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Daily 3576
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3576 PERIOD COVERED: DOY 83 OBSERVATIONS SCHEDULED ACS 9468 ACS Grism Parallel Survey of Emission- line Galaxies at Redshift z pl 7 We propose an ACS grism parallel survey to search for emission-line galaxies toward 50 random lines of sight over the redshift interval 0 zpl 7. We request ACS parallel observations of duration more than one orbit at high galactic latitude to identify ~ 300 HAlpha emission-line galaxies at 0.2pl zpl 0.5, ~ 720 O IILambda3727 emission-line galaxies at 0.3pl zpl 1.68, and pg 1000 Ly-alpha emission-line galaxies at 3pl zpl 7 with total emission line flux fpg 2* 10^-17 ergs s^-1 cm^-2 over 578 arcmin^2. We will obtain direct images with the F814W and F606W filters and dispersed images with the WFC/G800L grism at each position. The direct images will serve to provide a zeroth order model both for wavelength calibration of the extracted 1D spectra and for determining extraction apertures of the corresponding dispersed images. The primary scientific objectives are as follows: {1} We will establish a uniform sample of HAlpha and O II emission-line galaxies at z1.7 in order to obtain accurate measurements of co-moving star formation rate density versus redshift over this redshift range. {2} We will study the spatial and statistical distribution of star formation rate intensity in individual galaxies using the spatially resolved emission-line morphology in the grism images. And {3} we will study high-redshift universe using Ly-alpha emitting galaxies identified at z pl 7 in the survey. The data will be available to the community immediately as they are obtained. ACS/HRC/WFC 10059 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/HRC/WFC 9919 The Morphological, Photometric, and Spectroscopic Properties of Intermediate Redshift Cluster Galaxies: New and fundamental constraints on the evolutionary state of high redshift clusters will be made by obtaining deep, multiband images {SDSS r, i, z} over the central 1.5 Mpc regions of seven distant clusters in the range 0.76 z 1.27. The ACS data will allow us to {1} definitively establish the morphological composition and star formation rates as functions of clustercentric radius, local density, x-ray luminosity {obtained from accompanying Chandra, and XMM data}, {2} explore the relationship between substructure, kinematics, and morphology, {3} strongly constrain the galaxy merger frequency and the origins of elliptical and S0 galaxies, {4} measure the mass distribution independently from the light {via gravitational lensing} enabling comparisons with kinematically derived masses, and {5} study the evolution of the structure of the brightest cluster members. The clusters selected for this program already have extensive spectroscopic observations and NIR imaging is either in hand or underway from approved ground based programs. To date, the lower part of this redshift range has only been marginally studied with HST. Our sample includes the two most distant, spectroscopically confirmed superclusters and will significantly increase the baseline over which evolutionary effects can be studied. The data will also be used to identify very high-z galaxies via their unique spectral properties. ACS/NIC 9452 Characterizing the Star Formation History of a Highly Magnified z=5.6 Lyman Alpha Source We have located a remarkably faint pair of compact images arising from a z=5.6 Lyman Alpha emitting source, magnified 33-fold by the lensing foreground cluster Abell 2218. Keck spectra verify the lensing hypothesis but fail to locate any UV stellar continuum to interesting limits, suggesting the object is a 10^6 M_sun source viewed close to its epoch of formation. We argue the source could be representative of an abundant population of low mass systems forming their first stars at z5, this example becoming visible only by virtue of the strong gravitational magnification. We seek HST imaging to provide much tighter constraints on the nature and distribution of starlight in this intriguing source. ACS will be used to investigate the spatial extent of UV continuum light on 100 pc scales also providing the equivalent width of the Lyman Alpha emission. NIC will be used to measure the slope of the rest- frame continuum in order to break age and mass degeneracies caused by the unknown amount of dust extinction. HST uniquely provides the resolution and sensitivity to gather detailed information on a remarkable source which may be representative of a population seen in future surveys with NGST. ACS/WFC 9575 Default {Archival} Pure Parallel Program. The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels in POMS. ACS/WFC 9701 ACS Default {Archival} Pure Parallel Program II The proposal is designed to test ACS pure parallels in POMS. ACS/WFC 9744 HST Imaging of Gravitational Lenses Gravitational lenses offer unique opportunities to study cosmology, dark matter, galactic structure, galaxy evolution and quasar host galaxies. They are also the only sample of galaxies selected based on their mass rather than their luminosity or surface brightness. While gravitational lenses can be discovered with ground-based optical and radio observations, converting them into astrophysical tools requires HST. We will obtain ACS/WFC V and I images and NICMOS H images of 21 new lenses never observed by HST and NICMOS H images of 16 lenses never observed by HST in the IR. As in previous cycles, we request that the data be made public immediately. 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 9972 Calibrating the Mass-Luminosity Relation at the End of the Main Sequence We propose to use HST-FGS1R to calibrate the mass-luminosity relation {MLR} for stars less massive than 0.2 Msun, with special emphasis on objects near the stellar/brown dwarf border. Our goals are to determine M_V values to 0.05 magnitude, masses to 5 than double the number of objects with masses determined to be less than 0.20 Msun. This program uses the combination of HST-FGS3/FGS1R at optical wavelengths and ground-based infrared interferometry to examine nearby, subarcsecond binary systems. We are deriving high quality luminosities and masses for the components in the observed systems, and characterizing their spectral energy distributions from 0.5 to 2.2 Mum. Several of the objects included have M 0.1 Msun, placing them at the very end of the stellar main sequence. Three of the targets are brown dwarf candidates, including the current low mass record holder, GJ 1245C, with a mass of 0.062 +/- 0.004 Msun. The payoff of this proposal is high because all 10 of the systems selected have already been resolved with HST- FGS3/FGS1R during Cycles 5--10 and contain most of the reddest objects for which masses can be determined. 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 9801 Are OH/IR Stars the Youngest post-AGB stars? A NICMOS Imaging Survey Essentially all well-characterized preplanetary nebulae {PPNe}-- objects in transition between the AGB and planetary nebula evolutionary phases - are bipolar, whereas the mass-loss envelopes of AGB stars are strikingly spherical. In order to understand the processes leading to bipolar mass-ejection, we need to know at what stage of stellar evolution does bipolarity in the mass-loss first manifest itself. We have recently hypothesized that most OH/IR stars {evolved mass- losing stars with OH maser emission} are very young PPNe. We are conducting a multiwavelength survey program of imaging and spectroscopic observations of such objects, using a large, morphologically unbiased sample selected using IRAS 12-to-25 micron colors. Our ongoing HST/SNAP imaging survey of the optically bright half of this sample with WFPC2 and ACS is highly successful: 19/32 objects observed are extended with bipolar/multipolar shapes {remaining objects are unresolved}. Slightly more than 50% of our sample are optically too faint or undetected but have strong near-IR counterparts -- we therefore propose a NICMOS SNAPshot imaging survey of these optically-faint OH/IR stars. These observations are crucial for determining how and when the bipolar geometry asserts itself. The results from our NICMOS survey {together with the WFPC2/ACS survey} will allow us to draw general conclusions about the onset of bipolar mass-ejection during late stellar evolution. Our complementary program of interferometric mapping of the OH maser emission in our sources is yielding kinematic information with spatial resolution comparable to that in the HST images. The HST/radio data will provide crucial input for theories of post-AGB stellar evolution. In addition, these data will also indicate whether the multiple concentric rings, "searchlight beams'', and truncated equatorial disks recently discovered with HST in a few PPNe, are common or rare phenomena. 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 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 10085 STIS Pure Parallel Imaging Program: Cycle 12 This is the default archival pure parallel program for STIS during cycle 12. 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. 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 10084 WFII parallel archive proposal This is the generic target version of the WFPC2 Archival Pure Parallel program. The program will be used to take parallel images of random areas of the sky, following the recommendations of the 2002 Parallels Working Group. WFPC2 10090 WFII backup parallel archive proposal This is a POMS test proposal designed to simulate scientific plans. 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 6 6 FGS REacq 5 5 FHST Update 17 17 LOSS of LOCK SIGNIFICANT EVENTS: Set-up and execution of HST Battery Reconditioning Macro Ops Acceptance Test scheduled 084/11:00Z - 085/05:00Z with GDOC, HITT, SE, and VEST using CCS "D" (Prime) String with CCS Release 5.0.3.1 and PRD O06300ST and CCS "C" (Secondary) String with CCS Release 4.0.3.1 and PRD O06300T. The purpose of this testing is to verify installation and back-out procedures for the Battery Reconditioning Macro have capability to work in an operational scenario. |
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