Hubble Space Telescope Daily Report #2695 08/28/00
HUBBLE SPACE TELESCOPE
DAILY REPORT #2695
PERIOD COVERED: 0000Z (UTC) 08/25/00 – 0000Z (UTC) 08/28/00
Daily Status Report as of 241/0000Z
1.0 OBSERVATIONS SCHEDULED AND ACCOMPLISHED:
1.1 Completed STIS/CCD/MA1 8477 (Star Formation Knots in the Distant Galaxies)
The Space Telescope Imaging Spectrograph (CCD and MA1) was used to obtain long slit spectra in star-formation knots in NGC428. The observations completed with no reported problems.
1.2 Completed Four Sets of WF/PC-2 8826 (Cycle 9 Supplemental Darks pt 1)
The WF/PC-2 was used to perform a T dark calibration program that obtains three dark frames every day in order to provide data for monitoring and characterizing the evolution of hot pixels. There were no reported anomalies.
1.3 Completed Two Sets of STIS/CCD 8631 (Bright Quasar Close Lensing Search II)
The Space Telescope Imaging Spectrograph (CCD) was used to expand the Cycle 8 second generation HST snapshot survey of bright quasars, optimized to find lenses with component image separations < 1". The observations completed nominally.
1.4 Completed Two Sets of STIS/CCD 8640 (A Public STIS Survey of the Host Galaxies of Gamma-Ray Bursts)
The Space Telescope Imaging Spectrograph (CCD) was used to obtain high-resolution images of the fields containing gamma-ray burst with well-localized coordinates; i.e. the burst has been localized to within approximately one arcsecond. The goal of this survey is to obtain a uniform sample of images of the host galaxies of these bursts. As described in HSTAR 7819 and the previous report, the acquisition for the first iteration of this proposal failed and the take data flag remained down until the following re-acquisition. There were no further reported problems.
1.5 Completed Two Sets of WF/PC-2 8059 (POMS Test Proposal: Targeted Parallel Archive Proposal)
The WF/PC-2 was used to observe the parallel opportunities available in the neighborhood of bright galaxies are treated in a slightly different way from the normal pure parallels. Local Group galaxies offer the opportunity for a closer look at young stellar
populations. Narrow-band images in F656N can be used both to identify young stars via their emission lines, and to map the gas distribution in star-forming regions. As described in HSTAR 7819 and the previous report, the acquisition for the first iteration of this proposal failed and the take data flag remained down until the following
re-acquisition. Otherwise, the observations completed nominally.
1.6 Completed Three Sets of 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. As described in HSTAR 7819 and the previous report, the acquisition for the first iteration of this proposal failed and the take data flag remained down until the following re-acquisition. There were no further reported problems.
1.7 Completed Two Sets of WF/PC-2 8544 (POMS Test Proposal: WFII Backup Parallel Archive Proposal II)
The WF/PC-2 was used to execute a POMS test proposal that was designed to simulate scientific plans. No problems were encountered.
1.8 Completed Three Sets of STIS/CCD 8439 (Bias Monitor-Part 2 C8)
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 with no reported problems.
1.9 Completed Five Sets of STIS/CCD 8437 (Dark Monitor-Part 2 C8)
The Space Telescope Imaging Spectrograph (CCD) was used to monitor the darks. The proposal completed nominally.
1.10 Completed Two Sets of 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.
1.11 Completed Two Sets of WF/PC-2/STIS/CCD 8414 (STIS Sparse Field CTE test {Cycle 8))
Both the WF/PC-2 and the Space Telescope Imaging Spectrograph (CCD) were used to conduct CTE measurements using the "sparse field test", along both the serial and parallel axes. This program needs special commanding to provide {a} off-center MSM positionings of some slits, and {b} the ability to read out with any amplifier {A, B, C, or D}. All exposures are internals. The observations were completed as planned, and no anomalies were reported.
1.12 Completed STIS/CCD/MA1 8305 (Two Post-Common-Envelope Binaries in the Hyades Cluster)
The Space Telescope Imaging Spectrograph (CCD and MA1) was used to observe V471 Tau and HZ 9, two detached binaries that are members of the Hyades cluster and consist of hot white dwarfs with main-sequence K-M companions. They have emerged from common- envelope interactions which drastically reduced their initially wide separations. For V471 Tau used STIS to confirm and further explore the host of fascinating phenomena that we have found using GHRS in a very limited spectral range near
Lyman-Alpha. We also used STIS to obtain the first high-resolution UV spectra of HZ 9, to see to what extent the above phenomena occur in a non- magnetic system which is otherwise remarkably similar to V471 Tau, and to determine accurate component masses. The observations completed with no reported problems.
1.13 Completed STIS/CCD/MA1 8205 (UV Spectroscopy of Infalling Cometary Material in Solar-Type Pre-Main Sequence Stars)
The Space Telescope Imaging Spectrograph (CCD and MA1) was used to see whether models for the formation of the Solar System that predict that an intermediate stage in planet formation was the assembly of material in the disk into planetesimals, and that this should be a common step in the evolution of planetary systems are correct. The proposal completed with no reported problems.
1.14 Completed Seven 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. The proposal completed with no reported problems.
1.15 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.
1.16 Completed WF/PC-2 8829 (Observatory Focus Monitor)
The WF/PC-2 and the Space Telescope Imaging Spectrograph (CCD) were used to analyze the HST focus which drifts slowly and shows evidence of undergoing slips of a few microns at random times. The rate of the WFPC2 monitoring program is insufficient to track and/or understand OTA behavior in order to request timely and appropriate secondary mirror
corrections. This 14 orbit program obtains a large amount of high signal to noise focus data, sometimes in two Science Instruments at once, and will be sufficient to more accurately define the HST focus. There were no reported problems.
1.17 Completed 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.
1.18 Completed STIS/CCD/MA2 8569 (A New Survey for Low-Redshift Damped Lyman-Alpha Lines in QSO MgII Systems)
The Space Telescope Imaging Spectrograph (CCD and MA2) was used to support studies which have shown that most of the observable neutral gas mass in the Universe resides in QSO damped LyAlpha {DLA} systems. However, at low redshift , DLA can only be found by searching in the UV with HST. By boot-strapping from the MgII statistics, we will be able to further improve the determination of the low- redshift statistical properties of DLA {their incidence and cosmological mass density} and open up new opportunities for studies at low redshift. The observations completed nominally.
1.19 Completed FGS/1R 8832 (Long Term Monitoring in Position Mode)
Fine Guidance Sensor-!R was used to observe the relative positions of stars in a standard cluster at a fixed telescope pointing and orientation coordinates. The evolution of rhoA and kA were monitored and calibrated to preserve the astrometric integrity of the FGS. It is well known for our experience with FGS3, and later with FGS1r, that an FGS experiences long term evolution, presumably due to disorption of water from the instrument’s graphite epoxy composites. This manifests principally as a change in the plate scale and secondarily as a change in the
distortions. The proposal completed nominally, with no reported problems.
1.20 Completed Two Sets of STIS/CCD 8410 (STIS CCD Hot Pixel Annealing C8)
The Space Telescope Imaging Spectrograph (CCD) was used to assess the effectiveness of the CCD hot pixel annealing process by measuring the dark current behavior before and after annealing and by searching for any window contamination effects. In addition CTE performance is examined by looking for traps in a low signal level flat. The observations were completed as planned, and no anomalies were reported.
1.21 Completed STIS/MA1 8311 (Moderate Redshift Analogs To Lyman-Break Galaxies?)
The Space Telescope Imaging Spectrograph (MA2) was used to determine whether high luminosity galaxies selected using rest ultraviolet luminosity at low-to-moderate redshift {0.2<z<0.7, UV-selected Bright Galaxies are related to Lyman-Break galaxies at high redshift {3<z<5} selected by the drop-out technique. The observations completed with no reported problems.
1.22 Completed WF/PC-2 8645 (A Survey of Mid-UV Morphology of Nearby Galaxies: Galaxy Structure and Faint Galaxy)
The WF/PC-2 was used to investigate the relation between star formation and the global physical characteristics of galaxies to interpret the morphologies of distant galaxies in terms of their evolutionary status. The observations completed nominally.
1.23 Completed 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.
1.24 Completed WF/PC-2 8716 (Search For Sub-Stellar Companions To Young Brown Dwarfs In The Chamaeleon I Dark Cloud)
The WF/PC-2 was used to observe twelve very low-mass dwarfs in the Chamaeleon I dark cloud, a site of on-going star formation, all showing H-alpha emission with spectral types from M6 to M8. We propose to observe these young, very low-mass dwarfs in order to search for close, faint companions. There were no reported problems.
1.25 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 which is 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.
1.26 Completed WF/PC-2 8632 (A UV Atlas of Nearby Galaxies)
The WF/PC-2 was used to perform a snapshot survey of local galaxies at UV wavelengths with the F300W filter. The aim of the project is to build a reference UV Atlas of normal galaxies, whose optical images are well known, with the highest possible degree of information, covering all the morphological types and luminosity classes. The proposal completed normally.
1.27 Completed WF/PC-2 8701 (Multiplicity among Very-Low Mass Stars and Brown Dwarfs in Alpha Persei and the Pleiades)
The WF/PC-2 was used to observe open clusters which provide excellent hunting grounds for brown dwarf {BD} searches. The AlphaPer and Pleiades clusters are young, nearby and have low extinction. They are cosidered to be the best-suited places to study the Substellar Mass. A dozen of cool faint AlphaPer and Pleiades members have been confirmed as “bona-fide” BDs with the lithium test. By comparison with those, about 60 very good cluster BD candiates are currently known. The Pleiades SMF obtained using the most recent deep large CCD surveys indicates that BDs are quite numerous but do not make a significant contribution to the total cluster mass. The observations completed with no reported problems.
1.28 Completed FGS 8731 (A High Angular Resolution Survey of the Most Massive Stars in the SMC)
The Fine Guidance Sensors were used to conduct high angular resolution observations of some of the SMC’s hottest and most luminous objects by conducting a comprehensive survey of nearly every spectral type in the upper portion of the HR diagram. Binary or multiple star systems will be detected down to an unprecedented level, more than one order of magnitude better than possible with WFPC2. The targets selected include a representative list of normal Main Sequence O-stars and their evolved descendents, namely supergiants, hypergiants, LBVs, and WRs, many of which have been previously observed by HST’s spectrometers for purposes of cosmological calibrations. The observations completed, and no problems were reported.
1.29 Completed STIS/CCD/MA1 8305 (Two Post-Common-Envelope Binaries in the Hyades Cluster)
The Space Telescope Imaging Spectrograph (CCD and MA1) was used to observe V471 Tau and HZ 9, two detached binaries that are members of the Hyades cluster and consist of hot white dwarfs with main-sequence K-M companions. They have emerged from common- envelope interactions which drastically reduced their initially wide separations. For V471 Tau used STIS to confirm and further explore the host of fascinating phenomena that we have found using GHRS in a very limited spectral range near
Lyman-Alpha. We also used STIS to obtain the first high-resolution UV spectra of HZ 9, to see to what extent the above phenomena occur in a non- magnetic system which is otherwise remarkably similar to V471 Tau, and to determine accurate component masses. The observations completed with no reported problems.
1.30 Completed Two Sets of FGS/1 8777 (Calibrating Stellar Models with the Pleiades: Resolving the Distance Discrepancy-Cycle 9)
FGS-1 was used to measure an accurate distance to the Pleiades and to resolve the problem raised by the Hipparcos results for this cluster. The Hipparcos distance, taken at face value, indicates that solar-composition ZAMS stars are 30% fainter than previously believed. The resolution to the Hipparcos distance problem is vital for understanding all the parallaxes that have come from that mission and hence this issue is fundamental to the cosmic distance scale. In this first phase we observed several spectroscopic binary systems with 2 to 3 year orbital periods to assertain the prospects for deriving visual orbits and hence orbital parallaxes for these cluster members. The proposal completed with no reported problems.
1.31 Completed FGS 8335 (Calibrating Stellar Models with the Pleiades: Resolving the Distance Discrepancy)
The Fine Guidance Sensors were used to make astrometric observations of the stars H923 and H915 that are located in the Pleiades cluster. This is the first phase of a multi-year effort to measure true masses for low-mass dwarfs in the Pleiades and to determine an accurate distance to this fundamental cluster. The observations were completed as scheduled, and no anomalies were noted.
1.32 Completed FGS 8319 (Masses and Distances of Pre-Main Sequence Binaries)
The Fine Guidance Sensors were used to make astrometric observations of a pre-main sequence binary star system. Observations were also made of several reference stars. Our goal is to measure the masses of low mass young stars. This will enable a calibration of theoretical calculations of stellar evolution to the main sequence. The observations were completed as planned and no problems were reported.
1.33 Completed STIS/MA1 8426 (Cycle 8 MAMA Dark Measurements)
The Space Telescope Imaging Spectrograph (MA1) was used to make a routine Cycle-8 MAMA dark noise calibration measurement. This proposal will provide the primary means of checking on the health of the MAMA detectors. This is done through frequent monitoring of the background count rate. The observations were completed as planned, and no problems were reported.
1.34 Completed STIS/CCD 8155 (Highly Collimated Strings in the Nebula Around Eta Carinae – A New Phenomenon)
The Space Telescope Imaging Spectrograph (CCD) was used to observe a set of highly collimated strings in the nebula around Eta Car in order to determine their physical nature and their relation to phenomenologically similar structures in nebulae around evolved low mass stars. The observations completed with no reported anomalies.
1.35 Completed STIS/CCD 8808 (POMS Test Proposal: STIS Non-Scripted Parallel Proposal Continuation III)
The Space Telescope Imaging Spectrograph (CCD) was used to make non-scripted, parallel observations as part of a POMS test proposal. The observations completed with no anomalous activity.
2.0 FLIGHT OPERATIONS SUMMARY:
2.1 Guide Star Acquisitions:
Scheduled Acquisitions: 30
Successful: 30
Per HSTAR 7823, the acquisition at 241/065734Z defaulted to fine lock backup on FGS-2 only when the scan step limit was exceeded on FGS-3. Two proposals, each occurring during the period of the next report, may have been affected: STIS 8414 and WF/PC-2 8122.
Scheduled Re-acquisitions: 24
Successful: 24
2.2 FHST Updates:
Scheduled: 68
Successful: 66
The full maneuver updates scheduled for approximately 240/103108Z failed due to tracker 2. The following guide star acquisition was successful. HSTAR 7822 was written.
2.3 Operations Notes:
Using ROP SR-1A, the SSR EDAC error counter was cleared seven times.
The engineering status buffer limits were adjusted on five occasions as directed by ROP DF-18A.
On nine occasions, per an operations note, the SSA forward power (SSAFPWR) was transitioned from normal to high power mode.
Per HSTAR 7821, the battery 6 recharge ratio (CFSRRAT6) flagged high with a value of 1.28 (limit is 1.25) at 238/164016Z. The recharge ratio was actually higher than normal for all six batteries, and the trickle charge was not attained until late into orbit day. The parameter returned to normal range at 238/180352 (the next trickle charge).
3.0 SIGNIFICANT FORTHCOMING EVENTS:
Continuation of normal science observations and calibrations.