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 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 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<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.

    1.28 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.

/CAW