HUBBLE SPACE TELESCOPE

       DAILY REPORT #2976

PERIOD COVERED:  0000Z (UTC) 10/12/01 - 0000Z (UTC) 10/15/01

Daily Status Report as of 288/0000Z

1.0 OBSERVATIONS SCHEDULED AND ACCOMPLISHED:

    1.1 Completed Six Sets of STIS/CCD 8901 (Dark Monitor-Part 1)

        The Space Telescope Imaging Spectrograph (CCD) was used to monitor 
the darks.  There was no anomalous activity.

    1.2 Completed Seven Sets of WF/PC-2 8936 (Cycle 10 Supplemental Darks 
Pt1/3)

        The WF/PC-2 was used to perform a dark calibration program that 
obtains three dark frames every day to provide data for monitoring and 
characterizing the evolution of hot pixels.  As described in HSTAR 8367 and 
2.1, the acquisition for the sixth and seventh iterations of this proposal 
failed, the take data flag remained down, and observations were 
lost.  Otherwise, the proposal completed with no other reported problems.

    1.3 Completed STIS/CCD/MA2 8673 (The Properties of Ly-Alpha Absorbers 
at Redshifts Between 0.9HST)

        The Space Telescope Imaging Spectrograph (CCD and MA2) was used 
obtain new Echelle resolution spectra of three bright quasars which, when 
combined with archived and scheduled observations, will be used to 
characterize the properties of Ly-Alpha absorbers in the redshift range 
0.9<z<1.6.  There were no reported problems.

    1.4 Completed Eighteen Sets of WF/PC-2 9244 (POMS Test Proposal: WFII 
Parallel Archive Proposal Continuation)

        The WF/PC-2 was used to perform a generic target version of the 
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 described in HSTAR 8367 and 2.1, the 
acquisition for the eleventh iteration of this proposal failed, the take 
data flag remained down, and observations were lost.  Otherwise, the 
observations completed with no further anomalous activity.

    1.5 Completed WF/PC-2 9249 (POMS Test Proposal: WFII Backup Parallel 
Archive Proposal II)

        The WF/PC-2 was used to execute a POMS test proposal designed to 
simulate scientific plans.  The proposal completed with no reported problems.

    1.6 Completed STIS/CCD/MA2 9048 (Boron Constraints on Slow Mixing in 
Low Mass Stars)

        The Space Telescope Imaging Spectrograph (CCD and MA2) was used to 
observe the atomic and nuclear characteristics of the light elements Li, Be 
and B, that make their photospheric abundances ideal tracers of internal 
physical processes in stars.  Both Li and Be have been heavily utilized to 
this end since their diminished abundances are a direct result of the 
extent of internal slow mixing between surface and interior layers, as has 
been shown with ground-based data.  Boron provides a fresh and special 
probe because it survives to greater depths inside stars than does Li or 
Be, and can thus uniquely reveal the depth of mixing.  It is proposed to 
observe B in stars with very large depletions of Li and Be, i.e. stars 
which have been the most seriously affected by mixing.  No problems occurred.

    1.7 Completed Two Sets of STIS/CCD/MA2 8590 (UV Imaging and 
Spectroscopy of Luminous Blue Compact Galaxies from z=0 to z=1)

        The Space Telescope Imaging Spectrograph (CCD and MA2) was used to 
observe two well-defined samples of low-mass starburst galaxies, one in the 
local universe {z<0.1} and another at intermediate redshifts {0.2 < z < 
0.7}.  Both samples show optical sizes, morphologies, emission line widths, 
and luminosities comparable to those of LBGs at z=3, and are therefore 
probably the best local analogs and testbeds for further study of 
LBGs.  Our main goals are to: {1} explore the morphologies, surface 
brightness distributions, and half-light radii of nearby starforming 
galaxies in the FUV, near Ly-alpha; {2} search for systematic differences 
among UV, optical, and near-IR morphologies and structural parameters; {3} 
investigate the intrinsic emission and absorption spectra near Ly-alpha of 
starbursting dwarf galaxies, with special attention to Ly- alpha profiles 
and interstellar and stellar photospheric absorption from Si II, O I, C II, 
Si IV, and C IV; {4} measure their FUV-optical colors and dust extinction 
properties; and {5} test the hypothesis that low-mass starbursts are the 
local counterparts of LBGs.  The observation completed normally.

    1.8 Completed Two Sets of STIS/CCD 9136 (T Tauri Star Coronagraphic 
Survey: A PMS Protoplanetary Disk Census)

      The Space Telescope Imaging Spectrograph (CCD) was used to observe 
pre-main sequence solar-mass stars, the T Tauri stars that Millimeter and 
IR studies suggest at least 50 percent have circumstellar disks similar to 
the disk from which our planetary system formed.  High spatial resolution, 
high dynamic range imaging of such systems will map the spatial 
distribution of material around the star, constraining the disk sizes and 
inclinations, and provide a first assessment of when structure in the disk, 
such as cleared central zones and annuli, which has been linked to planet 
formation, develops.  All observations completed without incident.

    1.9 Completed WF/PC-2 9155 (The Cepheid Distance to NGC 1637: A Direct 
Comparison with the EPM Distance to SN 1999em)

        The WF/PC-2 was used to directly compare distances estimated by two 
primary extragalactic distance indicators. T he appearance of supernova 
1999em, a bright, extremely well- observed type II plateau event in the 
nearby SBc galaxy NGC 1637 offers the best chance to test the consistency 
of the Expanding Photosphere Method {EPM} of supernova distance 
determination with that derived from Cepheid variable stars.  Although EPM 
distances have been measured to 18 type II supernovae out to 180 Mpc and 
used to determine Hubble's constant independent of the Cepheid distance, 
there have never been any measurements of Cepheids in a galaxy that has 
hosted a normal type II-P supernova, the classic variety of core-collapse 
event to which EPM-derived distances are most robust.  The proposal 
completed nominally.

    1.10 Completed Seven Sets of STIS/CCD 9285 (POMS Test Proposal: STIS 
Non-scripted Parallel Proposal Continuation III)

        The Space Telescope Imaging Spectrograph (CCD) was used to make low 
galactic latitude, non-scripted parallel observations as part of a POMS 
test proposal.  The observations were completed as planned, and no 
anomalies were reported.

    1.11 Completed WF/PC-2/STIS/CCD 9258 (Observatory Focus Monitor)

        The WF/PC-2 and the Space Telescope Imaging Spectrograph (CCD) were 
used to more accurately define the HST focus.  The HST focus drifts slowly 
and shows evidence of undergoing slips of a few microns at random 
times.  The rate of the WF/PC-2 monitoring program is insufficient to track 
and/or understand OTA behavior in order to request timely and appropriate 
Secondary Mirror corrections.  There were no reported problems.

    1.12 Completed WF/PC-2 9069 (Proper Motions in Extragalactic Optical Jets)

        The WF/PC-2 was used to observe the flow velocity of extragalactic 
jets which is a crucial missing parameter in our understanding of these 
objects.  We would like to build on our successful HST proper motion 
measurements in M87, and propose similar measurements in four other optical 
jets.  The proposal completed with no reported problems.

    1.13 Completed Three Sets of STIS/CCD 8903 (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.  There were no problems.

    1.14 Completed Three Sets of STIS/CCD 9066 (Closing in on the Hydrogen 
Reionization Edge of the Universe)

        The Space Telescope Imaging Spectrograph (CCD) was used in parallel 
constrain the Hydrogen reionization edge in emission that marks the 
transition from a neutral to a fully ionized IGM at a predicted 
redshifts.  The proposal completed uneventfully.

    1.15 Completed FGS/1 9227 (Observations of Astrophysically Important 
Visual Binaries)

        Fine Guidance Sensor #1 was used to perform observations of three 
visual binary stars that will ultimately yield fundamental astrophysical 
results, once their orbits and masses are determined.  The targets are the 
following: {1} Procyon {P=41 yr}, for which our first WF/PC-2 images 
yielded an extremely accurate angular separation of the bright F star and 
its very faint white-dwarf companion.  Combined with ground-based 
astrometry of the bright star, our observation significantly revised 
downward the derived masses, and brought Procyon A into excellent agreement 
with theoretical evolutionary tracks for the first time.  The mass of 
Procyon B, however, implies a completely unexpected chemical composition 
for the white dwarf, and now poses a sharp evolutionary puzzle.  With the 
continued monitoring proposed here, we will obtain masses to an accuracy of 
better than one percent, providing a test bed for theories of Sun-like 
stars and white dwarfs. {2} G 107-70, a close double white dwarf {P=19 yr} 
that promises to add two accurate masses to the tiny handful of white-dwarf 
masses that are directly known from dynamical measurements. {3} Mu Cas 
{P=21 yr}, a famous metal-deficient G dwarf for which accurate masses will 
lead to the stars' helium contents, with cosmological implications.  No 
problems were encountered for these observations.

    1.16 Completed WF/PC-2 9042 (An Archive To Detect The Progenitors Of 
Massive, Core-Collapse Supernovae)

         The WF/PC-2 was used to search for supernovae which have massive 
star progenitors.  The already extensive HST archive and high-resolution 
ground-based images of galaxies within ~20 Mpc enables us to resolve and 
quantify their individual bright stellar content.  As massive, evolved 
stars are the most luminous single objects in a galaxy, the progenitors of 
core-collapse supernovae should be directly detectable on pre-explosion 
images.  One Type II progenitor has been observed this year, and the 
investigators have proposed a short, companion WFPC2 proposal to confirm 
this candidate and identify a second.  The observations completed nominally.

    1.17 Completed Two Sets of STIS/CCD/MA1 8625 (The Metallicity of Gas in 
the Local Universe: Beyond the Milky Way)

        The Space Telescope Imaging Spectrograph (CCD and MA1) was used to 
obtain spectra of three QSO/AGN which lie behind nearby galaxies in order 
to measure the metallicity of the interstellar gas at the present epoch 
beyond the local group.  As described in HSTAR 8367 and 2.1, the 
acquisition for the second iteration of this proposal failed, the take data 
flag remained down, and observations were lost.  Otherwise, the proposal 
completed with no other reported anomalies.

    1.18 Completed STIS/CCD/MA1 9241 (The Disk and Wind of HD 104237)

         The Space Telescope Imaging Spectrograph (CCD and MA1) was used to 
perform GTO studies of intermediate-mass stars that have revealed 
circumstellar disks and associated nebulosities in 44% of our sample.  The 
largest-scale nebulosity is seen in those systems with emission in the 
unidentified infrared bands, which have been interpreted as being 
associated with C-H stretch and bend modes in small organic grains.  This 
hypothesis will be tested with coronagraphic observations of the nearby 
Herbig Ae star, HD 104237.  All observations completed normally.

    1.19 Completed Two Sets of FGS/1 9034 (The Masses and Luminosities of 
Population II Stars)

        Fine Guidance Sensor #1 was used to observe the mass-luminosity 
relation {MLR} of Population II stars of which very little is currently 
known.  With the advent of the Hipparcos Catalogue, improved distances to 
many spectroscopic binaries known to be Pop II systems are now 
available.  After surveying the literature and making reasonable estimates 
of the secondary masses, we find 13 systems whose minimum separation should 
be larger than the resolution limit of FGS #1.  The observations completed 
nominally.

    1.20 Completed WF/PC-2 9267 (Supernova Search)

        The WF/PC-2 was used to search for high-redshift supernovae in 
GO-observed fields, taking advantage of good first-epoch observations and 
of the scheduling opportunities available because STIS is not currently 
observing.  No anomalous activity was reported.

    1.21 Completed Four Sets of WF/PC-2 8941 (Cycle 10 UV Earthflats)

        The WF/PC-2 was used to monitor flat field stability by obtaining 
sequences of earth streak flats to improve the quality of pipeline flat 
fields for the WFPC2 UV filter set.  The proposal had no problems.

    1.22 Completed FGS/1 9170 (The Post-CE Status of the Massive WD Binary 
LB11146)

        Fine Guidance Sensor #1 was used to perform analyses of the 
spectrum of LB11146 that was discovered to be a binary system composed of 
magnetic/nonmagnetic white dwarfs each having a mass estimated to be ~0.9 
M_solar, making it the only known double degenerate system with a combined 
mass exceeding the Chandrasekhar limit.  No errors were reported

    1.23 Completed STIS/CCD 9284 (POMS Test Proposal: STIS Non-Scripted 
Parallel Proposal Continuation IV)

        The Space Telescope Imaging Spectrograph (CCD) was used in the 
parallel mode to make some low galactic latitude archive observations.  The 
observations were executed as scheduled, and no anomalies were noted.

    1.24 Completed WF/PC-2 9045 (The Relationship Between Radio Luminosity 
and Radio-Loud AGN Host Galaxy Properties)

        The WF/PC-2 was used to determine the relationship between the 
properties of the host galaxies of radio-loud AGN and their radio 
luminosities.  Previous studies in this area with the HST have concentrated 
on the 3C sample which shows a tight correlation between luminosity and 
redshift, such that evolutionary effects cannot be distinguished from those 
depending upon radio luminosity.  Our sample of 46 radio galaxies at z ~ 
0.5 comes from four complete, low-frequency-selected samples of radio 
sources with differing flux limits.  Thus the total sample spans an 
unprecedented three orders of magnitude in radio luminosity at a fixed 
redshift interval.  The proposal completed with no reported problems.

    1.25 Completed STIS/CCD/MA2 8651 (UV Spectroscopy in the Magellanic 
Bridge: A Typical QSO Absorption Line System?)

        The Space Telescope Imaging Spectrograph (CCD and MA2) was used to 
perform echelle UV absorption line spectroscopy through the Magellanic 
Bridge {near the SMC} to probe the temperature, ionization, and kinematic 
structure in a metal- poor environment like those observed in the early 
universe.  The sightline toward the QSO B0312-770 is especially interesting 
because of the proximity of the absorber  and the radio loud background 
source.  The observations completed nominally.

    1.26 Completed STIS/CCD 8669 (Merger-Driven Evolution Of Galactic 
Nuclei: Observations Of The Toomre Sequence)

        The Space Telescope Imaging Spectrograph (CCD) was used to observe 
galaxy mergers that are believed responsible for triggering starburst and 
AGN activity in galaxies, and even perhaps transforming spiral galaxies 
into ellipticals.  The proposal completed nominally.

    1.27 Completed WF/PC-2 9057 (Host Galaxies of Obscured QSOs Identified 
by 2MASS)

        The WF/PC-2 was used to perform a snapshot survey of red QSOs 
discovered in The Two Micron All Sky Survey {2MASS} to investigate the 
detailed properties of their host galaxies.  This large, possibly dominant, 
population of QSOs in the local universe has been previously overlooked 
because reddening by {intrinsic} obscuration along our line of sight causes 
their colors to be too red for identification by traditional "UV- excess" 
techniques.  Their near-IR colors are similar to PG- type {UV-excess} QSOs, 
but it is far from certain whether they are indeed from the same parent 
population or represent a completely new class of QSO.  There were no 
reported problems.

    1.28 Completed STIS/CCD 9143 (Spectrophotometry of Nearby Seyfert 2 
Nuclei: Can We Eliminate the Seyfert 2 Class?)

        The Space Telescope Imaging Spectrograph (CCD) was used to 
investigate Seyfert 2s that are distinguished by the absence of the broad 
emission lines characteristic of Seyfert 1s and more luminous QSOs.  Are 
Seyfert 2s fundamentally different from Seyfert 1s and their brighter 
cousins?  Or is the broad emission line region in Seyfert 2s simply 
suppressed by obscuring material as postulated by the unification 
model?  If the latter model is correct, the weak broad emission lines in 
the Seyfert 2s may simply be overwhelmed by starlight from the 
circumnuclear region, particularly in the case of recent star 
formation.  It is proposed to determine if all Seyfert 2s have {weak} broad 
emission line regions by obtaining long-slit STIS spectroscopy for a 
well-defined sample of 20 Seyfert 2s {3 archival, 17 new}.  The 
observations completed with no anomalous activity.

    1.29 Completed STIS/CCD 9176 (LMC Eclipsing Binaries with Cepheid 
Components: The Key to the Extragalactic Distance Scale)

        The Space Telescope Imaging Spectrograph (CCD) was used to 
determine the distance to the LMC and to observe the Cepheid P-L that form 
the backbone of the Cosmic Distance Scale and the determination of 
H_degrees.  Unfortunately, in spite of concerted efforts of many 
investigators, the zero point of the Cepheid P-L law and the LMC distance 
remain controversial and uncertain to ~10-15, using eclipsing binaries 
{EBs} as "standard candles'' to include two recently discovered LMC 
eclipsing binaries {EBs} with Cepheid components.  These observations of 
these extraordinary systems hold the key to determining simultaneously the 
Cepheid P-L zero point and the LMC distance, and to provide a direct test 
of the Baade-Wesselink parallax method.  There were no reported problems.

2.0 FLIGHT OPERATIONS SUMMARY:

    2.1 Guide Star Acquisitions:
       Scheduled Acquisitions: 27
Successful: 26

        The acquisition scheduled for 287/005807Z failed when the search 
radius limit was exceeded.  A subsequent FHST map showed relatively small 
errors.  HSTAR 8367 was written.  The proposals detailed in 1.2, 1.4, and 
1.17 were affected.
  Scheduled Re-acquisitions: 15
Successful: 15

    2.2 FHST Updates:
Scheduled: 66
Successful: 66

    2.3 Operations Notes:

        The SSR EDAC error counter was cleared ten times per ROP SR-1A.

        Using ROP DF-18A, the engineering status buffer limits were 
adjusted three times.

        Per ROP DF-01A, an HST table dump was performed at 285/1526Z.

        HSTAR 8366 documents an anomalous high condition for the high gain 
antenna x-axis gimbal position for one telemetry sample at 
286/171041Z.  The commanded value was 86.0 degrees; the anomalous value, 
87.6141 degrees.  The gimbal was not splining at the time.  The previous 
and following splines were nominal.

        ROP IC-2 was used to turn SSA #1 on and off for the interval 
286/1852Z through 286/1923Z and SSA #2 from 288/0834Z through 288/0845Z.

        A TTR was written when there was a required re-transmit at 
287/1800Z during a NSSC-1 load.  Accordingly, at 287/1806Z, per ROP NS-5, 
SI C&DH errors were reset.

        The engineering status buffer was dumped and cleared at 288/0242Z 
as directed by ROP DF-18A.

        A TTR was generated for a four-minute loss of engineering data 
starting at 288/0356Z as the result of a negative acquisition after a Mode 
1 GCMR.

3.0 SIGNIFICANT FORTHCOMING EVENTS:

        Continuation of normal science observations and calibrations.

/CAW