HUBBLE SPACE TELESCOPE <br /><br />DAILY REPORT # 3138 <br /><br />PERIOD COVERED: DOY 165-167: 0000Z (UTC) 06/14/02 - 0000Z (UTC) 06/16/02 <br /><br />OBSERVATIONS SCHEDULED:(see HSTARS below for possible observation problems)<br /><br />ACS 9289 <br /><br />Low Redshift Cluster Gravitational Lensing Survey <br /><br />This proposal has two main scientific goals: to determine the dark matter<br />distribution of massive galaxy clusters, and to observe the high redshift<br />universe using these clusters as powerful cosmic telescopes. Deep, g, r, i, z<br />imaging of a sample of low-z {0.2-0.4} clusters will yield a large sample of<br />lensed background galaxies with reliable photometric redshifts. Using multiple<br />pointings with a central overlap region we will reach HDF-like depth in the<br />central, highly magnified cluster region and a shallower but wider coverage in<br />the outer cluster regions. By combining strong and weak lensing constraints with<br />the photometric redshift information it will be possible to precisely measure<br />the cluster dark matter distribution with an unprecedented combination of high<br />spatial resolution and area coverage, avoiding many of the uncertainties which<br />plague ground-based studies and yielding definitive answers about the structure<br />of massive dark matter haloes. In addition, the cosmological parameters can be<br />constrained in a largely model independent way using the multiply lensed objects<br />due to the dependence of the Einsteinng radius on the distance to the source. We<br />can also expect to detect several highly magnified dropout galaxies behind the<br />clusters in the redshift ranges 4-5 5-6 and 7-8, corresponding to a drop in the<br />flux in the g, r, and i bands relative to longer wavelength. We will obtain the<br />best information to date on the giant arcs already known in these clusters,<br />making possible detailed, pixel-by-pixel studies of their star formation rate,<br />dust distribution and structural components, including spiral arms, out to a<br />redshift of around z~2.5 in several passbands. <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/HRC 9391 <br /><br />High-Resolution Imaging of Pluto's Surface <br /><br />We will collect a series of observations with the ACS/HRC from which we will<br />derive a two-color global map of Pluto's surface. We will image Pluto at F435W<br />and F555W, wavelengths that have been extensively studied from the ground over<br />the past 50 years. The maps will provide albedos with accurate error<br />determinations down to 52 degrees South latitude. These observations will<br />provide a second epoch of HST mapping of the active surface of Pluto as it<br />continues to recede from the Sun and will provide an important context for other<br />detailed studies of Pluto. <br /><br />ACS/WFC 9575 <br /><br />Default {Archival} Pure Parallel Program. <br /><br />The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels in<br />POMS. <br /><br />ACS/WFC/HRC 8947 <br /><br />Weekly Test. <br /><br />The Advanced Camera for Surveys (WFC and HRC) was used to perform basic tests to<br />monitor, the read noise, the development of hot pixels and test for any source<br />of noise in ACS CCD detectors. This program will be executed at least once a day<br />for the entire lifetime of ACS. <br /><br />FGS/1 9169 <br /><br />An Interferometric Harvest of Double Degenerates. <br /><br />Fine Guidance Sensor #1R was used to observe the white dwarf mass and age<br />distributions that hold clues to the star formation history of our Galaxy and<br />the age of the disk. <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 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 8588 <br /><br />Gamma-Ray Bursts and their Host Environments. <br /><br />The Space Telescope Imaging Spectrograph (CCD) was used to investigate the<br />physics of gamma-ray bursts {GRBs} and the nature of their host galaxies. The<br />approach is three-pronged: 1} rapid HST ultraviolet spectroscopy and Chandra<br />imaging obtained within two days of an outburst will allow probing the physics<br />of the relativistic fireball and the nature of the ISM surrounding the GRB; 2}<br />long-term optical monitoring of the optical transient {OT} will permit testing<br />the hypothesis that GRBs are frequently highly collimated and to determine<br />whether supernovae underlie GRBs; 3} Chandra and HST observations of "dark" GRBs<br />will allow probing one of the greater mysteries surrounding GRBs, the nature of<br />the bursts without optical counterparts. <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 9136 <br /><br />T Tauri Star Coronagraphic Survey: A PMS Protoplanetary Disk Census. <br /><br />The Space Telescope Imaging Spectrograph (CCD) was used to observe pre-main<br />sequence solar-mass stars, the T Tauri stars that Millimeter and IR studies<br />suggest at least 50 percent have circumstellar disks similar to the disk from<br />which our planetary system formed. High spatial resolution, high dynamic range<br />imaging of such systems will map the spatial distribution of material around the<br />star, constraining the disk sizes and inclinations, and provide a first<br />assessment of when structure in the disk, such as cleared central zones and<br />annuli, which has been linked to planet formation, develops. <br /><br />STIS/CCD 9074 <br /><br />The Origin and Physics of Gamma-Ray Bursts. <br /><br />The Space Telescope Imaging Spectrograph (CCD) was used to make observations<br />that will provide the most stringent tests yet performed of the hypothesis that<br />GRBs are powered by the collapse of massive stars. STIS CCD spectroscopy will be<br />used to detect broad atomic features of supernovae underlying GRB optical<br />transients, at flux levels more than a factor of three fainter than SN 1998bw. <br /><br />WF/PC-2 9180 <br /><br />Gamma-ray Burst Progenitors: Probing Their Environment. <br /><br />The WF/PC-2 was used to perform a target of opportunity observation of gamma ray<br />burster (GRB), GRB-011121. GRB astronomy is a field maturing at a phenomenal<br />rate. Three important new observational and theoretical discoveries, formulated<br />over the last twelve months, allow the proposer to address new, and in many<br />cases, more sophisticated questions than could have been posed previously. These<br />developments: the discovery of X-ray lines in GRB 991216; the observation that<br />N_H as deduced from X-ray afterglow are one to two orders of magnitude larger<br />than the dust extinction inferred from optical afterglow; and the growing<br />realization that the afterglow emission may exhibit features of dust echoes,<br />appear to offer unexpected and new diagnostics that will directly inform us<br />about the progenitor, the circum-progenitor material and the immediate<br />interstellar environs. <br /><br />WF/PC-2 9319 <br /><br />POMS Test Proposal: WFII Backup Parallel Archive Proposal II. <br /><br />The WF/PC-2 was used to execute a POMS test proposal, designed to simulate<br />future scientific plans. <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 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. FLIGHT OPERATIONS<br />SUMMARY: <br /><br />HSTARS: (For details http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf) <br /><br />8700 - Scheduling Errors in Final Products: SMS168M01 @ 165/0000z <br /> Two occurrences of Forward link supports scheduled outside <br /> of Return link, one occurrence of SSAT turned on several <br /> minutes prior to SSAR service. Under investigation.<br /><br />8701 - Interface Mean Temperature OOL @ 165/1730z<br /> At 165/17:30:59 the mnemonic ICDZ5BMN flagged out of limit <br /> red high EV= -5.98429 degC. Red limits L=-46.0 H=-6.0. We were <br /> in orbit day and we were not in a SAA. The anomaly happen right <br /> after a centering slew and the start of a GSacq.Under investigation.<br /><br />8702 - EMNBF3T (Main Baffle 3 Temp) Out of Limit Low @ 166/1150z Beginning <br /> at 166/11:05:18 the mnemonic EMNBF3T (Main Baffle 3 temperature) <br /> flagged intermittently out of limit low with a value of -30.3746 <br /> degrees, limit was -30.0. An extract plot shows temperature was <br /> steadily decreasing beginning at approximately 165/23:00 and is <br /> most likely due to V1-sun angle of 178 degrees and off nominal roll <br /> angle of 101 degrees during the period from 165/20:00 to 166/09:11, <br /> followed by a V1-sun angle of 135 degrees and off nominal roll angle <br /> of 18 degrees during the period beginning at 09:11. On call OTA and <br /> TCS engineers were notified. Ops Note 1014-1 was submitted at 13:14 <br /> to lower limit to -31.0 degrees at request of TCS SE. Additional<br /> intermittent limit violations occurred from 13:20:51 to 14:03:32 <br /> with a low value of -31.1859 degrees, no further action was taken to <br /> lower limit because the temperature began to increase at 14:03:32 <br /> and is no longer violating the revised limit. Ops Note will expire <br /> at 174/00:00 after a similar period of high V1-sun angle on day 173.<br /> Under investigation.<br /><br />8703 - GSacq(2,1,2) Results in Fine Lock Backup (2,0,2) @ 166/2333z. The <br /> GSacq (2,1,2) of 166/23:33:09 showed Star Selector Cmp Er A flag on <br /> FGS2, then resulted in Fine Lock Backup using FGS# 2 (2,0,2). FGS #1 <br /> started the walkdown process but was stopped after FGS #2 reached <br /> Fine Lock first. No flags remained after the Acquisition completed a<br /> and no error message was sent to the 486 STB events record. <br /> The following Three REacqs all failed to FLBU on FGS #2 (2,0,2) as well. <br /> Under investigation.<br /><br /> ******The following science observations may have been affected: ACS 211-229 <br /> STIS 141-153 NIC 165-177 WFPC 185-194 <br /><br />8704 - GSacq(1,3,3) Failed to RGA Mode @ 168/0117z. The GSACQ(1,3,3) scheduled <br /> at 168/01:17:54 failed to RGA Mode, due to search radius limit exceeded <br /> on FGS #1. Primary FGS #1 search radius = 55 a-s. Subsequent MAP at <br /> 168/01:55:00 showed vehicle axis errors: v1= -3.244, v2= -2.424, v3= 1.704 <br /> (arcsec). This shows that this is not an attitude error. PCS_SE Dan Smith <br /> was called. REAcq's(1,3,3) at 168/ 02:54:05, 04:30:14 and 06:06:23 all <br /> failed to RGA Mode. Under investigation.<br /><br /> *****Observations affected: STIS 2 - 8, WFPCII 3 - 13, ACS 2 - 6, NIC 1 - 12 <br /><br />COMPLETED OPS REQs: <br />16789-0 - NSSC-1 Memory Dump (ROP NS-2) @ 165/1701z <br />16790-0 - FHST Map @ 168/0511z <br /><br />OPS NOTES EXECUTED: <br />1014-1 - Main Baffle 3 limit adjust @ 166/1315z <br />939-1 - NSSC-1 Load in Count Mode @ 166/2053z <br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES <br />FGS GSacq 13 12 HSTAR 8704 <br />FGS REacq 30 27 HSTAR 8704 <br />FHST Update 34 33 168/0101z <br />LOSS of LOCK None <br /><br />Operations Notes: None<br /><br />SIGNIFICANT EVENTS: <br /><br />Continuation of Servicing Mission Orbital Verification and the gradual<br />resumption of normal science observations and calibrations.