line-profile shape. In two cases {Arp 102B and NGC 1097} such variations have been claimed. The goal of this proposal is to confront the relativistic disk model for the double-peaked Balmer lines with independent limits on the central masses for 5 of the nearest and brightest "double-peaked emitters" {NGC 1097, Arp 102B, Pictor A, 3C390.3, 3C332}, determined by using STIS long-slit spectroscopy to map the velocity field of circum-nuclear ionized gas. These observations will critically test the idea that the line emission in these objects comes from an accretion disk and thus provide unique insights into the physical processes operating in both the BLR and the "central engine". 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. 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 10073 Earth Flats This proposal monitors flatfield stability. This proposal obtains sequences of Earth streak flats to construct high quality flat fields for the WFPC2 filter set. These flat fields will allow mapping of the OTA illumination pattern and will be used in conjunction with previous internal and external flats to generate new pipeline superflats. These Earth flats will complement the Earth flat data obtained during cycles 4-11. 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. WFPC2 10068 WFPC2 CYCLE 12 Standard Darks This dark calibration program obtains dark frames every week in order to provide data for the ongoing calibration of the CCD dark current rate, and to monitor and characterize the evolution of hot pixels. Over an extended period these data will also provide a monitor of radiation damage to the CCDs. 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 10049 ACS Internal Flat Field Stability The stability of the CCD flat fields will be monitored using the calibration lamps and a sub-sample of the filter set. High signal observations will be used to assess the stability of the pixel-to- pixel flat field structure and to monitor the position of the dust motes. Shorter exposures will be used to identify charge traps and to assess the stability of the DQ arrays. Only internal exposures with the calibration lamps will be required. 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. STIS/CCD 10016 STIS CCD Performance Monitor This activity measures the baseline performance and commandability of the CCD subsystem. Only primary amplifier D is used. Bias and Flat Field exposures are taken in order to measure bias level, read noise, CTE, and gain. Numerous bias frames are taken to permit construction of "superbias" frames in which the effects of read noise have been rendered negligible. Full frame and binned observations are made, with binning factors of 2 x 1, 1 x 2, 2 x 2, 4 x 1, and 4 x 2. Bias frames are taken in subarray readouts to check the bias level for ACQ and ACQ/PEAK observations. All exposures are internals. WFPC2/ACS/HRC/WFC 10013 Focus Monitor The focus of HST is measured from WFPC2/PC and ACS/HRC images of stars. Multiple exposures are taken in parallel over an orbit to determine the influence of breathing on the derived mean focus. Observations are taken of clusters with suitable orientations to ensure stars appear in all fields. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) HSTAR 9405: FHST Roll Delay Update (U1,3RD) @ 122/14:33:49Z failed with Error Box results reading "1 FAILED". Under investigation. COMPLETED OPS REQs: 17160-0 MTS Compensated MSS Data Collection @ 123/23:48z OPS NOTES EXECUTED: 1231-1 Packet Filter and CCC config for On-going Network changes @ 121/13:08z 1232-0 MSS Data Collection Ops Req # 17160-0, @ 123/23:48z 1233-0 Adjust ACS Error Count Limit (ACS 935) @ 122/14:44z. 1233-1 Adjust ACS Error Count Limit (ACS 935) @ 122/19:03z 1233-2 Adjust ACS Error Count Limit (ACS 935) @ 122/21:26z SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 36 36 FGS REacq 13 13 FHST Update 43 42 See Hstar # 9405 LOSS of LOCK SIGNIFICANT EVENTS: None |
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