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Daily 3621
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3621 PERIOD COVERED: DOY 147 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 coronographic monitoring is required to assess the changing position of the spots. 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/HRC/WFC 9731 Kepler's Supernova Remnant: an Imaging Study of the Blast Wave - Circumstellar Medium Interaction Kepler's SNR {SN 1604 AD} is the prime example of a young Galactic SNR where the blast wave is running into the wind of the progenitor star. The interaction between the blast wave and the inhomogeneous circumstellar medium gives rise to knots, evolving on a time scale of years, that dominate the optical emission from the remnant. Also visible in the optical are fainter Balmer line filaments that exhibit a range of geometries - from normal sheet-like filaments to more diffuse clumps of emission, the latter unique to this remnant. We propose to image Kepler's SNR through several narrowband filters using ACS/WFC and WFPC2. The morphology and ionization structure of the knots will be obtained from H-alpha, [S II], and [O III] images. We will also obtain a [N II] image, which is known to be strong and spatially variable in the remnant. The proposed H-alpha images will be deep enough so that the physical scales and structure of the Balmer dominated non-radiative shocks can be investigated. Our data will be a critical part of multiwavelength studies of Kepler's SNR. They will complement Chandra and XMM X-ray data and VLA radio data, and provide a significant advance in understanding the processes of magnetic field amplification and cosmic ray acceleration in SNRs as well as the evolution and dynamics of the blast wave - circumstellar medium interaction. ACS/WFC 10002 Detailed Study of X-ray Jets from a Complete Survey We propose deep followup HST and Chandra observations of two X-ray jets, which are the X-ray brightest discovered in our Chandra survey of quasars with known radio jets. With these data, we will compare their X-ray, optical and radio morphologies. We will also obtain X-ray and optical spectral indices, and spatially resolved SEDs from the radio through the X-rays. This will allow us to determine the X-ray emission mechanism at each point in these jets, and test critical predictions made by each mechanism. We will also be able to track any changes in physical conditions {including magnetic field and bulk Lorentz factor} that are present in the observed 90 degree bends. 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 9833 T Dwarf Companions: Searching for the Coldest Brown Dwarfs Faint companions to known stars have historically led to the discovery of new classes of stellar and substellar objects. Because these discoveries are typically limited by the flux ratio of the components in the system, the intrinsically faintest companions are most effectively identified around the intrinsically faintest primaries. We propose to use NICMOS to image a sample of 22 of the coolest known {T-type} brown dwarfs in the Solar Neighborhood in order to search for fainter and cooler brown dwarf companions. The high spatial resolution of the NIC 1 detector enables us to distinguish binary systems with apparent separations greater than 0"08, or physical separations greater than 1.2 AU at the nominal distances of the objects in our sample. Furthermore, the substantial sensitivity of NICMOS imaging allows us to probe companion masses of 5-50 Jupiter masses and companion effective temperatures of 250-1300 K in a maximally efficient manner. Based on work to date, we expect that roughly 20% of the objects in our sample will be binary, and that one or two of these will likely harbor a significantly fainter secondary. Hence, we expect to find a companion cooler than any currently known brown dwarf, a potential prototype for the next spectral class. In addition, our investigation will add substantially to the sample of known binary brown dwarfs, allowing improved statistical analyses of the binary fraction, separation distribution, and mass ratio distribution of these systems, key quantities for probing brown dwarf formation. We will also identify optimal substellar systems for astrometric mass measurements, a critical check for theoretical models of brown dwarfs and extrasolar planets. 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. 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/MA1 9754 Intergalactic O VI absorption at redshift 0.004 Simulations of the formation of large-scale structure in the universe predict that at the present time a large fraction of the baryons in the intergalactic medium {IGM} is in a warm/hot phase, with T=10^5-10^7 K. The warm phase has been detected with HST in absorption through the OVI 1031.926, 1037.671 doublet at redshifts ~0.15-0.3. In a sample of 100 extra-galactic objects observed with FUSE, we find 12 detections of OVI at redshifts z=0.0008-0.004 {v=250 to 1200 km/s}. Many of these occur within 400 kpc and 50 km/s of a nearby galaxy, making it much easier to understand the relation between the OVI absorbers and galaxies. Our sample allows a comparison of the properties of nearby vs more distant OVI absorbers. However, modeling the physical conditions in the gas requires measurements of HI, OVI, CIV, NV and CIII. High velocity resolution is required to resolve the HI, CIV and NV lines in order to discriminate between collisional and photoionization. We propose to obtain improved HI data, as well as the CIV and NV measurements for two absorbers at z0.004. One appears to represent collisional ionization {Mrk 876}, while the other probably represents a case of a photoionized system {Ton S180}. Understanding the ionization of the warm IGM is essential for determining elemental abundance and the baryonic content of the gas. WFPC2 10067 WFPC2 Cycle 12 Decontaminations and Associated Observations This proposal is for the monthly WFPC2 decons. Also included are instrument monitors tied to decons: photometric stability check, focus monitor, pre- and post-decon internals {bias, intflats, kspots, & darks}, UV throughput check, VISFLAT sweep, and internal UV flat check. 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.) HSTAR 9427: GS Acquisition (2,1,2) @ 148/03:17:34Z resulted in FL backup on FGS 2 due to SSLE on FGS 1. Prior FHST FM Updates @ 148/03:12:04Z and 03:14:49Z showed good attitude error vector. FHST Map @ 148/03:25:50Z showed 3-axis (RSS) error value of ~ 8.00 arcsec. Subsequent GS Reacquisition (2,1,2) @ 148/04:02:13Z resulted in FL backup. Under investigation. COMPLETED OPS REQs: 17166-0 Off-line the +DD SPA @147/13:00z OPS NOTES EXECUTED: 1115-0 CCC IPCONFIG Connnection 147/13:08z SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 08 08 FGS REacq 08 08 FHST Update 12 12 LOSS of LOCK SIGNIFICANT EVENTS: Successfully completed EPS Reconfiguration (offline +DD SPA), 5 to 4 Strings Offline during first uplink opportunity @ 147/13:00:11Z (OR 17166 with attached IP-057 and IP-062 procedures. EPS monitored power system operations for the MOR for two orbits to verify nominal operations of TRSWCC (+DD SPA Trim Relay disconnected and commanded relay order upon Trickle Charge initiation). Batteries experienced Trickle Charge durations of 31 minutes during both the first and second orbits. EPS SE continued close monitoring of the power system performance, especially battery temperatures and pressure, to assess the effects of this change. Successfully completed second round of OBAD Data Collections, Sections J through M 147/23:52Z - 01:45Z, adding four more scheduled OBAD/Rate Control combinations to the seven collected yesterday. See Ops Request 17169 with attached OBAD Data Collection procedure. Additional OBAD data collection periods are necessary for further analysis of the process in support of future TGS efforts. OBAD data collection series scheduled as follows: 148/01:25:00 - 148/02:03:00 (HN) 148/16:02:30 - 148/16:22:00 (HN) 148/23:43:00 - 149/00:25:00 (PN) One of these periods involves a transition to PN format in order to capture FHST position and intensity data at a higher rate. All commanding relating to the OBAD data collection is on a NIB with routine spacecraft activities. See Ops Request 17169 with attached OBAD Data Collection script for details. |
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