HUBBLE SPACE TELESCOPE DAILY REPORT # 3130 PERIOD COVERED: DOY 155: 0000Z (UTC) 06/03/02 - 0000Z (UTC) 06/04/02 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. 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. 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. ACS 9010 SMOV Contamination Plan. This program has two main goals: {1} manage ACS operations to minimize the risk of contamination of its optics by materials outgassed during servicing activity, and {2} initiate a program to monitor the UV sensitivity of HRC and SBC as early as possible after the service mission. ACS/WFC/HRC 9075 Cosmological Parameters from Type Ia Supernovae at High Redshift. The Advanced Camera for Surveys (WFC and HRC) was used to obtain a Hubble diagram of Type Ia supernovae {SNe Ia} that will be of long lasting value as a record of the expansion history of the universe. 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. ACS/HRC 9473 Masses and IMF Variations in Super Star Clusters We are proposing to obtain high spatial resolution images of a set of super star clusters for which we have been granted observing time to measure velocity dispersions via high- resolution ground-based optical echelle and K-band spectroscopy. The images will allow us to fit the light profiles and measure the radii of the clusters, and when combined with the velocity dispersions, will enable us to estimate the cluster masses. By comparing the mass-to-light ratios with those predicted from spectral synthesis models, we will investigate possible variations in the slope and lower mass cut-offs of the initial mass functions in these clusters. Correlations of the variations of these parameters with cluster environment may provide insight into the formation mechanisms for super star clusters. By comparing the light profiles obtained in a blue and red filter, we will also search for evidence of mass segregation in the clusters. Since these clusters are too young to have experienced dynamical mass segregation, differences in the light profiles of the clusters in the two filters could be due to processes that differentiate between high and low mass stars during the birth of the clusters and would provide further constraints on theoretical models of cluster formation. Since these clusters are far too compact to be resolved by any ground-based observations, the ACS/HRC on board HST is the only instrument capable of carrying out these observations. 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 9568 Grism/Prism Calibration A Planetary Nebula in the LMC and a Galactic White Dwarf are observed through the prism of the High Resolution Channel to measure: 1} the dispersion of the prism and its field dependence; 2} the prism throughput and its field dependence. Therefore, these measurements will be carried out at several positions on the chip including the centre and the corners of the HRC chip. The same White Dwarf is observed together with a Galactic Wolf-Rayet star through the grism of the Wide Field Channel in a number of positions complementing those already observed in SMOV. The purpose here is to better characterize the field dependence of the grism dispersion in the WFC. ACS/WFC 9575 Default {Archival} Pure Parallel Program. FLIGHT OPERATIONS SUMMARY: HSTARs: 8672 FOF Queue buffer overflow @ 149/02:44:30z 8673 GRG2_4GT out of limits briefly @ 155/21:54:41z COMPLETED OPS REQs: 16781-2 Adjust Battery Pressure Test Limits @ 155/1728z 16782-1 Patch Benchmark SOC & SOC1 and SOC2 Safing limits @ 155.1734z OPS NOTES EXECUTED: NONE SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 7 7 FGS REacq 6 6 FHST Update 15 15 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.