Hubble Space Telescope Daily Report #2700 5 September 2000

HUBBLE SPACE TELESCOPE

DAILY REPORT #2700

PERIOD COVERED: 0000Z (UTC) 09/01/00 – 0000Z (UTC) 09/05/00

Daily Status Report as of 249/0000Z

1.0 OBSERVATIONS SCHEDULED AND ACCOMPLISHED:

1.1 Completed STIS/CCD 8847 (Full-Field Sensitivity Monitor C9)

The Space Telescope Imaging Spectrograph (CCD) was used to measure
a photometric standard star field in Omega Cen in 50CCD mode (which will be
done every few months) to monitor CCD sensitivity over the whole field of
view. The proposal completed with no reported problems.

1.2 Completed Three 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.

1.3 Completed Twenty-One Sets of 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.

1.4 Completed Twelve 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

1.5 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.

1.6 Completed FGS/2R 8465 (Long Term Stability of FGS2R in Transfer
Scan Mode)

Fine Guidance Sensor 2R was used to determine the stability of
FGS-2R S-curves which is not certain at this time due to
desorption. Changes in S curve morphology and amplitude can potentially
render the operational calibration database for FG2r obsolete, resulting in
an unacceptable increase in guide star acquistion failures and HST pointing
errors. The data gathered from these visits will monitor the FGS2r
S-curves to allow for a predictive assessment of the validity of the FGS2r
calibrations and its expected performance as a guiding instrument. The
observations completed with no reported problems.

1.7 Completed Nineteen 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.

1.8 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 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.

1.10 Completed WF/PC-2 8122 (The Evolution Of Galaxies — Mining The
Stellar Content Of The Two Most Local Blue Compact Dwarf Galaxies)

The WF/PC-2 was used to make high spatial resolution observations
of the local, blue, compact, dwarf galaxy NGC6789 in order to study its
stellar content by obtaining a deep color-magnitude diagram. This diagram
will provide a unique laboratory for understanding the effects of starburst
feedback on the interstellar meduim. The observations were completed as
planned, and no anomalies were noted.

1.11 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.

1.12 Completed FGS 8319 (Masses and Distances of Pre-Main Sequence
Binaries)

The Fine Guidance Sensors were used to make astrometric
observations of the pre-main sequence binary star system
DF-Tau. 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.

1.13 Completed Four 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.

1.14 Completed Fourteen Sets of WF/PC-2 8445 (WF/PC-2 Cycle 8 Earth Flats)

The WF/PC-2 was used to make Cycle 8 Earth flat calibration
observations. This is to obtain sequences of earth streak flats to
construct high quality flat fields for the WF/PC-2 filter set. The
observations were executed as scheduled, and no anomalies were noted.

1.15 Completed Two Sets of 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.

1.16 Completed WF/PC-2 8167 (WF/PC-2 Imaging of a Galaxy at z = 5.34
and its Field)

The WF/PC-2 was used to make observations of the galaxy 0140+326D
which is at a distance of Z = 5.34. This galaxy was the first
spectroscopically confirmed object at Z > 5 and among the few confirmed
objects at z > 5 currently. The observations were completed as planned,
and no anomalies were reported.

1.17 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.

1.18 Completed WF/PC-2 8268 (Lensed Quasar Hosts at High Redshift)

The WF/PC-2 was used to make observations of the high redshift,
lensed quasar B0739+366. Gravitational lensing offers a novel way to
detect quasar host galaxies at z > 1 and to measure their properties. The
observations were completed as scheduled, and no anomalies were reported.

1.19 Completed Two Sets of WF/PC-2 8871 (The Merger Of The 60-Year Old
Jupiter’s White Ovals)

The WF/PC-2 was used to observe Three White Ovals (nicknamed BC,
DE, FA) formed in Jupiter’s atmosphere in 1939-1940. Two of these
anticyclones {BC and DE} merged in February 1998, generating a new large
oval. Unfortunately the phenomenon took place during the solar conjunction
so the details of the event were lost. In March 2000 a second merger
occurred. Visual and infrared observations carried out with the one-meter
planetary telescope at Pic-du-Midi Observatory {France} and with the
3.5-meter NASA Infrared Telescope Facility {Mauna Kea, Hawaii}
respectively, showed the merger of the 60-year old FA with the recently
formed BE . There were no reported problems.

1.20 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.

1.21 Completed Six 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.

1.22 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.

1.23 Completed Eight 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. There were no reported problems.

1.24 Completed FGS 8729 (Speedy Gonzales Mass Determinations: Fast
Orbiting Red Dwarf Systems)

The FGSs were used to observe five fast-orbiting red dwarf systems
to determine masses for objects near the end of the stellar main
sequence. All five systems have periods of two years or less, hence the
moniker “Speedy Gonzales” systems. In addition, all have parallaxes
placing them within 10 parsecs, so high quality masses with errors less
than 5% can be derived. The observation completed as planned.

1.25 Completed STIS/CCD 8603 (Secular Changes In The Temperatures And
Radii Of Extreme Helium Stars)

The Space Telescope Imaging Spectrograph (CCD) was used to make
observations of 15 extreme helium stars (EHEs_ which, together with IUE
data, will give a 20-year baseline of ultraviolet spectrophotometry. EHEs
are luminous stellar remnants evolving rapidly to become white
dwarfs. They represent an important stage in the evolution of at least
some low-mass stars, and are closely related to the R Coronae Borealis
variables. Models do not agree about their origin, nor about what fraction
of normal stars pass through this phase, in which the stars have been
completely stripped of their outer layers. The models do predict that EHEs
are contracting and provide rate predictions and evolutionary
lifetimes. The observations completed with no reported problems.

1.26 Completed STIC/CCD/MA1 8633 (The Physical Parameters of the
Hottest, Most Luminous Stars as a Function of Metallicity)

The Space Telescope Imaging Spectrograph (CCD and MA1) was used to
obtain higher spatial resolution data on the H Alpha line for six of our
stars for which nebular contamination is significant even with long-slit
subtraction in our ground- based data. There were no reported problems.

1.27 Completed STIS/CCD/MA2 8311 (Moderate Redshift Analogs To
Lyman-Break Galaxies?)

The Space Telescope Imaging Spectrograph (CCD and MA2) was used to
determine whether high luminosity galaxies selected using rest ultraviolet
luminosity at low-to-moderate redshift {0.2

1.28 Completed 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.

1.29 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.

1.30 Completed FGS 8468 (Calibrating FGS1R’s Interferometric Response
as a Function of Spectral Color)

The Fine Guidance Sensor (FGS1R) was used to make observations of
star BP-Tau and several other reference stars as part of calibrating
FGS1R’s interferometric response as a function of spectral color. The
purpose of this proposal is to obtain reference transfer functions through
various filters at the center positions of the field of view of the
FGS1R. The observations were executed as scheduled, and no anomalies were
noted.

1.31 Completed Two Sets of 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.

1.32 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.

1.33 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.

1.34 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.

1.35 Completed WF/PC-2 8719 (A Continuation Of A Snapshot Survey Of X-
Ray Selected Central Cluster Galaxies0

The WF/PC-2 was used to perform snapshot images of a representative
subset of the central cluster galaxies from an X-ray selected cluster
sample that would provide important constraints on the formation and
evolution of dust in cluster cores that cannot be obtained from
ground-based observations. The observations completed as planned.

1.36 Completed Two Sets of STIS/CCD/MA2 7752 (The Distribution and
Evolution of Lyman-Alpha Forest Cloud Sizes)

The Space Telescope Imaging Spectrograph (MA2) was used to make
ultraviolet observations of the quasar Q0107-025B in order to study the
distribution and evolution of the Lyman-Alpha forest cloud sizes in deep
space. These observations will establish whether the correlation with
column density is real, further constrain the size of the clouds at two
different redshift ranges, and probe cloud sizes on scales up to 1
Mpc. The observations were executed as scheduled, and no anomalies were noted.

1.37 Completed STIS/CCD/MA1 8316 (The Lyman-Alpha Absorption
Cross-Section of Nearby Galaxies)

The Space Telescope Imaging Spectrograph (CCD and MA1) was used to
study the Lyman-Alpha absorption cross-section of nearby galaxy
ISO1475+35. The high resolution of the spectra will allow us to accurately
determine the velocity of the gas, which can be compared to the systemic
velocity of the galaxy, and to the velocity field determined from 21 cm H-I
emission measurements, when available. This will enable us to determine if
or how the gas is kinematically tied to the galaxy. A wavelength
calibration image was also taken. The observations were executed as
scheduled, and no anomalies were noted.

1.38 Completed STIS/CCD 8653 (Collimation and Physical Conditions
Within the HH 30 Protostellar Jet)

The Space Telescope Imaging Spectrograph (CCD) was used to observe
the protostellar jet HH 30 through a wide slit in order to determine the
distance from the star that the jet becomes collimated, and to diagnose the
density, temperature, shock structure, and ionization within the
collimation region. There were no reported problems.

1.39 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.

1.40 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.

1.41 Completed STIS/CCD 8848 (Dispersion Solutions)

The Space Telescope Imaging Spectrograph (CCD) was used to make
wavelength dispersion solutions that will be determined on a yearly basis
as part of a long-term monitoring program, and to obtain deep engineering
wavecals for all CCD gratings at several wavelength centers. The
observations were completed nominally.

1.42 Completed STIS/CCD 7912 (STIS Parallel Archive Proposal – Nearby
Galaxies – Imaging and Spectroscopy)

The Space Telescope Imaging Spectrograph (CCD) was used to make
parallel observations of nearby galaxies. This survey will be useful to
study the star formation histories, chemical evolution, and distances to
these galaxies. These data will be placed immediately into the Hubble Data
Archive. The observations were completed as scheduled, and no problems
were reported.

1.43 Completed Two Sets of WF/PC-2 8812 (Cycle 9 Internal Monitor)

The WF/PC-2 was used to obtain routine internal monitors for WFPC2
in order to monitor the health of the cameras. A variety of internal
exposures are obtained in order to provide a monitor of the integrity of
the CCD camera electronics in both bays {gain 7 and gain 15}, a test for
quantum efficiency in the CCDs, and a monitor for possible buildup of
contaminants on the CCD windows. There were no reported problems.

1.44 Completed S/C 5582 (FOC/48 Monthly Activation (Camera Section
Only): Cycle 4)

This proposal was executed as scheduled, and no anomalies were noted.

1.45 Completed Two Sets of STIS/MA1/MA2 8426 (Cycle 8 MAMA Dark
Measurements)

The Space Telescope Imaging Spectrograph (MA1 and MA2) 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.

1.46 Completed FOC/96 7923 (FOC F/96 Turn-on)

The Faint Object Camera (f/96) was used to take an internal flat
and a dark to ensure that the 30-day limit for the FOC is not
exceeded. The observations were executed as scheduled, and no anomalies
were noted.

1.47 Completed STIS/CCD/MA2 8126 (Observations Of QSO Pairs)

The Space Telescope Imaging Spectrograph (CCD and MA2) was used to
obtain ultraviolet spectra of four QSO pairs with similar common redshift
ranges {z ~ 0.7–1} and projected linear separations gradually increasing
from ~0.5 to sim1 h^-1_100 Mpc. This is being done to: {i} to probe the
extension and structure of gaseous complexes giving rise to the formation
of LyAlpha absorption lines at intermediate redshift {z ~ 0.9}, {ii} to
investigate the transversal proximity effect of the foreground quasar along
the line of sight to the background quasar; and {iii} study the environment
in which QSOs reside and in particular the presence of gas around the
foreground quasar. The observations completed nominally.

1.48 Completed FGS-3 8783 (Orbits of Pre-Main Sequence Binaries)

FGS-3 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. In cycle 5 we began to map
the orbits of young multiple star systems in Taurus using FGS3. It is
proposed to continue to measure the orbits of the binary and triple systems
that have been determined to have the smallest angular separations with the
more capable FGS-1R. The proposal completed with no reported problems.

1.49 Completed STIS/CCD 7310 (The Interaction of Accretion Disks with
Protostellar Binaries)

The Space Telescope Imaging Spectrograph (CCD) was used to study
the interaction of the accretion disk with the protostellar binary system
UZ-Tau. This should determine how the accretion disk interacts with stars
in young binary systems and will measure the rates that mass accumulates
onto each component of the pair. The observations were executed as
scheduled, and no anomalies were noted

2.0 FLIGHT OPERATIONS SUMMARY:

2.1 Guide Star Acquisitions:

Scheduled Acquisitions: 43

Successful: 43

Scheduled Re-acquisitions: 27

Successful: 27

2.2 FHST Updates:

Scheduled: 107

Successful: 106

Per HSTAR 7835, the roll delay update scheduled for 246/084200Z
failed due to tracker #1. The following two full maneuver updates were
successful, as were following acquisitions.

2.3 Operations Notes:

Operations will be transferred to the Science Institute for the day
and swing shifts on days 249, 250 and 251.

Using ROP SR-1A, the SSR EDAC error counter was cleared eleven times.

The engineering status buffer limits were updated twice, using ROP
DF-18A.

The NSSC-1 status buffer was dumped at 246/0520Z per ROP NS-3.

There were STIS EMC retries at 246/110735Z, 248/012401Z, and at
249/052224Z. After each occurrence, the STIS flight software error counter
was reset, per ROP NS-12.

The SSR pointers were set at 246/1543Z and at 246/1954Z as directed
by ROP SR-3.

Using ROP IC-2, SSA transmitter 1 was turned on at 246/1631Z and
off at 246/1654Z.

SI C&DH errors were reset at 247/0348Z and at 247/1728Z, per ROP NS-5.

Using ROP IC-2, SSA transmitter 2 was turned on at 247/0754Z and
off at 247/0822Z.

Using ROP IC-2, SSA transmitter 1 was turned on at 247/1417Z and
off at 247/1433Z.

As directed by ROP DF-18A, the 486 engineering status buffer was
dumped and cleared at 248/1141Z.

Using ROP IC-2, SSA transmitter 2 was turned on at 248/1732Z and
off at 248/1828Z.

The ephemeris table was uplinked at 249/0010Z per ROP DF-07B.

3.0 SIGNIFICANT FORTHCOMING EVENTS:

Continuation of normal science observations and calibrations.