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Daily 3448
HUBBLE SPACE TELESCOPE DAILY REPORT******* # 3448 PERIOD COVERED: DOY 258 OBSERVATIONS SCHEDULED ACS 9655 ACS Post-SMOV UV Contamination Monitor A standard star field {NGC6681} is observed about once a month through all the ACS broad band UV filters. NGC6681 hosts several UV spectro - photometric standard stars for which accurate spectra have been {and will continue to be} measured with STIS. The target cannot be observed for three months from mid November through to mid February, so the standard star GRW+70 will be observed twice in its stead. This program continues the UV sensitivity monitoring campaign {ACS SMOV proposal 9010} of the HRC and SBC after the end of the SMOV period. An SBC dark current measurement is taken as the last exposure of each SBC sequence. ACS 9658 ACS Earth Flats This program will obtain sequences of flat field images by observing the bright Earth. Several UV filters from the interim calibration program {9564} require additional exposures to obtain the required illumination. A few UV filters from this program will be repeated to monitor for changes in the flat fields and to verify the interim results. Since no streaks are observed in the UV, the wavelength coverage is extended to longer wavelengths in order to explore the severity of streaks in the flats from clouds in the FOV. We have added exposures for the HRC in the visible filters to verify the results derived from the L-flat campaign and to explore the severity of streaks. We have also added exposures on WFC using the minimum exposure time and using filters which will not saturate the brightest WFC pixel by more than 10 times the full well. ACS 9675 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 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. ACS/HRC 9853 A Search for Young Binary Brown Dwarfs: Constraining Formation Scenarios and Masses Through Multiplicity We propose to use the Advanced Camera for Surveys / High Resolution Camera to conduct a direct imaging multiplicity survey of 34 young brown dwarfs in the nearest regions of recent star formation, the T association Taurus-Auriga and the OB association Upper Scorpius. The determined multiplicity fraction, the separation distribution, and the mass ratio distribution will offer stringent observational constraints on proposed brown dwarf formation scenarios. Moreover, the small semi-major axes of known field and open cluster brown dwarf binaries suggest the exciting possibility of our identifying several very close binaries { 15 AU}. Continued monitoring of these systems would yield, on a decade timescale, the first dynamical mass estimates of T Tauri brown dwarfs. With masses intermediate between those of stars and planets, brown dwarfs offer our best hope of relating the reasonably well understood processes of star formation to the less well understood processes of planet formation. ACS/WFC 10056 Extreme Red Stars ACS provides unprecedented sensitivity in the far red, this coupled with recent astronomical pushes to ever cooler objects {e.g. new classifications for L and T stellar dwarfs, and extremely high redshift galaxies} increases the need for extending the photometric calibration to include such objects. We propose observations of 2 stellar objects for which STIS spectra will exist, as well as NICMOS grism. The two targets include a late M dwarf and a T dwarf. The M dwarf provides a temporal check with WFC and new constraint for the HRC. The T dwarf provides new results for the WFC. ACS/WFC 9892 H-alpha Snapshots of Nearby Galaxies observed in F300W: Quantifying Star Formation in a Dusty Universe Previous studies of nearby galaxies show large discrepancies between different star formation {SF} indicators on large {100 pc, or even global} scales: the strikingly complex interplay of young stars, dust and ionized gas are the primary cause of this variance. The few galaxies in the HST Archive with both WFPC2 H-alpha and mid-UV {F255W or F300W} imaging show this complex geometry extending down to 10 pc scales. We propose a SNAPshot survey in the ACS/WFC H-alpha filter of 48 galaxies of all Hubble types, that are nearby but beyond the Local Group, and that were previously imaged with WFPC2 in the mid-UV and in F814W. We aim to provide a benchmark for understanding the SF processes in both normal and star-bursting galaxies, at spatial resolutions unattainable from the ground for a large and varied galaxy sample. These data can be applied to a wide range of astrophysical problems and will, therefore, be made public immediately. Our science goals are to: {1} spatially resolve the dust clouds and filaments which strongly affect mid-UV and H-alpha derived SF rates, {2} test how the large-scale correlation between H-alpha and mid-UV flux breaks down on pc scales, and {3} model the propagation of star formation by comparing the SF over time scales of ~100 Myr {via mid-UV} and ~5 Myr {via H-alpha}. This will {4} significantly improve our insight into, and calibration of SF in UV-bright galaxies at high z, and into the cosmic SF history. ACS/WFC 9991 The Orbit of a Newly Discovered Transneptunian Binary We have recently discovered a binary companion to the transneptunian object {TNO} 1999 RZ253. We are requesting rapid follow up observations during cycle 12 to make observations sufficient for a preliminary characterization of the orbital period, semimajor axis, eccentricity, and inclination. In particular, it is urgent to determine if this object is a candidate for observable mutual events in the near future, a possibility that would greatly add to its scientific interest. The study of TNBs is in a stage of explosive growth, fueled in large part by the capabilities of HST that we seek to exploit. 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 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/STIS/CCD/WFPC2 9738 Spectroscopy and Polarimetry of Mars at Closest Approach We plan a coordinated program of spectroscopy, imaging, and spectropolarimetry of Mars during the August 2003 opposition to study the composition and physical state of surface materials and airborne aerosols. The observations include {a} Moderate spectral resolution 290 to 570 nm STIS long-slit push-broom imaging spectroscopy of Mars, to constrain the properties of airborne aerosol particles and to search for and globally map iron-bearing minerals that are diagnostic of specific past climatic conditions; {b} WFPC2 UV-VIS images designed primarily to quantify the effects of ice and dust aerosols on our STIS spectra; {c} NICMOS near-IR images to search for and globally map the presence of hydrated surface minerals; and {d} ACS multispectral polarizer images to provide critical phase function measurements needed to constrain the physical properties of the Martian surface layer. The observations are timed to take advantage of the closest approach of Mars to Earth for the next several hundred years. Images and spectra will be acquired at a spatial scale comparable to existing spacecraft orbital spectroscopy data {~10 km/pixel} and in wavelength regions not sampled by past or current Mars spacecraft instrumentation. These observations also provide complementary scientific and calibration measurements in support of current and future NASA and ESA Mars exploration missions. NIC2 9834 Finding Planets in the Stellar Graveyard: A Faint Companion Search of White Dwarfs with NICMOS We propose to do a deep search for substellar objects in orbit around white dwarfs with the newly refurbished NICMOS camera as part of the PI's doctoral thesis work. Direct imaging of planets around main sequence stars is difficult due to the large contrast ratio, a problem which is much less severe for companions to white dwarfs. White dwarfs are not usually considered in planet searches but recent theoretical work and observations are motivating new searches for planetary systems and dust disks around DAZ white dwarfs. We propose to conduct the search with the NIC2 coronagraph to find resolved companions and do photometry to search for unresolved companions through Near-IR excesses. We estimate that the survey will be sensitive to brown dwarfs, high mass jovian planets, and dust disks. By probing a wide range of orbital separations and companion masses, this survey will help to answer questions about the brown dwarf desert, common envelope evolution, and planet formation. HST and NICMOS provide a unique capability to do this search, as no ground based observatory with AO can adequately search for faint companions as close and with such high contrast. NICMOS 8791 NICMOS Post-SAA calibration - CR Persistence Part 2 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 9606 CCD Dark Monitor-Part 2 Monitor the darks for the STIS CCD. STIS 9608 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 9615 Cycle 11 MAMA Dark Monitor This test performs the routine monitoring of the MAMA detector dark noise. This proposal will provide the primary means of checking on health of the MAMA detectors systems through frequent monitoring of the background count rate. The purpose is to look for evidence of change in dark indicative of detector problem developing. STIS/CCD 10000 STIS Pure Parallel Imaging Program: Cycle 12 This is the default archival pure parallel program for STIS during cycle 12. STIS/MA1 9790 Separating Activity and Accretion in T Tauri Stars Due to their unique evolutionary state, the naked {non-accreting} T Tauri stars {NTTS} are the only real proxies for what the underlying magnetically active star of a classical TTS {CTTS} system looks like. Comparative analysis then allows us to separate stellar properties from accretion properties in CTTS. In addition, the late-type NTTS are excellent candidates for studying rotation-activity relationships in fully convective stars and probing the properties of turbulent dynamos. With the limited data currently available, NTTS appear to be very magnetically active stars with higher than expected H-alpha/X-ray flux ratios but lower transition region fluxes relative to other active stars. However, the data are very incomplete. We will use HST-STIS observations of transition region line fluxes on 11 fully convective NTTS to establish the level and structure of dynamo generated emission in these young stars. In principal, these far ultraviolet emission lines are sensitive diagnostics of mass accretion onto CTTS, since accretion shocks on the stellar surface should produce substantial emission measure at 10^5 - 10^6 K. However, it is imperative that we first understand the emissions from NTTS before we can use these lines to study accretion onto CTTS. 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 9595 WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt3/3 This dark calibration program obtains 3 dark frames every day to provide data for monitoring and characterizing the evolution of hot pixels. 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. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) HSTAR 9147:* FHST Full Maneuver Updates (U1,3FM) failed @ 259/02:16:57Z and 259/02:19:42Z with Error Box results showing "1 FAILED" for mnemonics QEBSTFG0 and QEBSTFG1 and "1 & 2 FAILED" for QEBSTFG2. GS Acquisition @ 259/02:31:11Z failed due to SRLE. Under investigation. HSTAR 9149:* GS Acquisition (2,1,2) @ 259/02:23:11Z failed to Gyro hold due to SRLE on FGS 2.* GS Re-acquisition @ 259/03:20Z also failed. FHST Map @ 259/02:30:43Z showed vehicle axis errors of 46.310, -78.194, and 58.524. GS Re-acquisition @ 259/04:55:00Z failed.* An ARU/PRT was uplinked and GS Re-acquisition @ 259/06:31:22Z was successful. Under investigation. COMPLETED OPS REQs: 17040-0* R/T Map @259/0520z 17041-0* ARU/PRT @259/0550z OPS NOTES EXECUTED: 1155-0* Change Limits for MAMA2 Threshold Voltage (closed) @258/1343z ************************* SCHEDULED**** SUCCESSFUL*** FAILURE TIMES FGS GSacq************* 11********************** 10************* @259/0230z (HSTAR#9149) FGS REacq************* 5************************* 3************** @259/0320 & 0454z (HSTAR#9149) FHST Update*********** 28*********************** 26************ @259/0220z (HSTAR#9147) LOSS of LOCK SIGNIFICANT EVENTS: Primary GS Acquisition failed @ 259/02:23:11Z, see HSTAR 9147 and 9149.* FHST Full Maneuver Updates (U1,3FM) @ 259/02:16:57Z and 259/02:19:42Z failed with Error Box results showing "1 FAILED" for mnemonics QEBSTFG0 and QEBSTFG1 and 1 & 3 Fail for QEBSTFG2.* Subsequent GS Acquisition @ 239/02:23Z failed due to SRLE.* FHST Map @ 259/02:30Z showed attitude errors of 46.310, -78.194, and 58.524 (V1, V2, and V3 respectively).* FOT attempted ARU/PRT generation based on Map scheduled @ 259/03:32Z, but had insufficient time to process.* A FAD and ARU/PRT generation was performed @ 259/05:15Z and uplinked @ 259/05:49:10Z. Resulting attitude allowed for a successful GS Re-acquisition @ 259/06:31Z and science activities were resumed. Battery 1 Capacity Test scheduled 259/11:24Z (OR 17035-1 with attached script. There are three opportunities to connect SA Section 1 to Diode Bus B:* 259/11:33Z, 13:09Z, and 15:01Z.* These three opportunities ensure no large trickle discharge in the orbit prior to start of capacity test.* Estimate reconfiguration to FSW 6-Battery system @ 261/14:57Z. |
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