Hubble Space Telescope Daily Report #2821 5 March 2001
HUBBLE SPACE TELESCOPE
DAILY REPORT #2821
PERIOD COVERED: 0000Z (UTC) 03/02/01 – 0000Z (UTC) 03/05/01
Daily Status Report as of 064/0000Z
1.0 OBSERVATIONS SCHEDULED AND ACCOMPLISHED:
1.1 Completed Three Sets of 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. As detailed in HSTAR 8103, the acquisition
and re-acquisition for the third iteration of this proposal defaulted to
fine lock backup on one FGS only, possibly affecting that iteration of this
proposal. Otherwise, the proposals completed nominally.
1.2 Completed Thirteen 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. As detailed in HSTAR 8103, the acquisition
and re-acquisition for the twelfth iteration of this proposal defaulted to
fine lock backup on one FGS only, possibly affecting that iteration of this
proposal. Otherwise, the proposal completed with no further reported problems.
1.3 Completed Seven Sets of WF/PC-2 8815 (Cycle 9 Earth Flats)
The WF/PC-2 was used to monitor flatfield stability. This proposal
obtains sequences of Earth streak flats to construct high quality flat
fields for the WF/PC-2 filter set. These flat fields will allow mapping of
the OTA illumination pattern and will be used in conjunction with previous
internal and external flats to generate new pipeline superflats. See HSTAR
8100 and 2.1 for details of acquisition failure during the sixth iteration
of this proposal. Otherwise, the proposals completed nominally.
1.4 Completed Five 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. See HSTAR 8102 and 2.1 for details of acquisition failure during
the third and fourth iterations of this proposal. Otherwise, the proposals
completed nominally.
1.5 Completed Five Sets of STIS/CCD 8864 (CCD Dark Monitor-Part 2)
The Space Telescope Imaging Spectrograph (CCD) was used to monitor
the darks for the CCD. See HSTAR 8093 and 2.1 for details of acquisition
failure during the second and third iterations of this
proposal. Otherwise, the proposals completed nominally.
1.6 Completed Twenty-five 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. See HSTAR 8093 and 2.1 for details of acquisition failure
during the seventh and eighth iterations of this proposal. See HSTAR 8102
and 2.1 for details of acquisition failure during the fourteenth iteration
of this proposal. Otherwise, the proposals completed nominally.
1.7 Completed Four Sets 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.
1.8 Completed Four Sets of WF/PC-2 8604 (Stellar Populations Across the
Small Magellanic Cloud (SMC) : History and Structure)
The WF/PC-2 was used to investigate the structure and evolutionary
history of the SMC by obtaining a series of 50 three-color snapshots of
selected SMC regions. With this polling of SMC field star properties, we
will produce color-magnitude diagrams in the U, V and I bands which will
reach V~23.5 in regions too crowded to be observed accurately from the
ground. See HSTAR 8093 and 2.1 for details of acquisition failure during
the first iteration of this proposal. Otherwise, the observations
completed nominally.
1.9 Completed STIS/CCD 8865 (Bias Monitor-Part 2)
The Space Telescope Imaging Spectrograph was to be 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. See HSTAR 8094 and 2.1 for details of acquisition failure this
proposal.
1.10 Completed Three Sets of 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.
1.11 Completed WF/PC-2 9041 (Direct Imaging Of The Progenitors Of
Massive, Core-Collapse Supernovae)
The WF/PC-2 was used to continue recent surveys of star-forming
galaxies in the nearby Universe that are discovering significant numbers of
supernovae which have massive star. There were no reported problems.
1.12 Completed Three Sets of WF/PC-2 8815 (Cycle 9 Earth Flats)
The WF/PC-2 was used to monitor flatfield stability. This proposal
obtains sequences of Earth streak flats to construct high quality flat
fields for the WF/PC-2 filter set. These flat fields will allow mapping of
the OTA illumination pattern and will be used in conjunction with previous
internal and external flats to generate new pipeline superflats. The
proposal completed nominally.
1.13 Completed STIS/CCD 8596 (Environmental Pollution: The Outflow in
the Archetypal Galaxy-Quasar Pair NGC3067/3C232)
The Space Telescope Imaging Spectrograph (CCD) was used to observe
galactic-scale outflows that are now known to be a common occurrence in
star-forming galaxies, in the nearby universe and at high redshift. These
superwinds have fundamental astrophysical implications for regulating star
formation, determining the evolution of the host galaxies, disseminating
the products of stellar nucleosynthesis over large volumes, and are
probably responsible for many of the metal absorption lines seen in QSO
spectra. The observations completed with no reported problems.
1.14 Completed STIS/CCD/MA1 8606 (Determining the Nature of the
Variable Absorption in AGN: Monitoring NGC 3783 with HST And Chandra)
The Space Telescope Imaging Spectrograph (CCD and MA1) was used to
investigate Seyfert 1 galaxies, many of which show intrinsic UV absorption
lines, characterized by high moderate widths, significant outflow
velocities, and variability on time scales as small as days. Seyferts with
UV absorption also show variable X-ray “warm absorbers”, characterized by
O VII and O VIII absorption edges, which suggests a common
origin. Variability monitoring is the key to understanding the absorbers,
by providing their radial locations, densities, and evolution in
ionization, column density, velocity, and coverage of the inner active
nucleus. The proposal completed with no problems.
1.15 Completed STIS/CCD/MA1/MA2 8857 (MAMA Sensitivity and Focus
Monitor C9)
The Space Telescope Imaging Spectrograph (CCD, MA1 and MA2) was
used to monitor the sensitivity of each MAMA grating mode to detect any
change due to contamination or other causes. There were no problems.
1.16 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.
1.17 Completed Four Sets of WF/PC-2 8720 (Masses and Multiplicity of
Nearby Free- floating Methane and L Dwarfs)
The WF/PC-2 was used to observe 50 very-low-mass objects in the
solar neighborhood with spectral types of L0 and later {including several
dwarfs with Methane absorption bands in their atmospheres}. These objects
will be observed in two filter bands with the aim to identify close
companions, measure their colors, and to obtain first epoch data of the
newly discovered binaries. The observations completed nominally.
1.18 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.
1.19 Completed Two Sets of STIS/CCD 8865 (Bias Monitor-Part 2)
The Space Telescope Imaging Spectrograph 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 anomalous activity.
1.20 Completed Seven Sets of WF/PC-2 8699 (The Origin of Short-Period
Comets)
The WF/PC-2 was used to detect and characterize cometary nuclei in
order to determine the basic physical properties of a large fraction of the
population of short-period comets. By acquiring statistically significant
data, we can study the origin of this family of comets and test the
hypothesis that they are collisional fragments from the Kuiper Belt
Objects. See HSTAR 8094 and 2.1 for details of acquisition failure during
the first iteration of this proposal. See HSTAR 8095 and 2.1 for details
of acquisition failure during the second iteration of this proposal. See
HSTAR 8100 and 2.1 for details of acquisition failure during the fifth
iteration of this proposal. See HSTAR 8101 and 2.1 for details of
acquisition failure during the sixth iteration of this proposal. See HSTAR
8102 and 2.1 for details of acquisition failure during the seventh
iteration of this proposal. Otherwise, the observations completed with no
further reported problems.
1.21 Completed Two Sets of STIS/MA1 8862 (FUV-MAMA Cycle 9 Flats)
The Space Telescope Imaging Spectrograph (MA1) was to be used to
obtain FUV-MAMA observations of the internal Krypton lamp to construct an
FUV flat applicable to all FUV modes. See HSTAR 8094 and 2.1 for details
of acquisition failure during the first iteration of this proposal. See
HSTAR 8100 and 2.1 for details of acquisition failure during the second
iteration of this proposal.
1.22 Completed STIS/MA2 8863 (NUV-MAMA Cycle 9 Flats)
The Space Telescope Imaging Spectrograph (MA2) was used to obtain
NUV-MAMA observations of the internal Deuterium lamp to construct an NUV
flat applicable to all NUV modes. There were no reported problems.
1.23 Completed WF/PC-2 8816 (Cycle 9 UV Earthflats)
The WF/PC-2 was to be 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. See HSTAR 8101
and 2.1 for details of acquisition failure during this proposal.
1.24 Completed FGS-1 8783 (Orbits of Pre-Main Sequence Binaries)
FGS-1 was used to dynamically measure the masses of low mass
pre-main sequence stars. This is important because there are still no low
mass young stars with reliably known masses. The proposal completed with
no reported problems.
1.25 Completed Two Sets of 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.
1.26 Completed FGS/1R 8833 (Long Term Stability of FGS1r in Transfer Mode)
Fine Guidance Sensor #1R was used to monitor the temporal stabilty
of the FGSr1 S-curves. During its first 1.5 years onboard HST FGS1r
demonstrated evolution of its S-curves, both in fringe visibility
{amplitude} and fringe morphology. By June of 1998 the fringes appeared to
have stabilized. The articulated mirror assembly, or AMA, was adjusted in
Sept. 1998 to re-optimize the instrument’s interferometric response. The
S-curves were monitored for the remainder of cycles 7 and 8. Remarkably,
no changes larger that typical “observational noise” {induced by spacecraft
jitter} have been seen in either the X or Y axis S-curves since September
1998. Until now the monitoring of FGS1r was carried out by periodically
observing the standard star UPGREN69 at the center of the FGS1r FOV in
Transfer mode with both the F583W filter and the 2/3 PUPIL stop. This
proposal marks a departure from that approach. Four standard stars of
different B-V colors from the FGS1r Transfer Mode calibration library will
be observed once each. There was no anomalous activity.
1.27 Completed FGS/ 18731 (A High Angular Resolution Survey of the Most
Massive Stars in the SMC)
Fine Guidance Sensor #1 was 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.
1.28 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.
1.29 Completed WF/PC-2 8602 (A Snapshot Survey of the Sites of Recent,
Nearby Supernovae)
The WF/PC-2 was used to conduct a snapshot survey in V and I of the
sites of the nearby SNe, which have precisely known positions, to obtain
high-resolution information on their local environment. The proposal
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 time scales decrease with
decreasing quasar luminosity. The proposal completed nominally.
1.32 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.
1.33 Completed STIS/CCD/MA1 8569 (A New Survey for Low-Redshift Damped
Lyman-Alpha Lines in QSO MgII Systems)
The Space Telescope Imaging Spectrograph (CCD and MA1) 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.
2.0 FLIGHT OPERATIONS SUMMARY:
2.1 Guide Star Acquisitions:
Scheduled Acquisitions: 42
Successful: 36
HSTAR 8093 describes an acquisition failure at 062/045820Z due to
the search radius limit being exceeded on FGS-3. The proposals outlined in
1.6 and 1.8 were affected.
Per HSTAR 8094, the acquisition at 062/121347Z failed due to FGS-3
which never went to SSM control. The proposals described in 1.9, 1.20, and
1.21 were affected.
The acquisition at 062/135009Z failed due to FGS-3-and FGS-2 when
the search radius limit was exceeded. HSTAR 8095 was written. The
proposal detailed in 1.20 was affected.
HSTAR 8100 documents an acquisition failure at 062/201505Z due to
search radius limit failures on both FGS-1 and FGS-2. Proposals outlined
in 1.3, 1.20, and 1.21 were affected.
As documented in HSTAR 8101, the acquisition at 062/215159Z failed
when the search radius was exceeded on FGSs 1 and 2. The proposals
detailed in 1.20 and 1.23 were affected.
The acquisition at 062/232822Z failed when the search radius limit
was exceeded on both FGS-1 and FGS-2. HSTAR 8102 was created. Proposals
described in 1.4, 1.5, 1.6 and 1.20 were affected.
Per HSTAR 8103, the acquisition at 063/152804Z defaulted to fine
lock back-up on FGS-3 only when a walkdown failure occurred on FGS-1. The
re-acquisition at 063/1701Z suffered the same fate. Proposals detailed in
1.1 and 1.2 may have been affected.
Scheduled Re-acquisitions: 10
Successful: 10
2.2 FHST Updates:
Scheduled: 98
Successful: 93
Per HSTAR 8096, the roll delay update at 062/165755Z failed due to
a bad star on FGS-3.
Per HSTAR 8097, the roll delay update at 062/182847Z failed due to
a bad star on FGS-3.
Per HSTAR 8098, the full maneuver updates at 062/183313Z and at
062/183558Z both failed due to a bad star on FGS-3.
Per HSTAR 8099, the roll delay update at 062/200104Z failed due to
a bad star on FGS-3.
2.3 Operations Notes:
Using ROP SR-1A, the SSR EDAC error counter was cleared nine times.
The engineering status buffer limits were adjusted twelve times per
ROP DF-18A, due mainly to the numerous FGS and FHST failures.
The high/low gyro bias table was uplinked at 061/1937Z.
Gyro #6 was powered off at 061/1947Z.
The STIS MCE-2 reset at 062/010119Z while the low voltage was on
and while outside any SAA interval. The STIS flight software error counter
was reset at 062/0105Z per ROP NS-12. MAMA-2 was recovered via normal SMS
commanding at 062.1717Z.
Per ROP NS-3, the NSSC-1 status buffer was dumped and reset at
062/0939Z.
SSA transmitter #2 was turned on at 062/1623Z and turned off at
062/1633Z. ROP IC-2 was used.
As directed by ROP IC-2, SSA transmitter #1 was turned on at
064/0429Z and turned off at 064/0444Z.
A TTR was written for negative acquisition for two TDRSS passes
beginning at 064/0640Z. It was subsequently determined that MTEs 1 and 2
had failed a temperature test, sending the HST into software safemode at
064/063856Z. Plans are currently underway for recovery.
3.0 SIGNIFICANT FORTHCOMING EVENTS:
Continuation of normal science observations and calibrations.
