HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3129<br /><br />PERIOD COVERED: DOY 154: 0000Z (UTC) 06/02/02 - 0000Z (UTC) 06/03/02<br /><br />OBSERVATIONS SCHEDULED AND ACCOMPLISHED:<br /><br />STIS 8594<br /><br />H-deficient condensations in PNe -- a key to discrepancies in abundance<br />determinations<br /><br />Much of our knowledge of elemental abundances in our own and other galaxies<br />rests on emission line nebulae. Our recent CNO abundance determinations for Pne<br />using optical recombination lines {ORLs} have yielded abundances systematically<br />higher than the `standard' values deduced from UV/optical collisionally excited<br />lines {CELs}, with discrepancies covering a wide range from 1--20. In the<br />extreme case of NGC 6153, multi-waveband analysis has yielded CNO and Ne<br />abundances from ORLs which are all about a factor of ten higher than the CEL<br />values. Temperature fluctuations and density inhomogeneities fail to <br />explain all<br />the available data. Instead our analysis indicates that NGC 6153 may have<br />experienced a recent ejection of H-deficient knots, similar to those <br />observed in<br />the `born-again' PN Abell 30. We propose to obtain deep STIS long-slit spectra<br />for the well-resolved H- deficient knots of A 30 and to search for such <br />knots in<br />NGC 6153. The data will yield the spatially resolved temperature, density and<br />ionization structure of the knots in Abell 30, and, for the first time, <br />accurate<br />ORL C and O abundances for them. The results will lead to a much better<br />understanding of the physics of such knots and their effects on abundance<br />determinations. The observations of NGC 6153 will allow us to test if the<br />observed central peaking of its ORL C and O abundances is a consequence of a<br />central concentration of similar H-deficient knots.<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. <br />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 <br />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/MA1/MA2 8920<br /><br />Cycle 10 MAMA Dark Measurements.<br /><br />The Space Telescope Imaging Spectrograph (MA1 and MA2) was used to perform the<br />routine monitoring of the MAMA detector dark noise, and is the primary means of<br />checking on health of the MAMA detectors systems through frequent monitoring of<br />the background count rate.<br /><br />WF/PC-2 8935<br /><br />Cycle 10 Standard Darks.<br /><br />The WF/PC-2 was used to obtain dark frames every week in order to provide data<br />for the ongoing calibration of the CCD dark current rate, and to monitor and<br />characterize the evolution of hot pixels. Over an extended period these data<br />will also provide a monitor of radiation damage to the CCDs.<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 />WF/PC-2 8939<br /><br />Cycle 10 Internal Monitor.<br /><br />The WF/PC-2 was used to calibrate the internal monitor, to be run weekly to<br />monitor the health of the cameras.<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 <br />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 <br />a day<br />for the entire lifetime of ACS.<br /><br />FGS/1 9034<br /><br />The Masses and Luminosities of Population II Stars.<br /><br />Fine Guidance Sensor 11R was used to observe the mass-luminosity relation {MLR}<br />of Population II stars of which very little is currently known. With the advent<br />of the Hipparcos Catalogue, improved distances to many spectroscopic binaries<br />known to be Pop II systems are now available. After surveying the <br />literature and<br />making reasonable estimates of the secondary masses, we find 13 systems whose<br />minimum separation should be larger than the resolution limit of FGS #1.<br /><br />STIS/CCD 9117<br /><br />Spatially Resolved Spectroscopy of Super Star Clusters in the M82 Starbursts.<br /><br />The Space Telescope Imaging Spectrograph (CCD) was used to obtain<br />spatially-resolved STIS spectroscopy of 20 clusters in M82's active starburst<br />core and also in its ``fossil'' starburst region {of age >~ 200 Myr} as a means<br />of tracing the history of star formation and its propagation. With the<br />spatially-resolved spectra, the proposers will be able to study the internal<br />structure of the clusters, evidence for internal mass segregation, their<br />interaction with their surroundings {including M82's superwind}, and the<br />character of the bright, diffuse non-cluster populations.<br /><br />NICMOS 9269<br /><br />NICMOS Parallel Thermal Background<br /><br />NICMOS Camera 3 pure parallel exposures in the F222M filter will be <br />obtained for<br />the entire duration of SMOV to establish the stability of the <br />HST+NCS+Instrument<br />thermal emission.<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 <br />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 <br />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 9326<br /><br />NICMOS Cycle 10 Early Calibration Monitor<br /><br />This calibration program is the early Cycle 10 NICMOS monthly monitor <br />program. A<br />series of flat field observations will be obtain to monitor the stability and<br />health of the NICMOS detectors.<br /><br />ACS/CAL 9558<br /><br />ACS weekly Test<br /><br />This program consists of basic tests to monitor, the read noise, the <br />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 9564<br /><br />ACS Cycle 11: UV Earth Flats<br /><br />This proposal will obtain sequences of UV flats by observing the bright Earth.<br />The HRC UV filters were chosen for modes which were not obtained in the lab.<br />Since the UV transmission is likely to vary as a function of position on the<br />Pol_UV filters and on the coronograph, and since this behavior is currently<br />unconstrained by measurement, a good estimate for the missing UV flats <br />cannot be<br />made. Although POL_UV and CORON transmissions change little at long <br />wavelengths,<br />the UV transmission may change by amounts larger than can be estimated in the<br />absence of actual UV transmission measurements<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: None<br /><br />COMPLETED OPS REQs: None<br /><br />OPS NOTES EXECUTED: None<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 5 5<br />FGS REacq 11 11<br />FHST Update 10 10<br />LOSS of LOCK None<br /><br />Operations Notes: None<br /><br />SIGNIFICANT EVENTS:<br /><br />Continuation of Servicing Mission Orbital Verification and the gradual<br />resumption of normal science observations and calibrations.