HUBBLE SPACE TELESCOPE DAILY REPORT # 3127 PERIOD COVERED: 0000Z (UTC) 05/29/02 - 0000Z (UTC) 05/30/02 OBSERVATIONS SCHEDULED AND ACCOMPLISHED: 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. WFPC2 8938 WFPC2 CYCLE 9 SUPPLEMENTAL DARKS pt3/3. characterizing the evolution of hot pixels. WF/PC-2 8941 Cycle 10 UV Earthflats. improve the quality of pipeline flat fields for the WFPC2 UV filter set. 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/HRC 9012 HRC Coronagraph Acquisition. The Advanced Camera for Surveys (HRC) was used to verify the abilities of the flight and ground software to perform isolated point-source acquisition onto the coronagraph occulting spots and the Fastie Finger. Successful execution of these acquisitions will also demonstrate the ability of the software to calculate the centroid of the target positions and to perform automated telescope pointing. ACS 9023 ACS SBC Image Quality Verification This activity will obtain a series of images to evaluate the point source image quality over the field of view of the ACS SBC channel, after the corrector mechanisms have been used to optimize the image focus and symmetry using the HRC channel. NGC 6681 {18.7 h, -32 deg} will be the target, as this star field has been used extensively by the STIS program for UV PSF measurement and photometry. High SNR images will be obtained in the F125LP and F150LP filters, with dithers in each axis. Images will also be obtained with the F122M filter, at lower SNR, for direct comparison with CEI specs at Lyman alpha. The field will also be observed with the HRC {F250W} to establish the relative aperture location/orientation. STIS/CCD 9066 Closing in on the Hydrogen Reionization Edge of the Universe. The Space Telescope Imaging Spectrograph (CCD) was used in parallel constrain the Hydrogen reionization edge in emission that marks the transition from a neutral to a fully ionized IGM at a predicted redshifts. ACS/WFC/HRC 9075 Cosmological Parameters from Type Ia Supernovae at High Redshift. {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. 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. STIS/FUV 9412 The Physical Parameters of the Hottest, Most Luminous Stars as a Function of Metallicity We have obtained excellent, new ground-based blue optical and HAlpha spectra of a sample of very early-type stars in the Magellanic Clouds in order to measure their physical properties, for comparison with the extensive data that exists for higher-metallicity Galactic stars. Our aim is to understand how effective temperatures depend upon metallicity {necessary in determining IMFs}, and to explore the astrophysically interesting regime of stars of extreme temperatures, masses, and luminosities. In order to do this, we need to measure the stellar wind terminal velocities for our stars, necessary to constrain the stellar models. These can only be measured with STIS/FUV on HST. In addition, we will obtain higher spatial resolution data on the HAlpha line for stars for which nebular contamination is significant in our ground-based data. We also include several R136 stars with excellent STIS/CCD data but which lack UV line measures. These new HST data will provide important information about the strengths of stellar winds at extreme luminosities and the calibration of the Wind Momentum- Luminosity Relationship at lower metallicities. This proposal was highly rated in Cycle 9, but only 4 snapshots were obtained. We have completed the analysis of these plus additional data from the archives, but need spectra of the remaining objects if we are to answer the questions we pose. 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: 8666 Fep Q channel DMT FOF queue buffer overflow" C-string @ 149/12:41z 8667 GSacq (3,2,3) results in Fine Lock Backup (3,0,3) @ 151/06:29:30z COMPLETED OPS REQs: None OPS NOTES EXECUTED: None SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 9 9 FGS REacq 10 10 FHST Update 21 21 LOSS of LOCK None Operations Notes: FOT is now in building 23 with C String Prime, Due to isolation test. SIGNIFICANT EVENTS: Continuation of Servicing Mission Orbital Verification and the gradual resumption of normal science observations and calibrations.