HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3148<br /><br />PERIOD COVERED: DOY 179-181<br /><br />OBSERVATIONS SCHEDULED [see HSTARS below for possible observation problems]<br /><br />ACS 9565<br /><br />ACS Post-SMOV UV Contamination Monitor<br /><br />This programme continues the UV sensitivity monitoring campaign {ACS SMOV<br />proposal 9010} of the HRC and SBC after the end of the SMOV period.<br /><br />ACS 9301<br /><br />PHOTOMETRY AND GRISM SPECTROSCOPY IN HDF NORTH/SOUTH<br /><br />Take deep ACS images and grism exposures of fields with very deep infrared<br />imaging data. The combined optical - infrared data and grisms will be uniquely<br />suited to study galaxies at high redshift: very high redshift galaxies from the<br />grism data, and internally red galaxies from the combined optical - IR imaging.<br />The comparison of the grism redshifts with ground based spectroscopy will enable<br />an evaluation of the effectiveness of the grism for redshift studies. The 3<br />fields of interest for this study are: 1} HDF North, 2} HDF South, 3} MS1054-03.<br /><br />ACS/CAL 9558<br /><br />ACS weekly Test<br /><br />This program consists of basic tests to monitor, the read noise, the 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/WFC 9442<br /><br />Optical Counterparts for Low-Luminosity X-ray Sources in Omega Centauri<br /><br />We propose to use narrow-band HAlpha imaging with ACS to search for the optical<br />counterparts of low-luminosity X-ray sources {Lx ~ 2 x 10^30 - 5 x 10^32 erg/s}<br />in the globular cluster Omega Centauri. With 9 WFC fields, we will cover the<br />inner two core radii of the cluster, and encompass about 90 of the faint sources<br />we have identified with Chandra. Approximately 30-50 of these sources should be<br />cluster members, the remainder being mostly background galaxies plus a smaller<br />number of foreground stars. This large population of low-Lx cluster X-ray<br />sources is second only to the more than 100 faint sources recently discovered in<br />47 Tuc with Chandra {Grindlay et al. 2001a}, which have been identified as a<br />mixture of cataclysmic variables, quiescent low-mass X-ray binaries, millisecond<br />pulsars, and coronally active main-sequence binaries. Our Cycle 6 WFPC2 program<br />successfully identified 2 of the 3 then-known faint X-ray sources in the core of<br />Omega Cen using H-alpha imaging. We now propose to expand the areal coverage by<br />a factor of about 18 to encompass the much larger number of sources that have<br />since been discovered with Chandra. The extreme crowding in the central regions<br />of Omega Cen requires the resolution of HST to obtain optical IDs. These<br />identifications are key to making meaningful comparisons between the populations<br />of faint X-ray sources in different clusters, in an effort to understand their<br />origins and role in cluster dynamics.<br /><br />CAL/WF2 9597<br /><br />Intflat Sweep, Visflat Sweep, and Filter Anomaly Check<br /><br />No abstract available.<br /><br />GO 9585<br /><br />Discovery of a Binary Kuiper Belt Object by HST<br /><br />We will observe 1997CQ29 at three epochs to make a first determination of its<br />orbital properties<br /><br />GTO/ACS 9290<br /><br />The Nature of Galaxies at z > 4.<br /><br />The Morphological, Photometric, and Spectroscopic Properties of Intermediate<br />Redshift Cluster.New and fundamental constraints on the evolutionary state of<br />high redshift clusters will be made by obtaining deep, multiband images {SDSS g,<br />r, i, z} over the central 1.5 Mpc regions of seven distant clusters in the range<br />0.76 < z < 1.27. In addition, slitless spectroscopy, using the WFC GRISM, will<br />be performed over the central 750 kpc region of each system galaxy.<br /><br />NICMOS 9321<br /><br />Dark current, shading profile, and read noise monitoring program<br /><br />The purpose of this proposal is to monitor the detector dark current, read<br />noise, and shading profile for all three NICMOS cameras from the onset of normal<br />NCS operations throughout the start of Cycle 11.<br /><br />NICMOS 9269<br /><br />NICMOS Parallel Thermal Background<br /><br />NICMOS Camera 3 pure parallel exposures in the F222M filter will be obtained for<br />the entire duration of SMOV to establish the stability of the HST+NCS+Instrument<br />thermal emission.<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. 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 POST-SAA<br />darks will be non-standard reference files available to users with a USEAFTER<br />date/time mark.<br /><br />STIS 9618<br /><br />STIS MAMA Dispersion Solutions<br /><br />Obtain wavecals just deep enough to constrain wavelength and spatial distortion<br />maps without overusing the calibration lamp. For the first time on orbit, data<br />will be obtained at all available central wavelengths. This information will<br />help constrain global models of STIS optical performance being developed at ECF<br />and STScI. During the observations, MSM monthly offsets will be set to zero to<br />complement observations over the past couple of cycles, which occurred at extreme<br />monthly offsets. The echelle observations at zero offset will yield dispersion<br />solutions that are directly applicable to all echelle science data obtained<br />after monthly offsets are disabled.<br /><br />STIS/CCD 9110<br /><br />A Search for Kuiper Belt Object Satellites.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to investigate whether<br />the large number of collisions thought to have taken place in the primordial<br />Kuiper belt suggest that many Kuiper belt objects {KBOs} could have suffered<br />binary-forming collisions similar to that which formed the Pluto -- Charon<br />binary. Detection of such KBO satellites would allow measurement of KBO masses,<br />would help to understand the past collisional environment of the Kuiper belt,<br />and would give a context to the otherwise unique-seeming formation of the Pluto<br />-- Charon binary.<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/CCD 9066<br /><br />Closing in on the Hydrogen Reionization Edge of the Universe.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used in parallel constrain<br />the Hydrogen reionization edge in emission that marks the transition from a<br />neutral to a fully ionized IGM at a predicted redshifts.<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 9126<br /><br />Galaxy Mass and the Fate of Luminous, Blue Compact Galaxies at z~0.6.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to obtain long-slit<br />spectra for a sample of 6 luminous, blue, compact galaxies {LBCGs} at z ~ 0.6.<br />Despite being very luminous, LBCGs have velocity widths Sigma ~ 60 kms and<br />half-light radii r_e ~ 0.5'' {or R_e ~ 3Kpc}. Small sizes and velocity widths<br />suggest LBCGs are low- mass stellar systems , while their blue colors, strong<br />emission lines and low M/L-ratios indicate they are undergoing a major<br />starburst. I f the star-forming process halts after the current burst, models<br />predict that LBCGs will fade by ~2-4 magnitudes after a few Gyrs to reach the<br />low luminosities and surface brightnesses characteristic of spheroidal galaxies.<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 />STIS/CCD 9077<br /><br />Survey of the LMC Planetary Nebulae.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to perform a snapshot<br />survey of all known LMC planetary nebulae {PNe} in order to study the<br />co-evolution of the nebulae and their central stars, and to probe the chemical<br />enrichment history of the LMC.<br /><br />STIS/CCD/MA1 8625<br /><br />The Metallicity of Gas in the Local Universe: Beyond the Milky Way.<br /><br />The Space Telescope Imaging Spectrograph [CCD and MA1] was used to obtain<br />spectra of three QSO/AGN which lie behind nearby galaxies in order to measure<br />the metallicity of the interstellar gas at the present epoch beyond the local<br />group.<br /><br />STIS/CCD/MA1/MA2 9036<br /><br />An Ultraviolet Spectroscopic Survey of Star-Forming Galaxies in the Local<br />Universe.<br /><br />The Space Telescope Imaging Spectrograph [CCD, MA1 and MA2] was used to perform<br />a comprehensive STIS ultraviolet spectroscopic survey of star-forming galaxies<br />in the local universe. The sample covers a broad range of morphologies, chemical<br />composition, and luminosity. The observations will provide spectral coverage<br />between 1200 and 3100 Angstrom, at a resolution of 100 to 200 kms and S/N of<br />about 30. The data set will allow the proposers to document and quantify the<br />effects of massive stars on the interstellar medium and to infer implications<br />for the evolution of the host galaxies.<br /><br />WF/PC-2 9087<br /><br />Black Hole X-ray Transients and X-ray Binaries in M31.<br /><br />The WF/PC-2 was used to search for M31 for x-ray transients which had previously<br />been seen as part of the Chandra Guaranteed Time Observations {GTO} program. The<br />x-ray properties of these transient sources {spectra, variability} allow us to<br />determine whether the accreting object is a black hole or a neutron star. It is<br />proposed to determine the nature of the mass-losing star. Massive stars will<br />show little {<2 mag} change in their UV luminosities during outbursts, while<br />low-mass stars will show large {>5 mag} changes in their UV luminosities. By<br />determining the nature of the primary {accreting} and secondary stars in these<br />x-ray transients, we will have the first dataset that will allow the evolution<br />of black hole and neutron star binaries to be studied in an external galaxy.<br /><br />WF/PC-2 9258<br /><br />Observatory Focus Monitor.<br /><br />The WF/PC-2 was used to more accurately define the HST focus. The HST focus<br />drifts slowly and shows evidence of undergoing slips of a few microns at random<br />times. The rate of the WF/PC-2 monitoring program is insufficient to track<br />and/or understand OTA behavior in order to request timely and appropriate<br />Secondary Mirror corrections.<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 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 Group.<br /><br />WFPC2 9634<br /><br />POMS Test Proposal: WFII targeted parallel archive proposal<br /><br />The parallel opportunities available with WFPC2 in the neighborhood of bright<br />galaxies are treated in a slightly different way from the normal pure parallels.<br />Local Group galaxies offer the opportunity for a closer look at young stellar<br />populations. Narrow-band images in F656N can be used both to identify young<br />stars via their emission lines, and to map the gas distribution in star-forming<br />regions. Thus, the filter F656N is added to the four standard filters. Near more<br />distant galaxies, up to about 10 Mpc, we can map the population of globular<br />clusters; for this purpose, F300W is less useful, and only F450W, F606W, and<br />F814W will be used.<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 />FLIGHT OPERATIONS SUMMARY:<br /><br />HSTARS: [For details see ]http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf]<br /><br />8718 HRC CEB Clock 2 Voltage OOL 178/15:47:51z.At 178/15:47:51 the mnemonic<br /> JHCK2P5 [HRC CEB Clock 2 +5V]flagged out of limits red high EV= 5.23447 v.<br /> The red limits are L=4.8v H=5.2v . ACS was in WFC/HRC Operate. This happen<br /> during a T2 slew and we were not in a SAA. No observations were being taken<br /> during the anomaly. Under investigation.<br />8719 Nicmos Aft Truss Temp OOL 179/14:11:37z.The mnemonic NATRSTMP [Aft Truss<br /> Temp] flagged out of limit red high EV =20.3854degC at 179/14:11:37 and went<br /> back inbound at 14:11:46. It flagged out of limits again at 14:17:17, 14:18:56<br /> and 14:34:47 for about 10 seconds at 20.3854 degC The red high limits are L= -18.0<br /> degC H= 20.0275 degC. Nicmos was in operate. At 15:08:57 the mnemonic began<br /> toggling in and out of limits at the same temperature 20.3854 degC.Under<br /> investigation.<br />8720 SSR1 Thermal Limit Violation 179/16:35:22z.At 179/16:35:22, DS1T2 [SSR1 thermal<br /> monitor] flagged for 6 seconds [one sample] to 40.0698 degrees C. The yellow<br /> limits are -15 and 40 degrees C. SSR1 is in Bay 5 with the SSA transmitters<br /> which were experiencing extensive use in the previous few hours. It is also the<br /> end of a period of high sun time. Also, the violation occurred towards the end<br /> of orbit day.Under investigation.<br />8721 HRC CED ASPC 1 +5v OOL @ 180/13:58:56z.At 180/13:58:56 the mnemonic JHAS1P5<br /> [ HRC CED ASPC 1 +5v] flagged out of limit red high EV= 5.23447v and went back<br /> inbound at 13:59:55. The red limits are L=4.8 H=5.2. ACS was in WFC/HRC Obs.<br /> We were not in a SAA. Under investigation.<br />8722 C String Interface @ 180/13:27z.at 180/1327z on the DOC NT"S 1&2 both A and<br /> C string went flatline and purple on the core and backbone,contacted FOT and<br /> they went flatline only on C string Backbone and no problem on A string.At<br /> 180/1344z the Remote Patrol was gone from the DOCs console, at this point I<br /> contacted RT. George Gibson came and Arnold called back, George had me to<br /> contact Nabil, Nabil suspected a possible network problem and contacted Dan<br /> Worton. J.Guy and ST called and at 1500z Nabil and Dan Worton was here in<br /> building #23. The System C was in good condition and Nabil and Dan found<br /> INTERNAL-B Router interface to all vlans was down b23 switch had peaked at 16%.<br /> They disconnected and rebooted the b22 switch and cycled the interface on<br /> INTERNAL-B-Router and this cleared the problem. DOC was able to bring Patrol<br /> [ccm]back and logon to the docnts with no problems. The FOT was able to<br /> connect to the C string Backbone. Nabil and Dan Monitored the string and left<br /> after all looked good. Under investigation.<br /><br />COMPLETED OPS REQs:<br />16794-0 Quick Update EPS CCL ''dsctest tcl''<br />16793-0 Genslew for program 9110-slot 1<br /><br />OPS NOTES EXECUTED:<br />1016-0 Adjust Recharge Ratio Limits for high sun DOY 164-180 closed<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 21 21<br />FGS REacq 19 19<br />FHST Update 50 50<br />LOSS of LOCK None<br /><br />Operations Notes: None<br /><br />SIGNIFICANT EVENTS: None