Hubble Space Telescope Daily Report #2791 01/22/01
HUBBLE SPACE TELESCOPE
DAILY REPORT #2791
PERIOD COVERED: 0000Z (UTC) 01/19/01 – 0000Z (UTC) 01/22/01
Daily Status Report as of 022/0000Z
1.0 OBSERVATIONS SCHEDULED AND ACCOMPLISHED:
1.1 Completed Nine Sets of WF/PC-2 8827 (Cycle 9 Supplemental Darks pt2/3)
The WF/PC-2 was used to obtain three dark frames every day to provide data for monitoring and characterizing the evolution of hot pixels. The proposal completed nominally.
1.2 Completed Seven Sets of STIS/CCD 8837 (CCD Dark Monitor-Part 1)
The Space Telescope Imaging Spectrograph (CCD) was used to monitor the darks. The proposal completed with no reported problems.
1.3 Completed WF/PC-2/STIS/CCD 8573 (Newborn Planets and Brown Dwarf Companions in IC 348)
The WF/PC-2 and the Space Telescope Imaging Spectrograph (CCD) were used to search for young giant planets and brown dwarfs around ~100 low-mass stars and brown dwarfs in the nearby cluster IC 348. The observations completed with no reported problems.
1.4 Completed Seven Sets WF/PC-2 8816 (Cycle 9 UV Earthflats)
The WF/PC-2 was used to obtain sequences of Earth streak flats to improve the quality of pipeline flat fields for the WFPC2 UV filter set and in order to monitor flat field stability. There were no reported problems.
1.5 Completed Three Sets of STIS/CCD 8838 (Bias Monitor – Part 1)
The Space Telescope Imaging Spectrograph (CCD) was used to monitor the bias in the 1×1, 1×2, 2×1, and 2×2 bin settings at gain=1, and 1×1 at gain = 4, to build up high-S/N superbiases and track the evolution of hot columns. The proposal completed nominally.
1.6 Completed STIS/CCD 8673 (The Properties of Ly-Alpha Absorbers at Redshifts Between 0.9)
The Space Telescope Imaging Spectrograph (CCD) was used to obtain new Echelle resolution {10 km/ sec} spectra of three bright quasars which, when combined with archived and scheduled observations, will be used to characterize the properties of Ly-Alpha absorbers in the redshift range. The observations completed with no reports of problems.
1.7 Completed Ten Sets of WF/PC-2 8805 (POMS Test Proposal: WFII Parallel Archive Proposal Continuation)
The WF/PC-2 was used to perform a generic target version of the WFPC2 Archival Pure Parallel program. The program will be used to take parallel images of random areas of the sky, following the recommendations of the Parallels Working Group. The proposal completed with no reported problems.
1.8 Completed WF/PC-2 8598 (Snapshot Survey of Extended OIIl Lambda 5007Angstrom Emission in Seyfert Galaxies)
The WF/PC-2 was used for a snapshot survey of narrow band OIII Lambda 5007Angstrom images for a well defined sample of 88 Seyfert galaxies {29 Seyfert 1s and 59 Seyfert 2s}, 18 of which already have data in the archive, selected from a mostly isotropic property, the 60Mum flux. These data will be used: 1} to determine the origin of the misalignment between the accretion disk axis and the host galaxy plane axis, which can be due to mergers with other galaxies, or by the self induced radiation warping; 2} to compare the size and shape of the Narrow Line Regions (NLR) of Seyfert 1s and Seyfert 2s, and to study the frequency of conically shaped NLR in Seyfert galaxies, which are usually unresolved from ground-based observations; and 3} estimate the importance of shocks to the ionization of the NLR. The observations completed with no reported problems.
1.9 Completed Eight Sets of STIS/CCD 8562 (Probing the Large Scale Structure: Cosmic Shear Observations)
The Space Telescope Imaging Spectrograph (CCD) was used to probe the distortion of light bundles from distant galaxies, looking at the statistical properties of the intervening inhomogeneous {dark} matter distribution. The proposal completed nominally.
1.10 Completed STIS/CCD 8846 (Imaging Flats C9)
The Space Telescope Imaging Spectrograph (CCD) was used to investigate flat-field stability over a monthly period. The proposal completed nominally.
1.11 Completed WF/PC-2 7407 (Continuation of Temporal Monitoring of the Crab Synchrotron Nebula)
The WF/PC-2 was used to observe the synchrotron nebula surrounding the Crab pulsar that has been the subject of intensive study for decades. It is generally accepted that the structure and activity in this region are due to wave phenomena near the termination shock of the pulsar wind, observations of which hold unique promise of leading to more complete models of the pulsar and its magnetosphere. Unfortunately, this promise has not been fulfilled, largely because of the low spatial resolution and uneven temporal coverage of existing studies. Recent WF/PC-2 observations of the Crab synchrotron nebula offer new hope in this quest. These data, which reach the natural size scale defined by the Larmor radius of energetic electrons, resolve the majority of the known features in the Crab. For the first time it is possible to reliably establish the physical conditions {e.g., emissivities, equipartition fields, and pressures} of features associated with the wind and its termination shock. The observations completed as planned.
1.12 Completed Two Sets of STIS/CCD/MA1 8695 (The Nature and Distribution of O VI Absorbers in the Vicinity of Galaxies)
The Space Telescope Imaging Spectrograph (CCD and MA1) was used to study PG1259+593 with the E140M echelle mode to substantially improve the statistical base of observed O VI absorbers {including weak lines} for comparison with the cosmological models and to constrain the physical conditions and abundances in these systems and their relationships with galaxies. With these observations we will {1} measure the number of O VI absorbers per unit redshift {dN/dz} with a limiting equivalent width of W_Lambda ~25 mAngstrom , {2} examine whether the O VI absorption arises in photoionized, collisionally ionized, or multiphase gas, {3} estimate the absorber metallicities, and {4} study the dependence of the absorber properties on the proximity of luminous galaxies. The observations completed nominally.
1.13 Completed STIS/MA1 8561 (The Ionizing Flux from Star-Forming Galaxies)
The Space Telescope Imaging Spectrograph (MA1) was used to measure the meaningful upper limits on the amount of ionizing radiation from galaxies in the current epoch. The proposal completed nominally.
1.14 Completed STIS/CCD 8572 (Identifying Normal Galaxies at 1.3 < z < 2.5)
The Space Telescope Imaging Spectrograph (CCD) was used to perform studies of faint, distant galaxies. It is now possible to observe hundreds of galaxies out to z=1 and in the range 3 < z < 4.5, yet the redshift range 1 < z <3 remains largely unexplored. No problems were noted.
1.15 Completed Two Sets of WF/PC-2 8601 (A Snapshot Survey of Probable Nearby Galaxies)
The WF/PC-2 was used to continue the very successful snapshot survey in order to use the high spatial resolution of HST to determine whether selected galaxies are nearby on the basis of resolution into stars, and the magnitudes and colors of the brightest stars. There were no reported problems.
1.16 Completed STIS/CCD 8845 (Spectroscopic Flats C9)
The Space Telescope Imaging Spectrograph (CCD) was used to obtain CCD flats in the spectroscopic mode. The observations completed with no reported problems.
1.17 Completed STIS/CCD 8849 (Faint Standard Extension)
The Space Telescope Imaging Spectrograph (CCD) was used to observe fainter standard stars that are needed for the flux calibration of COS, while re-observations are required to check for variability and to improve S/N. The observations completed nominally
1.18 Completed WF/PC-2 8683 (Imaging Of Brightest Cluster Galaxies: The High End Of The Black Hole Mass Distribution)
The WF/PC-2 was used to make kinematic black hole detections in galaxies to decide whether they indicate that the mass correlates with both optical luminosity and radio power. The observation completed with no reported problems.
1.19 Completed Two Sets of STIS/CCD 8664 (Structural Measurement of Globular Clusters in M31 and NGC 5128: Stalking the Fundamental Plane)
The Space Telescope Imaging Spectrograph (CCD) was used to observe in the snapshot mode to image a wide selection of individual globular clusters in two other large galaxies {M31 and NGC 5128} for measurement of their structural parameters {r_c, c, central surface brightness}. We will use these to compute their binding energies and define the FP in these two galaxies. Comparison with the Milky Way will then give us powerful new information on just how “universal” the cluster formation process was in the early protogalaxies. The observations completed with no reported problems.
1.20 Completed FGS 8830 (Long Term Monitoring of FGS-2R in Position Mode)
FGS-2R was used to monitor the instrument’s plate scale and distortions to assure its continued reliably as a guiding FGS. The observations completed with no reported anomalies.
1.21 Completed FGS/1 8730 (The Masses of the O-type Binary 15 Monocerotis)
Fine Guidance Sensor #1 was used to investigate the O-type star 15 Mon {HD 47839} that was recently discovered to be an astrometric and spectroscopic binary with an orbital period of 25 years. It is the first known O-star system to bridge the observational gap between the period regimes normally probed by these techniques. The proposal completed nominally.
1.22 Completed Two Sets of STIS/MA1 8657 (Jovian Auroral Variability Due to the Solar Wind/Magnetosphere Interaction)
The Space Telescope Imaging Spectrograph (MA1) was used to observe Jupiter, covering nearly complete Jupiter rotations, permitting the observers to perform several known key measurements of the auroral emissions, and also to study uniquely the effects of solar wind variations on the auroral morphology. The proposal completed nominally.
1.23 Completed STIS/MA1 8843 (Cycle 9 MAMA Dark Measurements)
The Space Telescope Imaging Spectrograph (MA1) was used to perform the routine monitoring of the MAMA detector dark noise. The proposal completed nominally.
1.24 Completed WF/PC-2 8581 (A Search For Low-Mass Companions To Ultracool Dwarfs)
The WF/PC-2 was used to search for very low-mass {VLM} companions to a complete sample of 120 late-M and L dwarfs, drawn mainly from the 2MASS and SDSS surveys. The primary goal is to determine the multiplicity of M < 0.1 M_odot dwarfs. In particular, we aim to identify binary systems suitable for long-term astrometric monitoring and mass measurement, and systems with cool, sub-1000K companions. The proposal completed with no reported problems.
1.25 Completed STIS/CCD 8884 (POMS Test Proposal: STIS Non-Scripted Parallel Proposal Continuation)
The Space Telescope Imaging Spectrograph (CCD) was used to take parallel images of random areas of the sky. The proposal completed nominally.
1.26 Completed STIS/CCD/MA2 8672 (Establishing the Gaseous Phases of Galaxies Following the Epoch of Star Formation)
The Space Telescope Imaging Spectrograph (CCD and MA2) was used in an ambitious program designed to: {1} establish if high ionization, metal-rich halos/coronae were in place as early as z~1, which would imply that extended, early-epoch, galactic halos result from reprocessed galactic gas and that the kinematics are mechanically driven; {2} obtain the first comparison of the relative kinematics of low and high ionization species in z~1 galaxies, covering a wide range of N{HI} environments and MgII kinematic spreads up to ~400 km/s; {3} discriminate between single-phase and multi-phase ionization, and therefore spatial, absorbing structures {eg. MgII clouds embedded in diffuse high ionization halos}; and {4} place constraints on the gas-phase metallicites in early-epoch galaxies. The observations complete with no reported problems.
1.27 Completed STIS/CCD 8663 (Survey of SMC Planetary Nebulae: Nebular and Stellar Evolution in a Low- Metallicity Environment)
The Space Telescope Imaging Spectrograph (CCD) was used to survey of SMC planetary nebulae {PNe} in order to study the co-evolution of the nebulae and their central stars, in an environment that is chemically very metal poor. We will obtain STIS imaging and medium-resolution slitless spectroscopy that will yield line fluxes and nebular morphologies in important emission lines, plus magnitudes of the central stars. From these data we will gather a harvest of information: the nebular size, morphology, ionization structure, density, and mass; and the central star temperature, luminosity, and mass. The proposal completed with no reported anomalies.
1.28 Completed WF/PC-2 8726 (Cometary Knots in Planetary Nebulae)
The WF/PC-2 was used to make second epoch observations of the Cometary Knots in NGC 2392 in order to get a better idea of just how these objects are formed by comparison of their spatial motions with that of the ambient gas. The observations completed with no reports of problems.
1.29 Completed Two Sets of STIS/CCD 8840 (Read Noise Monitor)
The Space Telescope Imaging Spectrograph (CCD) was used to measure the read noise of all the amplifiers on the STIS CCD using pairs of bias frames. Full frame and binned observations are made in both Gain 1 and Gain 4, with binning factors of 1 x 1, 1 x 2, 2 x 1 and 2 x 2. All exposures are internals. The observations completed with no reported problems.
1.30 Completed WF/PC-2 8597 (The Fueling of Active Nuclei: Why are Active Galaxies Active?)
The WF/PC-2 was used to investigate the accretion onto massive black holes that are believed to be the energy source for AGN. However, evidence for black holes in quiescent galaxies has also been reported. Why are these galaxies inactive? One possibility is that active galaxies are better at providing fuel to the nuclear region than quiescent
galaxies. Other possible fueling mechanisms such as “bars-within-bars” or nuclear spirals cannot be investigated from the ground because they are relatively small features in the ISM. The observations were completed as planned.
1.31 Completed STIS/CCD/MA2 8681 (Snapshot Survey of Variability of Narrow and Broad Associated Absorption Lines in Quasars)
The Space telescope Imaging Spectrograph (CCD and MA2) was used to investigate the variability in the strength of absorption lines in quasar spectra which is definitive proof that we are observing material that is physically associated with the quasars. This proposal will conduct a STIS snapshot survey to provide second epoch observations of 37 quasars with narrow associated or broad absorption lines {NALs and BALs}, previously observed with the FOS. At high redshift several intrinsic NALs and about two thirds of BALs are known to vary, often in accord with continuum variability. The amplitudes increase and the timescales decrease with decreasing quasar luminosity. The proposal completed nominally.
1.32 Completed WF/PC-2/STIS/CCD 8191 (The Faintest Radio Galaxies: Interacting Starbursts at z<1)
Deep WF/PC-2 imaging and Space Telescope Imaging Spectrograph (CCD) slitless spectroscopy of two of our ultra-deep VLA fields were
performed. There were no reported problems.
2.0 FLIGHT OPERATIONS SUMMARY:
2.1 Guide Star Acquisitions:
Scheduled Acquisitions: 26
Successful: 26
Scheduled Re-acquisitions: 15
Successful: 15
2.2 FHST Updates:
Scheduled: 60
Successful: 60
2.3 Operations Notes:
Using ROP SR-1A, the SSR EDAC error counter was cleared seven times.
Two TTRs were written for required re-transmits during uplinks when command dropouts occurred.
As documented in HSTAR 8051, the main bus voltage (CSFBUSV1) went out-of-limits high for one sample at 020/072949Z with a value of 32.712.
The engineering status buffer limits were adjusted at 020/1213Z, per ROP DF-18A.
The telemetry monitor for the Coarse Sun Sensor #1 temperature flagged out-of-limits low with a value of 45.0897 for one six-second telemetry sample, beginning at 021/073230Z. HSTAR 8053 was written.
ROP SR-8R was used to start autonomous engineering record at 021/1130Z and to end the function at 021/1259Z.
SI C&DH errors were reset at 022/0311Z as directed by ROP NS-5.
SSA transmitter #2 was turned on at 022/034157Z and turned off at 022/040814Z.
At 022/072606Z, HGA-1 Y-position flagged out-of-limits to 75.6186 for one sample. HSTAR 8055 was written.
3.0 SIGNIFICANT FORTHCOMING EVENTS:
Continuation of normal science observations and calibrations.
