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Daily 3493
HUBBLE SPACE TELESCOPE
DAILY REPORT # 3493 PERIOD COVERED: DOYs 322-323 OBSERVATIONS SCHEDULED ACS/HRC 9989 Starburst Galaxies and Their Population of Super Star Clusters Starbursts are ideally suited to study the evolution of high mass stars, the physics of star formation, and the chemical enrichment of the intergalactic medium {IGM}. Starbursts efficiently form Super Star Clusters {SSC} which may be young protoglobular clusters. High resolution imaging will address two important outstanding issues: 1} how long starbursts last and 2} whether SSCs are indeed young globular clusters. The duration of starbursts is important because: {1} it determines how efficiently a starburst can heat and enrich the IGM; {2} the duration combined with estimates of the fraction of galaxies which host starbursts yields the total number of starbursts a galaxy can suffer. Finally, since local starbursts are analogs to high-z galaxies, the results have implications on the initial formation timescale of galaxies. Starburst duration will be determined from HRC imaging of two face-on starburst galaxies rich in SSCs. The UV to optical colors of the SSCs, which represent single burst chronometers, will yield their reddening and ages. The range of ages gives the starburst duration. The nature of SSCs will be investigated by imaging four of the nearest starbursts in 3 bands. By comparing the sizes of their SSCs at different wavelengths we will address the issue of whether SSCs suffer from early mass segregation. Without some mass segregation the velocity dispersions of SSCs suggest that they are deficient in low mass stars, and hence may not represent true proto-globular clusters. ACS 9984 Cosmic Shear With ACS Pure Parallels Small distortions in the shapes of background galaxies by foreground mass provide a powerful method of directly measuring the amount and distribution of dark matter. Several groups have recently detected this weak lensing by large-scale structure, also called cosmic shear. The high resolution and sensitivity of HST/ACS provide a unique opportunity to measure cosmic shear accurately on small scales. Using 260 parallel orbits in Sloan textiti {F775W} we will measure for the first time: beginlistosetlength sep0cm setlengthemsep0cm setlength opsep0cm em the cosmic shear variance on scales 0.7 arcmin, em the skewness of the shear distribution, and em the magnification effect. endlist Our measurements will determine the amplitude of the mass power spectrum sigma_8Omega_m^0.5, with signal-to-noise {s/n} ~ 20, and the mass density Omega_m with s/n=4. They will be done at small angular scales where non-linear effects dominate the power spectrum, providing a test of the gravitational instability paradigm for structure formation. Measurements on these scales are not possible from the ground, because of the systematic effects induced by PSF smearing from seeing. Having many independent lines of sight reduces the uncertainty due to cosmic variance, making parallel observations ideal. NIC/NIC3/STIS/CCD 9877 A test of the foreground proximity effect at z=1.2 The diffuse UV background flux J is a crucial component for cosmological evolution models, though few determinations have been made. The prox- imity effect, the thinning out of the Lyman alpha forest near a sight- line's background quasar and explained at least partly by the enhanced ionization from the quasar, is a key method to measure J. A foreground proximity effect {FPE} should exist from quasars close on the sky but at different z; it can constrain J and test the enhanced ionization model. Galaxy clustering around the quasar may modify the effect, but knowing the galaxy density around the Lya forest should allow for corrections. We propose to measure the FPE at z=1.2, which is advantageous because 1} the diffuse UV flux is lower, and thus contrast with the UV flux of neighboring quasars is higher, and 2} galaxies are easier to identify at z=1.2. We have good knowledge of the physical volume we wish to study through surveys for quasars, MgII absorbers and galaxies, to constrain the redshift-dependent galaxy density along the line of sight. We will analyze the results based on pixel opacities, which is more sensitive to fluctuations in J than traditional line counting, and will compare our results with cosmological simulations to derive estimates of the UV background in the context of available physical models. NIC2 9875 The Fundamental Plane of Massive Gas-Rich Mergers We propose deep NICMOS H-band imaging of a carefully selected sample of 33 luminous, late-stage galactic mergers. This program is part of a comprehensive investigation of the most luminous mergers in the nearby universe, the ultraluminous infrared galaxies {ULIGs}. The high-resolution HST images will complement an extensive set of ground-based data that include long-slit NIR spectra from a recently approved Large VLT Programme. This unique dataset will allow us to derive with unprecedented precision structural -and- kinematic parameters for a large unbiased sample of objects spanning the entire ULIG luminosity function. These data will refine the fundamental plane of massive gas-rich mergers and enable us to answer the following questions: {1} Do ultraluminous mergers form elliptical galaxies, and in particular, giant ellipticals? {2} Do ULIGs evolve into optically bright QSOs? The results from this detailed study of massive mergers in the local universe will be relevant to understanding galaxy formation and evolution at earlier epochs, and in particular, the dusty sub-mm population that accounts for more than half of the star formation at z 1. 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. 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. Only HST observervations have the resolution to detect any changes in the morphologies of SCUBA galaxies with increasing cosmic time. 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. ACS/HRC 9823 Rings of Uranus: Dynamics, Particle Properties and Shepherding Moons We propose to image the rings and small inner satellites of Uranus using the High Resolution Channel of the ACS. The revolutionary capabilities of the ACS will allow us to address a variety of important questions relating to ring properties and ring-moon interactions. Observations at a range of wavelengths and phase angles will reveal the opposition surges of these rings and moons, providing information on color and surface structure. Measurements of the ring in front of the planet will provide complementary information on optical depth; any variations of optical depth with wavelength will reveal the rings' poorly-constrained population of embedded dust. The rings of Uranus are closing rapidly as the planet approaches equinox in 2007, an event that takes place only every 42 years. Using this opportunity, our observations will be repeated at different solar and terrestrial tilt angles; this sequence of images will be particularly valuable for constraining the physical thickness and packing density of the rings. We will place particular emphasis on the rotational variations of the Epsilon Ring, whose radial width {and therefore its packing density} varies by a factor of five. In addition, a set of deep exposures targeted just off the planet will enable us to detect any 4-5 km moons embedded within the ring system. Dynamicists invoke numerous such moons to "shepherd" the many sharp ring boundaries, so this will serve as a definitive test of the theory. NIC3/ACS/HRC/WFC 9803 Deep NICMOS Images of the UDF The ACS Ultra Deep Field {UDF} images will greatly enhance the rich suite of deep multi-wavelength images in the Chandra Deep Field South {CDF--S}. We propose to complete the image set with deep near-IR NICMOS images at 1.1 and 1.6 microns over a significant fraction of the UDF, providing a critical link between the HST ACS and SIRTF observations. The timely addition of the near-IR images ensures that investigators will have images that span the spectrum from X-ray to far IR. In recognition of the value of the near IR images this proposal is submitted as a Treasury proposal with no proprietary period. The proposal team will deliver science quality images, mosaiced images covering 4.9 sq arc min, and a photometric catalog complete to an AB mag of 28.2 in both the F110W and F160W filters. The program also delivers a parallel extremely deep ACS field, 8' away, that reaches to within 0.6 mag of the UDF in the same filters as the UDF. The scientific program of the proposal team focuses on the star formation history of the universe, evolved galaxies at high redshift, galaxies at the epoch of reionization, and the redshift evolution of AGNs and ULIRGs. The HDF-N is currently the only field with spatially-coincident deep HST imaging in both the optical and near-IR. The small size of the HDF-N means that large scale structure is the dominant error in the results from the HDF-N. Providing observations in a field that is spatially uncorrelated is critically important. The UDF/CDF-S fulfills that goal. The depth of the UDF ACS imaging, and the wealth of Great Observatory and ground based observations in the CDF-S, make these NICMOS observations uniquely valuable. An extraordinarily rich array of science opportunities await the community from the NICMOS UDF data. 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/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 lastthree 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. ACS/HRC 9747 An Imaging Survey of the Statistical Frequency of Binaries Among Exceptionally-Young Dynamical Families in the Main Asteroid Belt We propose an ambitious SNAPSHOT program to determine the frequency of binaries among two very young asteroid families in the Main Belt, with potentially profound implications. These families {of C- and S-type} have recently been discovered {Nesvorny et al. 2002, Nature 417, 720}, through dynamical modeling, to have been formed at 5.8 MY and 8.3 MY ago in catastrophic impact events. This is the first time such precise and young ages have been assigned to a family. Main-belt binaries are almost certainly produced by collisions, and we would expect a young family to have a significantly higher frequency of binaries than the background, because they may not yet have been destroyed by impact or longer-term gravitational instabilities. In fact, one of the prime observables from such an event should be the propensity for satellites. This is the best way that new numerical models for binary production by collisions {motivated largely by our ground-based discoveries of satellites among larger asteroids}, can be validated and calibrated. HST is the only facility that can be used to search for binaries among such faint objects {V17.5}. We will also measure two control clusters, one being an "old" family, and the other a collection of background asteroids that do not have a family association, and further compare with our determined value for the frequency of large main-belt binaries {2%}. We request visits to 180 targets, using ACS/HRC. 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. HST has demonstrated that it is the only telescope that can in each case precisely locate the lens galaxy, measure its luminosity, color and structure, and search for lensed images of the source host galaxy given the typical image separations of ~1''. 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. NIC3 9735 ACS, NICMOS, and STIS Observations of Three Ongoing Mergers We propose to make ACS {U, B, V, I, H_alpha}, NICMOS {J, H, K}, and STIS {long-slit H_alpha} observations of NGC 520, NGC 2623, and NGC 3256, three merging galaxies in the middle of the Toomre Sequence and currently in the throes of violent relaxation. Two of these {NGC 2623 and NGC 3256} are the most IR luminous galaxies in the sequence. Hence, these ongoing mergers are ideal candidates for studying the triggering mechanism responsible for the formation of stars and star clusters. The ACS observations will allow us to age date the star clusters, and reliably distinguish clusters from stars based on their apparent sizes. They will also be used in conjunction with ground-based measurements of the stellar velocity dispersion to determine dynamical masses of the clusters and hence address the question of whether the IMF is truncated. The NICMOS observations will allow us to penetrate the dust and answer several fundamental questions such as: What fraction of the young clusters are hidden by dust? How do these clusters form and evolve? The STIS observations will allow us to study the kinematics of the young cluster system and measure the pressure and shock properties which may be triggering the formation of the clusters. A better understanding of how mergers form tremendous numbers of clusters and stars in the local universe will help shed light on processes that were crucial during galaxy assembly in the high-z universe. WFPC2 9712 Pure Parallel Near-UV Observations with WFPC2 within High-Latitude ACS Survey Fields In anticipation of the allocation of ACS high-latitude imaging survey{s}, we request a modification of the default pure parallel program for those WFPC2 parallels that fall within the ACS survey field. Rather than duplicate the red bands which will be done much better with ACS, we propose to observe in the near-ultraviolet F300W filter. These data will enable study of the rest-frame ultraviolet morphology of galaxies at 0z1. We will determine the morphological k-correction, and the location of star formation within galaxies, using a sample that is likely to be nearly complete with multi-wavelength photometry and spectroscopic redshifts. The results can be used to interpret observations of higher redshift galaxies by ACS. WFPC2 9709 POMS Test Proposal: 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. FGS 9335 Masses of Pre-Main Sequence Binaries We propose to continue to map the orbits of young star binaries in the Taurus and Ophiuchus star forming regions. Our goal is to measure their masses dynamically. This is important because there are still no low mass young stars with reliably known masses so calculations of their evolution to the main sequence are uncalibrated. NICMOS 8790 NICMOS Post-SAA calibration - CR Persistence Part 1. 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. WFPC2 10082 POMS Test Proposal: WFII backup parallel archive proposal This is a POMS test proposal designed to simulate scientific plans WFPC2 10075 WFPC2 CYCLE 12 Intflat and Viflat Sweeps and Filter Rotation Anomaly Monitor Using intflat observations, this WFPC2 proposal is designed to monitor the pixel-to-pixel flatfield response and provide a linearity check. The intflat sequences, to be done once during the year, are similar to those from the Cycle 11 program 9597. The images will provide a backup database in the event of complete failure of the visflat lamp as well as allow monitoring of the gain ratios. The sweep is a complete set of internal flats, cycling through both shutter blades and both gains. The linearity test consists of a series of intflats in F555W, in each gain and each shutter. As in Cycle 11, we plan to continue to take extra visflat, intflat, and earthflat exposures to test the repeatability of filter wheel motions. WFPC2 10069 WFPC2 CYCLE 12 Supplemental Darks, Part 1/3 This dark calibration program obtains 3 dark frames every day to provide data for monitoring and characterizing the evolution of hot pixels. 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 coronographic monitoring is required to assess the changing position of the spots. ACS/HRC/WFC 10042 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. STIS/CCD 10019 CCD Bias Monitor - Part 1 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 10017 CCD Dark Monitor-Part 1 Monitor the darks for the STIS CCD. ACS/HRC/WFC 10001 Locating Ultraluminous X-Ray Sources We propose to observe ultraluminous X-ray sources which are located near objects bright both in the X-rays and the optical using Chandra and HST. The presence of these reference objects will allow us to tie the x-ray and optical references frames and achieve 0.1-0.2 arcsecond relative position accuracy in searching for optical counterparts to the ultraluminous x-ray sources. This will be a significant improvement over the accuracy previously obtained for most ULXs {limited by Chandra's absolute astrometry} and will should permit identification of individual counterparts. STIS/CCD 10000 STIS Pure Parallel Imaging Program: Cycle 12 This is the default archival pure parallel program for STIS during cycle 12. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) HSTAR 9209: GS Reacquisition (1,2,2) @ 315/13:02Z required two attempts to achieve FL-DV on FGS 2.In GS Reacquisition that began @ 315/13:56Z due to SSLE on FGS 2 during the first attempt. As it was a GS Reacquisition and the second attempt was successful, there should not have been any science impact due to this anomaly. This anomaly was uncovered by OTA SE review of PTAS processing log from SA314N SMS TC run. Under investigation. HSTAR 9210: After successful GS Acquisition (1,2,1) @ 319/18:45Z and GS Reacquisition @ 319/20:22Z, this GS pair required two attempts to get to FL-DV in the GS Reacquisition that began @ 319/21:58Z due to SSLE on FGS 2 during the first attempt. As it was a GS Reacquisition and the seconds attempt was successful, there should not have been any science impact due to this anomaly. This anomaly was uncovered by OTA SE review of PTAS processing log from SA314N SMS TC run. Under investigation. HSTAR 9214 GSACQ(2,1,1) fine lock backup, scan step limit exceeded on FGS2. GSACQ(2,1,1) at 324/09:40:49 ended in fine lock backup on FGS 2 due to scan step limit exceeded on FGS 2 at 09:44:25. REACQ at 11:01:55 also ended in fine lock backup. Observations affected: ACS 196 to 212, NICMOS 57 to 58, STIS 71 to 73, WFPC 137 to 150. The guide star acquisition for this observation was non-nominal, further analysis will determine if a repeat observation is required. COMPLETED OPS REQs: None OPS NOTES EXECUTED: None SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 14 14 FGS REacq 17 17 FHST Update 35 35 LOSS of LOCK SIGNIFICANT EVENTS: Beta Testing with CCSPSS Release 3.3 scheduled 323/12:00Z - 17:00Z with GDOC, SOC, and HITT using CCS "C" String (Test Mode) with CCS Release 4.0.3 and PRD S07200. HST Project Interface Test to verify DSN Desktops (1 Mbps) scheduled 323/13:00Z - 19:30Z with HST STOCC, JPL, GDOC, DSS 046, NISN, and SOC using CCS "B" String (GSTND Test Mode) with CCS Release 4.0.3 and PRD O06300T. The purpose of this testing is to verify the DSS 046 (Canberra) Desktop upgrades for 1 Mbps data. |
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