HUBBLE SPACE TELESCOPE DAILY REPORT # 3119 PERIOD COVERED: 0000Z (UTC) 05/17/02 - 0000Z (UTC) 05/19/02 OBSERVATIONS SCHEDULED AND ACCOMPLISHED: ACS/HFC 9560 CCD Linearity Check. The Advanced Camera for Surveys (HFC) was used to obtain several exposures with both the to delineate linearity at both low and high signal levels. This is an exploratory set of observations aimed at basic instrument characterization. It is expected that positive results in some areas may serve to enable particularly demanding science observations: negative indications could lead to the need for corrections to be developed for some signal regimes. Each gain setting can have unique linearity issues, therefore exploratory observations with gains =1, 2, 4 e-/DN will be performed. Another specific goal is to obtain data that will allow accurate photometry to be extracted for point sources that saturate the ACS/WFC 9584 ACS Default {Archival} Pure Parallel Program II. The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels. ACS/WFC 9575 Default {Archival} Pure Parallel Program. The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels in 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. GTO/ACS 9290 The Nature of Galaxies at z > 4. The Morphological, Photometric, and Spectroscopic Properties of Intermediate Redshift Cluster.New and fundamental constraints on the evolutionary state of high redshift clusters will be made by obtaining deep, multiband images {SDSS g, r, i, z} over the central 1.5 Mpc regions of seven distant clusters in the range 0.76 < z < 1.27. In addition, slitless spectroscopy, using the WFC GRISM, will be performed over the central 750 kpc region of each system galaxy. NICMOS 8993 NICMOS Imaging of NGC 1241 {the Cone nebulae} and IRAS19297-0406 The purpose of this program is to obtain images that display the panchromatic capability of HST with refurbishment of NICMOS. We will obtain images of two targets using NICMOS, and if possible, ACS as well. Images will be obtained in J and H and Paschen alpha. If ACS is unavailable images will be taken in K as well. Two targets will be imaged. The ULIRG IRAS19297-0406 will be observed under all circumstance. And one object from the list of the Cone Nebula {NGC 2264} and NGC 1241 will be observed. The latter will depend upon the result of 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 NICMOS 9316 SM3B NICMOS Early Release Observations The purpose of this program is to obtain images that display the panchromatic capability of HST with the refurbished NICMOS. We will obtain images of two targets using NICMOS. Images will be obtained in J, H, and Paschen alpha. Two targets will be imaged: 1. Eta Carinae, which will also be imaged in WFPC2 to account for its variability; and 2. the edge-on galaxy NGC4013, for which NICMOS K-band images will be also obtained, and, in addition, Hubble Heritage WFPC2 NICMOS 1/2 8985 NICMOS Internal Flats. This proposal obtains sequences of NICMOS camera 1 & 2 medium and wide band filter flat fields, plus one orbit for selected Camera 3 filters. The observations will be used to build high S/N NICMOS flat fields to enable the STIS/CCD 9110 A Search for Kuiper Belt Object Satellites. The Space Telescope Imaging Spectrograph (CCD) was used to investigate whether the large number of collisions thought to have taken place in the primordial Kuiper belt suggest that many Kuiper belt objects {KBOs} could have suffered binary-forming collisions similar to that which formed the Pluto -- Charon binary. Detection of such KBO satellites would allow measurement of KBO masses, would help to understand the past collisional environment of the Kuiper belt, and would give a context to the otherwise unique-seeming formation of the 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/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. STIS/CCD 8902 Dark Monitor-Part 2. The Space Telescope Imaging Spectrograph (CCD) was used to monitor the darks. 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. STIS/CCD 9077 Survey of the LMC Planetary Nebulae. The Space Telescope Imaging Spectrograph (CCD) was used to perform a snapshot survey of all known LMC planetary nebulae {PNe} in order to study the co-evolution of the nebulae and their central stars, and to probe the chemical STIS/CCD/MA1 8919 MAMA Sensitivity and Focus Monitor C10. The Space Telescope Imaging Spectrograph (CCD and MA1) was used to monitor the sensitivity of each MAMA grating mode to detect any change due to contamination or other causes, and also to monitor the STIS focus in a spectroscopic and an imaging mode. STIS/CCD/MA1 9067 UV Detectability of Bright Quasars in the Sloan Fields. The Space Telescope Imaging Spectrograph (CCD and MA1) was used to take MAMA spectra of approximately 30 new, bright, high-redshift quasars in each of the next three cycles. STIS/MA1 8922 FUV-MAMA Cycle 10 Flats. The Space Telescope Imaging Spectrograph (MA1) was used to obtain FUV-MAMA observations of the STIS internal Krypton lamp to construct an FUV flat applicable to all FUV modes. STIS/MA1/MA2 9151 UV Snapshot Observation of Nearby Star Forming Galaxies. The Space Telescope Imaging Spectrograph (MA1 and MA2) was used to obtain FUV and NUV images of nearby emission- line galaxies with existing star-formation rate {SFR} measurements from their HAlpha flux. Recently, the use of the UV flux as a measure of SFR has gained much popularity for estimating SFRs at different cosmic epochs. However, the SFR estimated from UV flux could be greatly biased due to dust extinction. The KPNO International Spectroscopic Survey {KISS} provides a large sample of nearby HAlpha-selected starforming galaxies for which rich optical spectra are available for measuring metallicity and dust extinction through line ratios. By observing a subset of nearby emission-line galaxies in the KISS sample with the STIS FUV and NUV MAMA, a direct comparison between UV and Halpha SFR estimates will be possible. This will allow us to understand the effect of dust extinction on UV flux for star- forming galaxies over a wide range of HAlpha luminosity, metallicity absolute magnitude, and B-V color . A rough dust extinction curve will be constructed for such objects, making it possible to test plausible dust extinction curves used in previous SFR studies of the distant universe. Also, high-resolution UV images will allow us to search for plausible local counterparts to high redshift galaxies whose rest-frame UV morphology is available from existing optical HST WF/PC-2 9043 Cepheid Distances to Early-type Galaxies. The WF/PC-2 was used to continue observations in the HST Key Project on the Extragalactic Distance Scale and the HST project on the "Calibration of Nearby Type Ia Supernovae'' that have greatly improved our knowledge of the Hubble Constant by providing a solid zero point for the Tully- Fisher {TF} relation and Type Ia Supernovae {SNIa}. However, severe inconsistencies remain for distance estimators to early-type galaxies such as surface brightness fluctuations {SBF}, the planetary nebula luminosity function {PNLF}, the fundamental plane {FP}, and the globular cluster luminosity function {GCLF}. As a result, the distance to the Virgo cluster core remains uncertain by as much as 20 determination is directly affected by a lingering 0.1 mag {5 uncertainty in the photometric calibration of the WFPC2. Resolving these issues is essential not only to firm up the extragalactic distance scale, but also to understand the mass and velocity structure of the local universe. SBF in particular is emerging as the method of choice for mapping local velocity fields to 10, 000 kms because it offers an order of magnitude less Malmquist bias than TF, and SNIa are too rare to study large scale flows effectively. This project will tighten the photometric calibration of the WFPC2, and provide a solid Cepheid WF/PC-2 8940 Cycle 10 Earth Flats. The WF/PC-2 was used to monitor flatfield stability by obtaining sequences of Earth streak flats to construct high quality flat fields for the WF/PC-2 filter set. These flat fields will allow mapping of the OTA illumination pattern and will be used in conjunction with previous internal and external flats to WF/PC-2 8933 Decontaminations and Associated Observations Pt. 2/3. The WF/PC-2 was used for the monthly decons. Also included were instrument monitors tied to decons: photometric stability check, focus monitor, pre- and post-decon internals {bias, intflats, kspots, & darks}, UV throughput check, VISFLAT sweep, and internal UV flat check. WF/PC-2 9180 Gamma-ray Burst Progenitors: Probing Their Environment. The WF/PC-2 was used to perform a target of opportunity observation of gamma ray burster (GRB), GRB-011121. GRB astronomy is a field maturing at a phenomenal rate. Three important new observational and theoretical discoveries, formulated over the last twelve months, allow the proposer to address new, and in many cases, more sophisticated questions than could have been posed previously. These developments: the discovery of X-ray lines in GRB 991216; the observation that N_H as deduced from X-ray afterglow are one to two orders of magnitude larger than the dust extinction inferred from optical afterglow; and the growing realization that the afterglow emission may exhibit features of dust echoes, appear to offer unexpected and new diagnostics that will directly inform us about the progenitor, the circum-progenitor material and the immediate 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. 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. FLIGHT OPERATIONS SUMMARY: HSTARs: 8649 - 4 Forward Links outside Return Link SMS140 8650 - A string's AppServer lost connection @ 138/1005z 8651 - Battery 5 Temperature Out-of-limits @ 138/1705z 8652 - Unnecessary Gaps in SMS Scheduled TDRS Return Services @ 139/1709z 8653 - SMS Configures HST to the Wrong LGA @ 139/1706z COMPLETED OPS REQs: 16770-0 - Adjust NICMOS PAM1 Tilts @ 137/1313z 16771-1 - Disabling of SMAC 21 @ 137/1750z 16774-0 - Clear ACS SBC MAMA HV inhibit flags @ 137/2141z OPS NOTES EXECUTED: 1004-0 - Update Pressure-Based Battery Capacity Equations @ 137/1647z SCHEDULED SUCCESSFUL FGS GSacq 22 22 FGS REacq 20 20 FHST Update 54 54 LOSS of LOCK None Operations Notes: COMMENTS: R/T OPS transferred to CCS-B string (HSTAR# 8650) @ 138/1026z R/T OPS transferred back to CCS-A string @ 138/1344z SIGNIFICANT FORTHCOMING EVENTS: Continuation of Servicing Mission Orbital Verification and the gradual resumption of normal science observations and calibrations.