HUBBLE SPACE TELESCOPE

       DAILY REPORT #3087

PERIOD COVERED:  0000Z (UTC) 04/03/02 - 0000Z (UTC) 04/04/02

Daily Status Report as of 094/0000Z

1.0 OBSERVATIONS SCHEDULED AND ACCOMPLISHED:

    1.1 Completed ACS 9014 (Fine Corrector Alignment)

        The Advanced Camera for Surveys was used to optimize the ACS image 
quality over the by adjusting the IM1 and M1 corrector mechanisms in both 
tip/tilt {cylinder rotation} and focus.  This activity uses the same target 
field and exposures as proposal 9013 {ACS Coarse Corrector Alignment}, but 
performs fine focus and tip/tilt scans to refine the alignment resulting 
from that activity.  The proposal completed with no reported problems.

    1.2 Completed Three Sets of STIS/CCD 8902 (Dark Monitor-Part 2)

        The Space Telescope Imaging Spectrograph (CCD) was used to monitor 
the darks.  No problems were reported.

    1.3 Completed Three Sets of WF/PC-2 8937 (Cycle 9 Supplemental Darks pt2/3)

        The WF/PC-2 was used obtain three dark frames every day to provide 
data for monitoring and characterizing the evolution of hot pixels.  No 
problems were encountered.

    1.4 Completed WF/PC-2/ACS/HRC/WFC/STIS/CCD 9574 (Focus Monitor)

        The WF/PC-2, the Advanced Camera for Surveys (HRC and WFC) and the 
Space Telescope Imaging Spectrograph (CCD) were used to monitor HST 
focus.  In principle ACS/HRC should provide superior capability for 
monitoring the HST focus, bur since most of the HST science will shift to 
ACS in Cycle 11 trending observations are initiated with this program to 
establish the focus of WFPC2/PC1 {and hence HST} and ACS/HRC {and WFC to a 
lessor degree} using exposures over full orbits that are taken in 
parallel.  No problems were reported.

    1.5 Completed WF/PC-2 8952 (SM3B Flat Field Calibration)

        The WF/PC-2 was used to check for changes in flat field using 
external earth flat fields.  No problems were encountered.

    1.6 Completed STIS/CCD 8904 (Bias Monitor-Part 2)

        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 in order to build up high-S/N superbiases and track the evolution 
of hot columns.  The proposal completed with no anomalous activity.

    1.7 Completed ACS/HRC/WFC 9011 (ACS to FGS Alignment)

        The Advanced Camera for Surveys (HRC and WFC) was used to map the 
ACS detector coordinate frame to the FGS frame that will be determined from 
observations of an astrometric field with the ACS HRC and WFC 
channels.  Image quality over the field will also be assessed to verify the 
final adjustments to the corrector mechanisms from program 9014 (See 
1.1).  There were no reported problems.

    1.8 Completed FGS/1-2 9227 (Observations of Astrophysically Important 
Visual Binaries)

        The 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.

    1.9 Completed Five Sets of ACS/WFC/HRC 8947 (Weekly Test)

        The Advanced Camera for Surveys (WFC and HRC) was used to perform 
basic tests to monitor, the read noise, the development of hot pixels and 
test for any source of noise in ACS CCD detectors.  This program will be 
executed at least once a day for the entire lifetime of ACS.  There were no 
problems reported.

    1.10 Completed FGS/1 8898 (Calibrating FGS1r's Interferometric Response 
as a Function of Spectral Color)

        Fine Guidance Sensor #1 was used to obtain reference point source 
Transfer Functions {S-Curves} through the F583W filter and the F5ND 
attenuator at the center position of the FGS1r FOV for a variety of stellar 
spectral colors.  The data will be added to the library of point source 
interferograms that was assembled from the Cycles 8 and 9 calibration 
program.  These Transfer Functions are needed to support the analysis of GO 
science data for the study of close and wide binary star systems and for 
determining the angular diameter of extended sources.  The proposal 
completed with no reported problems.

    1.11 Completed Two Sets of FGS/1 8999 (SM3B Jitter Test)

        Fine Guidance Sensor 1R was used in both Position Mode {finelock} 
and Transfer Mode to observe selected targets in order to gain insight into 
the vehicle jitter characteristics after the alterations made to HST during 
SM3B.  No problems were encountered.

    1.12 Completed STIS/CCD 9147 (Probing The Structure Of The Shocks In 
The Narrow Line Region Of M 51)

        The Space Telescope Imaging Spectrograph (CCD) was used to 
determine whether nuclear or shock-induced photoionization dominates the 
gaseous ionization in the narrow-line region {NLR} of LINERs and Seyfert 
galaxies.  A critical issue is the determination of the input of mechanical 
energy in the NLR through jet/ISM interactions.  Previous studies suggest 
that the latter could actually suffice to power the NLR in most Seyfert 
galaxies.  Previous approaches to this problem have obtained integrated 
UV/visible line flux ratios, which are sensitive to uncertain 
reddening.  It is now proposed to map several spectral lines across the 
shock/precursor complex in the spatially extended, jet-driven NLR of the 
nearby Seyfert 2 galaxy M 51, measuring the spatial distribution of 
kinematic subsystems, the ionization structure, and the gaseous density, 
across this structure.  All observations completed nominally.

    1.13 Completed STIS/CCD 8914 (Sensitivity Monitor C10)

        The Space Telescope Imaging Spectrograph (CCD) was used to monitor 
the sensitivity of each CCD grating mode to detect any change due to 
contamination or other causes.  The STIS focus is also monitored in an 
imaging mode.  There was no anomalous activity.

    1.14 Completed WF/PC-2 9060 (Photometry of a Statistically Significant 
Sample of Kuiper Belt Objects)

        The WF/PC-2 was used to propel the physical study of KBOs forward 
by performing accurate photometry at V, R, and I on a sample of up to 150 
KBOs.  The sample is made up of objects that will be observed at thermal 
infrared wavelengths by SIRTF and will be used with those data to derive 
the first accurate diameters and albedos for a large sample of KBOs.  The 
observations completed nominally.

2.0 FLIGHT OPERATIONS SUMMARY:

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

  Scheduled Re-acquisitions:  6
    Successful:  6

    2.2 FHST Updates:
    Scheduled: 14
    Successful: 14

    2.3 Operations Notes:

        The NICMOS Cryo Cooler cool-down continues nominally.

        The STIS MCE-2 reset at 093/1912Z while the low voltage was on and 
while outside any SAA interval.  MAMA-2 will be recovered during next 
week's SMS commanding at the time of the next high voltage on 
commanding.  The STIS flight software error counter was cleared at 
093/1951Z per ROP NS-12.

        Per an operations note, the MAMA threshold voltage limits were changed.

        Using ROP SR-3A, the SSR pointer was set at 093/2106Z.

        The 486 engineering status buffer limits were adjusted at 094/0407Z 
as directed by ROP DF-18A.

3.0 SIGNIFICANT FORTHCOMING EVENTS:

        Continuation of Servicing Mission Orbital Verification and the 
gradual resumption of normal science observations and calibrations.

/CAW