HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3154<br /><br />PERIOD COVERED: DOY 191<br /><br />OBSERVATIONS SCHEDULED (see HSTARS below for possible observation problems)<br /><br />STIS/CCD 8902<br /><br />Dark Monitor-Part 2.<br /><br />The Space Telescope Imaging Spectrograph (CCD) was used to monitor the darks.<br /><br />STIS/CCD 8904<br /><br />Bias Monitor-Part 2.<br /><br />The Space Telescope Imaging Spectrograph (CCD) was used to monitor the bias in<br />the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4 in order<br />to build up high-S/N superbiases and track the evolution of hot columns.<br /><br />WFPC2 8938<br /><br />WFPC2 CYCLE 9 SUPPLEMENTAL DARKS pt3/3.<br /><br />This dark calibration program obtains 3 dark frames every day to provide data<br />for monitoring and characterizing the evolution of hot pixels.<br /><br />STIS 9049<br /><br />Boron in G64-12: Higher Big Bang Lithium or Signature of the Nu-Process?<br /><br />The extremely metal-poor { Fe/H ~ -3.3 } star G64-12 shows a remarkable lithium<br />{Li} abundance that is about 2 times larger than those seen in other warm<br />metal-poor stars, from which the Big Bang Li abundance is inferred. This star's<br />enhanced Li has resulted from either 1. Galactic Li enrichment from a lower Big<br />Bang value, or 2. stellar depletion from a higher Big Bang value, with<br />significant cosmological implications. We argue against two of the three<br />prominent mechanisms of Galactic Li enrichment, leaving the theoretical<br />Nu-process in Type II supernovae as the sole viable mechanism. This mechanism's<br />crisp signature is the concomitant production of copious amounts of boron {B};<br />if the Nu-process enriched the material out which G64-12 formed with the extra<br />Li observed today, then this star should also exhibit a large detectable B<br />overabundance. B in G64-12 can only be observed from space, using HST/STIS. If<br />this star's STIS-based B abundance lies above the established B-Fe trend, this<br />would be the first observational evidence for the Nu-process. But if its B<br />abundance lies near the B-Fe trend, this would provide direct evidence that<br />G64-12 is an elusive fossil of a Big Bang Li abundance about 0.3 dex above<br />currently favored values, providing consistency in standard Big Bang<br />Nucleosynthesis between Li and D {but not 4He}. EITHER RESULT would be of<br />fundamental importance to Astronomy.<br /><br />Note: 9049 maybe degraded because the Fine Guidance Sensors could only acquire<br />a single guide star at July 10, 2002 10:11<br /><br />GO 9172<br /><br />Molecular Hydrogen in the Damped LyAlpha Absorber of Q1331+170<br /><br />We wish to search for the Lyman and Werner absorption lines of molecular<br />hydrogen {rest LambdaLambda = 1104 to 911 Angstrom} associated with the<br />well-studied damped LyAlpha and 21-cm absorber at z=1.776 in Q1331+170. The rare<br />detection of C I absorption in this system make this a promising candidate for a<br />search. After detecting H_2, we plan to measure the relative population in the<br />individual rotation states. The J = 0, 1, 2, 3 states will yield the kinetic<br />temperature of the gas, while the weak J = 4 and higher states will measure {or<br />limit} the local UV radiation field and hydrogen density. The detection of C I^*<br />has been used to measure the cosmic microwave background temperature at z=1.776,<br />and test the validity of the Big Bang model. The observed population of the fine<br />structure levels of C I can be explained entirely by the expected CMB radiation,<br />with surprisingly strong limits on local sources of excitation. The H_2 spectrum<br />will enable us to check this result, by allowing us to make an independent<br />estimate of the rate of UV and collisional pumping of the C I^* levels.<br /><br />STIS/CCD 9317<br /><br />Pure Parallel Imaging Program: Cycle 10.<br /><br />The Space Telescope Imaging Spectrograph (CCD) was used to perform the default<br />archival pure parallel program for STIS during cycle 10.<br /><br />WF/PC-2 9318<br /><br />POMS Test Proposal: WFII Parallel Archive Proposal Continuation.<br /><br />The WF/PC-2 was used to perform the generic target version of the WFPC2 Archival<br />Pure Parallel program. The program was used to take parallel images of random<br />areas of the sky, following the recommendations of the Parallels Working Group.<br /><br />WFPC2 9394<br /><br />Halo Microlensing: Direct Detection of a Microlens<br /><br />The MACHO project has recently released 5.7 years of LMC microlensing data,<br />presenting 17 candidate microlensing events. These events suggest an 8-50 MACHO<br />halo and a most likely MACHO mass of 0.2-0.9 M_odot. However, nearly a decade<br />after the first reported event {Alcock et al. 1993} there still remains much<br />debate about the nature and location of the lensing matter. MACHO has also<br />obtained WFPC2 follow-up data of the microlensing source stars, to date we have<br />observed 16 candidates with HST. The WFPC2 follow-up data of MACHO event LMC-5<br />provided unexpected insight into the nature of the lens. This image revealed a<br />very red, faint object displaced by 0.134^ from the source star which may well<br />be the first direct detection of the dark matter component {lens} of a<br />microlensing event. A second epoch of WFPC2 photometry will verify the proper<br />motion of the lens and allow for a parallax measurement of its distance.<br /><br />GO 9493<br /><br />Revealing the nature of low luminosity radio-galaxies with imaging polarimetry<br /><br />HST imaging of low luminosity FR I radio-galaxies allowed us to isolate for the<br />first time their optical nuclear emission from that of the host galaxy. Fluxes<br />of these unresolved nuclear sources strongly correlate with those of the radio-<br />cores, suggesting a common non-thermal origin. The picture which emerges is that<br />these radio-galaxies differ in many fundamental aspects from the other classes<br />of AGN as they might be lacking the substantial BLR, thermal disk emission and<br />torii, usually associated to active nuclei, probably reflecting a fundamentally<br />different accretion mode. On the other hand, these results support the<br />identification of FR I as the misoriented population of BL Lac objects. It is<br />crucial at this stage to firmly establish the synchrotron origin of these<br />nuclear sources. A simple and direct test can be performed by measuring their<br />polarization. In case of synchrotron emission we expect to detect significant<br />nuclear polarization, as routinely measured in BL Lac objects, at level of 3 -<br />20 We thus propose to obtain imaging polarimetry of a sample formed by the 9<br />nearest FR I radio- galaxies.<br /><br />ACS/CAL 9558<br /><br />ACS weekly Test<br /><br />This program consists of basic tests to monitor, the read noise, the development<br />of hot pixels and test for any source of noise in ACS CCD detectors. This<br />programme will be executed once a day for the entire lifetime of ACS.<br /><br />ACS/WFC 9575<br /><br />Default {Archival} Pure Parallel Program.<br /><br />The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels in<br />POMS.<br /><br />ACS/WFC 9584<br /><br />ACS Default {Archival} Pure Parallel Program II.<br /><br />The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels.<br /><br />WFPC2 9634<br /><br />POMS Test Proposal: WFII targeted parallel archive proposal<br /><br />The parallel opportunities available with WFPC2 in the neighborhood of bright<br />galaxies are treated in a slightly different way from the normal pure parallels.<br />Local Group galaxies offer the opportunity for a closer look at young stellar<br />populations. Narrow-band images in F656N can be used both to identify young<br />stars via their emission lines, and to map the gas distribution in star-forming<br />regions. Thus, the filter F656N is added to the four standard filters. Near more<br />distant galaxies, up to about 10 Mpc, we can map the population of globular<br />clusters; for this purpose, F300W is less useful, and only F450W, F606W, and<br />F814W will be used.<br /><br />POMS 9677<br /><br />POMS Test Proposal: WFII backup parallel archive proposal<br /><br />This is a POMS test proposal designed to simulate scientific plans.<br /><br />FLIGHT OPERATIONS SUMMARY:<br /><br />HSTARS: (For details see http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf)<br /><br />8732 - GSACQ(2,3,2) FL Backup, scan step limit exceeded @ 191/1011z.GSacq(2,3,2) at<br /> 10:11:17 resulted in fine lock back-up on FGS 3 with scan step limit exceeded<br /> on FGS 2. Four subsequent REACQ's on day shift will also most likely fail.<br /> Vehicle was LOS at time of occurrence. Under investigation.<br /><br /> Note: Observations affected: WFPC 100 to 111, STIS 48 to 56, ACS 94 to 101.<br /><br />8733 - Equation Server 3 Java Processes @ 191/1105z.After recycling the equation<br /> and sky server, there were three java processes instead of two. Under<br /> investigation.<br /><br />COMPLETED OPS REQs:<br />16796-0 - SADE Command Test for DSC Design Verification<br /><br />OPS NOTES EXECUTED: None<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 4 4<br />FGS REacq 11 11<br />FHST Update 8 8<br />LOSS of LOCK None<br />Operations Notes:<br /><br />SIGNIFICANT EVENTS: FLASH REPORT: SADE COMMAND TEST FOR DSC Successful<br /><br />Commanding of the SADE fine pulses via CDI-A/B was completed at DOY 2002/192 02:42.<br />Solar Array wing motors operated as expected with very minimal vehicle disturbance<br />measured, and the subsequent roll delay update was also successful. All commands<br />were verified for DMU to SI-C&DH Cross-strap (DSC) use.