HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3135<br /><br />PERIOD COVERED: DOY 162: 0000Z (UTC) 06/10/02 - 0000Z (UTC) 06/11/02<br /><br />OBSERVATIONS SCHEDULED AND ACCOMPLISHED:<br /><br />STIS 7764<br /><br />ACTIVITY ON THE EDGE OF CONVECTION: THE ATMOSPHERE OF CANOPUS {F0 Ib-II}<br /><br />We shall obtain STIS observations of Canopus {Alpha Car}, the nearest {96 pc}<br />supergiant star. Canopus is an early F supergiant with a extremely thin<br />convection zone, yet it shows significant X-ray emission from a very hot corona.<br />UV chromospheric and transition {TR} region emission line fluxes will be used to<br />determine the emission measure {EM} distribution and radiative losses from these<br />regions, while the nonthermal turbulent motions in the TR will be measured from<br />the emission profiles. EUVE and ASCA coronal spectroscopy are also being sought<br />and will allow the coronal temperature and EM distributions to be established.<br />In conjuction with similar data for Beta Dra {G2 Ib-IIa} we shall investigate<br />how the TR turbulent energy relates to the observed coronal energy input for<br />supergiants with differing convection zone depths.<br /><br />NICMOS 8790<br /><br />NICMOS Post-SAA calibration - CR Persistence Part 1.<br /><br />A new procedure proposed to alleviate the CR-persistence problem of NICMOS. Dark<br />frames will be obtained immediately upon exiting the SAA contour 23, and every<br />time a NICMOS exposure is scheduled within 50 minutes of coming out of the SAA.<br />The darks will be obtained in parallel in all three NICMOS Cameras. The POST-SAA<br />darks will be non-standard reference files available to users with a USEAFTER<br />date/time mark.<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 />STIS/CCD 8906<br /><br />Hot Pixel Annealing.<br /><br />The Space Telescope Imaging Spectrograph (CCD) was used to measure the<br />effectiveness of the CCD hot pixel annealing process by measuring the dark<br />current behavior before and after annealing and by searching for any window<br />contamination effects. In addition, CTE performance is examined by looking for<br />traps in a low signal level flat.<br /><br />WFPC2 8934<br /><br />WFPC2 Decontaminations and Associated Observations Pt. 3/3<br /><br />This proposal is for the monthly WFPC2 decons. Also included are instrument<br />monitors tied to decons: photometric stability check, focus monitor, pre- and<br />post-decon internals {bias, intflats, kspots, & darks}, UV throughput check,<br />VISFLAT sweep, and internal UV flat check.<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 />ACS/WFC/HRC 8947<br /><br />Weekly Test.<br /><br />The Advanced Camera for Surveys (WFC and HRC) was used to perform basic tests to<br />monitor, the read noise, the development of hot pixels and test for any source<br />of noise in ACS CCD detectors. This program will be executed at least once a day<br />for the entire lifetime of ACS.<br /><br />ACS/WFC/HRC 9075<br /><br />Cosmological Parameters from Type Ia Supernovae at High Redshift.<br /><br />The Advanced Camera for Surveys (WFC and HRC) was used to obtain a Hubble<br />diagram of Type Ia supernovae {SNe Ia} that will be of long lasting value as a<br />record of the expansion history of the universe.<br /><br />STIS/CCD 9088<br /><br />Next Generation Spectral Library of Stars.<br /><br />The Space Telescope Imaging Spectrograph (CCD) was used to produce a "Next<br />Generation'' Spectral Library of 600 stars for use in modeling the integrated<br />light of galaxies and clusters by using the low dispersion UV and optical<br />gratings of STIS. The library will be roughly equally divided among four<br />metallicities, very low {Fe/H < -1.5}, low {-1.5 < Fe/H < -0.5}, near-solar<br />{-0.5 < Fe/H < 0.1}, and super-solar {Fe/H > 0.1}, well-sampling the entire<br />HR-diagram in each bin. Such a library will surpass all extant compilations and<br />have lasting archival value, well into the Next Generation Space Telescope era.<br /><br />FGS/1 9089<br /><br />Parallaxes of Cataclysmic Variables: Understanding Their Peculiar Secondary<br />Stars.<br /><br />Peg, and YZ Cnc}, whose orbital periods span a much larger range than explored<br />in previous observations, allowing examination of how the accretion luminosity<br />and secondary star change with orbital period.<br /><br />WF/PC-2 9124<br /><br />Mid-UV SNAPSHOT Survey of Nearby Irregulars: Galaxy Structure and Evolution<br />Benchmark.<br /><br />The WF/PC-2 was used to investigate the relation between star formation and the<br />global physical characteristics of galaxies to interpret the morphologies of<br />distant galaxies in terms of their evolutionary status. Distant galaxies are<br />primarily observed in their rest frame mid-ultraviolet. They resemble nearby<br />late-type galaxies, but are they really physically similar classes of objects?<br />It is proposed to address this question through a SNAPSHOT survey in the 2<br />mid-UV filter F300W of 98 nearby late-type, irregular and peculiar galaxies.<br /><br />FGS/1 9169<br /><br />An Interferometric Harvest of Double Degenerates.<br /><br />Fine Guidance Sensor #1R was used to observe the white dwarf mass and age<br />distributions that hold clues to the star formation history of our Galaxy and<br />the age of the disk.<br /><br />FGS/1 9234<br /><br />Calibrating the Mass-Luminosity Relation at the End of the Main Sequence.<br /><br />0.2 Msun, with special emphasis on objects near the stellar/brown dwarf border.<br /><br />NICMOS 9269<br /><br />NICMOS Parallel Thermal Background<br /><br />NICMOS Camera 3 pure parallel exposures in the F222M filter will be obtained for<br />the entire duration of SMOV to establish the stability of the HST+NCS+Instrument<br />thermal emission.<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 />WF/PC-2 9319<br /><br />POMS Test Proposal: WFII Backup Parallel Archive Proposal II.<br /><br />The WF/PC-2 was used to execute a POMS test proposal, designed to simulate<br />future scientific plans.<br /><br />NICMOS 9321<br /><br />Dark current, shading profile, and read noise monitoring program<br /><br />The purpose of this proposal is to monitor the detector dark current, read<br />noise, and shading profile for all three NICMOS cameras from the onset of normal<br />NCS operations throughout the start of Cycle 11.<br /><br />ACS/HRC 9391<br /><br />High-Resolution Imaging of Pluto's Surface<br /><br />We will collect a series of observations with the ACS/HRC from which we will<br />derive a two-color global map of Pluto's surface. We will image Pluto at F435W<br />and F555W, wavelengths that have been extensively studied from the ground over<br />the past 50 years. The maps will provide albedos with accurate error<br />determinations down to 52 degrees South latitude. These observations will<br />provide a second epoch of HST mapping of the active surface of Pluto as it<br />continues to recede from the Sun and will provide an important context for other<br />detailed studies of Pluto.<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/HRC 9562<br /><br />Cycle 11 Internal Flat Field Stability.<br /><br />characterization samples of the ACS filter set. Only internal exposures using<br />the calibration lamps were required.<br /><br />ACS 9567<br /><br />SBC Dark Current<br /><br />Dark current measurements will be made for the ACS SBC once a week.<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 />FLIGHT OPERATIONS SUMMARY:<br /><br />HSTARS: (For additional details on see http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf)<br /><br />8690 Unable to Establish Connection with CCS-A Equation Server @ 163/03:00:00z<br />8691 CCS-C Unable to Save to Current Page Name @ 163/05:00:00z<br /><br />COMPLETED OPS REQs: None<br /><br />OPS NOTES EXECUTED:<br />0900-1 Command Problem<br />0900-1 Command Problem<br />0900-1 Command Problem<br />0911-0 Limit Management During WFPC2 Decontamination (M001)<br /><br />Guide Star Acquisitions:<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 9 9<br />FGS REacq 7 7<br />FHST Update 17 17<br />LOSS of LOCK None<br /><br />Operations Notes:<br />1. ESB code 103 is "Block load interrupted a block load" due to the command dropouts.<br />2. R/T operations have been conducted on CCS-A ( GUI d 3.5.0.0.68 ) since 162/1320z.<br />SIGNIFICANT EVENTS:<br /><br />Continuation of Servicing Mission Orbital Verification and the gradual<br />resumption of normal science observations and calibrations.