HUBBLE SPACE TELESCOPE DAILY REPORT # 3129 PERIOD COVERED: DOY 154: 0000Z (UTC) 06/02/02 - 0000Z (UTC) 06/03/02 OBSERVATIONS SCHEDULED AND ACCOMPLISHED: STIS 8594 H-deficient condensations in PNe -- a key to discrepancies in abundance determinations Much of our knowledge of elemental abundances in our own and other galaxies rests on emission line nebulae. Our recent CNO abundance determinations for Pne using optical recombination lines {ORLs} have yielded abundances systematically higher than the `standard' values deduced from UV/optical collisionally excited lines {CELs}, with discrepancies covering a wide range from 1--20. In the extreme case of NGC 6153, multi-waveband analysis has yielded CNO and Ne abundances from ORLs which are all about a factor of ten higher than the CEL values. Temperature fluctuations and density inhomogeneities fail to explain all the available data. Instead our analysis indicates that NGC 6153 may have experienced a recent ejection of H-deficient knots, similar to those observed in the `born-again' PN Abell 30. We propose to obtain deep STIS long-slit spectra for the well-resolved H- deficient knots of A 30 and to search for such knots in NGC 6153. The data will yield the spatially resolved temperature, density and ionization structure of the knots in Abell 30, and, for the first time, accurate ORL C and O abundances for them. The results will lead to a much better understanding of the physics of such knots and their effects on abundance determinations. The observations of NGC 6153 will allow us to test if the observed central peaking of its ORL C and O abundances is a consequence of a central concentration of similar H-deficient knots. NICMOS 8790 NICMOS Post-SAA calibration - CR Persistence Part 1. 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. STIS/CCD 8902 Dark Monitor-Part 2. The Space Telescope Imaging Spectrograph (CCD) was used to monitor the darks. STIS/CCD 8904 Bias Monitor-Part 2. The Space Telescope Imaging Spectrograph (CCD) was used to monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4 in order to build up high-S/N superbiases and track the evolution of hot columns. STIS/MA1/MA2 8920 Cycle 10 MAMA Dark Measurements. The Space Telescope Imaging Spectrograph (MA1 and MA2) was used to perform the routine monitoring of the MAMA detector dark noise, and is the primary means of checking on health of the MAMA detectors systems through frequent monitoring of the background count rate. WF/PC-2 8935 Cycle 10 Standard Darks. The WF/PC-2 was used to obtain 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 8938 WFPC2 CYCLE 9 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. WF/PC-2 8939 Cycle 10 Internal Monitor. The WF/PC-2 was used to calibrate the internal monitor, to be run weekly to monitor the health of the cameras. ACS/WFC/HRC 8947 Weekly Test. The Advanced Camera for Surveys (WFC and HRC) was used to perform basic tests to monitor, the read noise, the development of hot pixels and test for any source of noise in ACS CCD detectors. This program will be executed at least once a day for the entire lifetime of ACS. FGS/1 9034 The Masses and Luminosities of Population II Stars. Fine Guidance Sensor 11R was used to observe the mass-luminosity relation {MLR} of Population II stars of which very little is currently known. With the advent of the Hipparcos Catalogue, improved distances to many spectroscopic binaries known to be Pop II systems are now available. After surveying the literature and making reasonable estimates of the secondary masses, we find 13 systems whose minimum separation should be larger than the resolution limit of FGS #1. STIS/CCD 9117 Spatially Resolved Spectroscopy of Super Star Clusters in the M82 Starbursts. The Space Telescope Imaging Spectrograph (CCD) was used to obtain spatially-resolved STIS spectroscopy of 20 clusters in M82's active starburst core and also in its ``fossil'' starburst region {of age >~ 200 Myr} as a means of tracing the history of star formation and its propagation. With the spatially-resolved spectra, the proposers will be able to study the internal structure of the clusters, evidence for internal mass segregation, their interaction with their surroundings {including M82's superwind}, and the character of the bright, diffuse non-cluster populations. NICMOS 9269 NICMOS Parallel Thermal Background NICMOS Camera 3 pure parallel exposures in the F222M filter will be obtained for the entire duration of SMOV to establish the stability of the HST+NCS+Instrument thermal emission. STIS/CCD 9317 Pure Parallel Imaging Program: Cycle 10. The Space Telescope Imaging Spectrograph (CCD) was used to perform the default archival pure parallel program for STIS during cycle 10. WF/PC-2 9318 POMS Test Proposal: WFII Parallel Archive Proposal Continuation. The WF/PC-2 was used to perform the generic target version of the WFPC2 Archival Pure Parallel program. The program was used to take parallel images of random areas of the sky, following the recommendations of the Parallels Working Group. WF/PC-2 9319 POMS Test Proposal: WFII Backup Parallel Archive Proposal II. The WF/PC-2 was used to execute a POMS test proposal, designed to simulate future scientific plans. NICMOS 9326 NICMOS Cycle 10 Early Calibration Monitor This calibration program is the early Cycle 10 NICMOS monthly monitor program. A series of flat field observations will be obtain to monitor the stability and health of the NICMOS detectors. ACS/CAL 9558 ACS weekly Test 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 9564 ACS Cycle 11: UV Earth Flats This proposal will obtain sequences of UV flats by observing the bright Earth. The HRC UV filters were chosen for modes which were not obtained in the lab. Since the UV transmission is likely to vary as a function of position on the Pol_UV filters and on the coronograph, and since this behavior is currently unconstrained by measurement, a good estimate for the missing UV flats cannot be made. Although POL_UV and CORON transmissions change little at long wavelengths, the UV transmission may change by amounts larger than can be estimated in the absence of actual UV transmission measurements ACS/WFC 9575 Default {Archival} Pure Parallel Program. The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels in POMS. FLIGHT OPERATIONS SUMMARY: HSTARs: None COMPLETED OPS REQs: None OPS NOTES EXECUTED: None SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 5 5 FGS REacq 11 11 FHST Update 10 10 LOSS of LOCK None Operations Notes: None SIGNIFICANT EVENTS: Continuation of Servicing Mission Orbital Verification and the gradual resumption of normal science observations and calibrations.