Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.stsci.edu/ftp/observing/status_reports/old_reports_00/hst_status_08_28_00 Дата изменения: Mon Aug 28 15:06:05 2000 Дата индексирования: Sun Dec 23 10:16:18 2007 Кодировка: Поисковые слова: redshift survey

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 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 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 Galaxies are related to Lyman-Break galaxies at high redshift {3 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.

/CAW