HUBBLE SPACE TELESCOPE

       DAILY REPORT #2995

PERIOD COVERED:  0000Z (UTC) 11/08/01 - 0000Z (UTC) 11/09/01

Daily Status Report as of 313/0000Z

1.0 OBSERVATIONS SCHEDULED AND ACCOMPLISHED:

    1.1 Completed Four 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.  The proposal completed with no 
reported problems.

    1.2 Completed Three Sets of 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.

    1.3 Completed Three 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.

    1.4 Completed Five 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.

    1.5 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.

    1.6 Completed Five 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.  The observations completed with no anomalous 
activity.

    1.7 Completed FGS/1 9305 (Photometric Calibration)

        Fine Guidance Sensor #1 was used to gather the data needed to 
verify/calibrate the time dependency of the photometric response that was 
seen for the first time during a long duration {> 2000 sec} observation of 
the bright target {V=7.8} HD 209458 under GO proposal 9179.  There were no 
reported problems.

    1.8 Completed WF/PC-2 8867 (Gamma-Ray Bursts: Discovering The 
Progenitors And Understanding The Explosion - Visits A0-R0)

        The WF/PC-2 was used to observe a gamma-ray burster, 
GRB010921.  Gamma-ray burst astronomy, one of the most active and exciting 
frontiers in astrophysics, is now entering a critical stage -- with 
dramatic leaps in understanding of these events, as well as new 
discoveries.  Improvements in triggering and positioning accuracy provided 
by the SAX and HETE-2 gamma-ray satellites will allow entirely new classes 
of events to be studied.  Given the recent progress in this field, the 
proposers are now in a position to design precision, broadband measurements 
that can provide quantitative information on the as-yet unknown energy 
sources, the explosion geometry, and the surrounding medium.  In 
particular, the growing evidence of an intimate connection between SNe and 
GRBs can be definitively tested.  The proposal completed with no reported 
problems.

    1.9 Completed 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.

    1.10 Completed Two Sets of STIS/CCD/MA2 9040 (Baryons In Intermediate 
Redshift {Z > 1} OVI Absorbers)

        The Space Telescope Imaging Spectrograph (CCD and MA2) was used to 
search for intervening OVI absorption systems in two further extremely UV 
bright intermediate redshift QSOs {HS 0747 + 4259, z = 1.9, V = 15.6; HS 
0818+2554, z = 1.5, V = 15.4} using the STIS E230M Echelle mode.  The 
scientific aim is to measure the baryonic fraction in the warm-hot 
intergalactic medium at redshifts 1 <=q z <=q 1.8.  Present existing data 
on HE 0515-4414 taken also with STIS E230M seem to indicate that the 
baryonic fraction at z = 1.5 is lower by a factor of ~ 15 than the high 
value found by Tripp et al. {2000} for z < 0.3.  Our results need to be 
confirmed by more lines of sight, and we plan to test hierarchical 
structure formation models which predict a rapid evolution between z = 1.5 
and z = 0.  The observations completed as planned with no reported 
anomalous activity.

    1.11 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.

2.0 FLIGHT OPERATIONS SUMMARY:

    2.1 Guide Star Acquisitions:
       Scheduled Acquisitions: 10
Successful: 10

  Scheduled Re-acquisitions:  4
Successful:  4

    2.2 FHST Updates:
Scheduled: 21
Successful: 21

    2.3 Operations Notes:

        The NSSC-1 status buffer was dumped and cleared at 312/1342Z per 
ROP NS-3.

        Using ROP SR-1A, the SSR EDAC error counter was cleared at 312/1346Z.

        An operations request was used to set a gyro bias deviation and a 
drift rate limit at 312/1420Z.

        A TTR was generated when there was a generic data drop out during a 
NSSC-1 uplink at 312/2046Z.  Using ROP NS-5, SI C&DH errors were reset at 
312/2049Z.

        SSA transmitter #2 was turned off and on for the interval 313/0836Z 
to 313/0905Z as directed by ROP IC-2.

3.0 SIGNIFICANT FORTHCOMING EVENTS:

        Continuation of normal science observations and calibrations.

/CAW