HUBBLE SPACE TELESCOPE

       DAILY REPORT #3100

PERIOD COVERED:  0000Z (UTC) 04/22/02 - 0000Z (UTC) 04/23/02

Daily Status Report as of 113/0000Z

1.0 OBSERVATIONS SCHEDULED AND ACCOMPLISHED:

    1.1 Completed Three Sets of ACS/WFC/HRC 9562 (Cycle 11 Internal Flat 
Field Stability)

        The Advance Camera for Surveys (WFC and HRC) was used to obtain 
flat field stability and characterization samples of the ACS filter 
set.  Only internal exposures using the calibration lamps were 
required.  There were no reported problems.

    1.2 Completed FGS/1 9034 (The Masses and Luminosities of Population II 
Stars)

        Fine Guidance Sensor #1R 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.

    1.3 Completed Four Sets of WF/PC-2 9318 (POMS Test Proposal: WFII 
Parallel Archive Proposal Continuation)

        The WF/PC-2 was used to perform the generic target version of the 
WFPC2 Archival Pure Parallel program.  The program was used to take 
parallel images of random areas of the sky, following the recommendations 
of the Parallels Working Group.  There were no reported problems.

    1.4 Completed STIS/CCD 8907 (Spectroscopic Flats C10)

        The Space Telescope Imaging Spectrograph (CCD) was used to obtain 
CCD flats in the spectrographic mode.  There were no reported problems.

    1.5 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.

    1.6 Completed Four 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.

    1.7 Completed STIS/CCD/MA1 9094 (The Wind-Wind Interactions in HD 5980)

        The Space Telescope Imaging Spectrograph CCD and MA1) was used to 
observe HD 5980, the visually brightest object in the SMC.  It contains a 
close eclipsing binary LBV+WR {=Star A+Star B}, the only one known to 
exist, with the possible exception of Eta Carinae.  The LBV underwent a 
great eruption in 1994, ejecting <10^-3 M_odot at velocities in the range 
of 200-800 km s^-1.  After the eruption, its wind velocity has been 
steadily increasing, and producing a circumstellar {CSM} fast- 
wind/slow-wind interaction region, which has now become visible 
spectroscopically in the C IV and Si IV lines at an expansion velocity of 
-680 km s^-1.  These narrow features varied over a 1 year timescale.  It is 
likely that HD 5980 is forming an H II region analogous to the Homunculus 
in Eta Carinae.  In addition, the wind-wind collision shocked region 
between the two stars currently {1999-2000} forms a shock cone that winds 
tightly around the WR star.  The purpose of this proposal is to: a} 
Determine the LBV's wind velocity close to the time when it will be 
observed with XMM and CHANDRA; b} follow the changes in the high velocity 
CSM absorption features; and c} Constrain the radial velocity variability 
of the third component, Star C, in order to determine whether it is bound 
to the A+B pair.  All observations completed without incident.

    1.8 Completed Thirteen Sets of NICMOS/1/2/3 8945 (Cooling System 
Monitoring)

        The Near Infrared Camera and Multi-Object Camera (NIC1, NIC2 and 
NIC3 was used 1) to measure NICMOS detector performance during the 
cool-down and steady state operation of the NCS. 2}. to demonstrate 
stability {+/-0.1K} of the NICMOS detector temperature at the optimal 
science operating temperature. and 3}.to demonstrate repeatability {+/-0.1 
K} of NICMOS detector temperature following changes from the optimal 
science operating temperature.  No problems were encountered.

    1.9 Completed Five Sets of WF/PC-2 8935 (Cycle 10 Standard Darks)

        The WF/PC-2 was used to obtain dark frames every week in order to 
provide data for the ongoing calibration of the CCD dark current rate, and 
to monitor and characterize the evolution of hot pixels.  Over an extended 
period these data will also provide a monitor of radiation damage to the 
CCDs.  The proposal completed with no reported problems.

    1.10 Completed Two Sets of STIS/MA1 8920 (Cycle 10 MAMA Dark Measurements)

        The Space Telescope Imaging Spectrograph (MA1) was used to perform 
the routine monitoring of the MAMA detector dark noise, and is the primary 
means of checking on health of the MAMA detectors systems through frequent 
monitoring of the background count rate.  The proposal completed with no 
reported anomalous activity.

    1.11 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.

    1.12 Completed Two Sets of STIS/CCD/MA2 9496 (UV Spectroscopic 
Investigation of Any Bright, Newly Discovered Comet)

        The Space Telescope Imaging Spectrograph (CCD and MA1) was used to 
perform a Target of Opportunity program to investigate any bright comet 
{mboxV<=sssim7} that is newly discovered during Cycle 11, including comets 
of any dynamical class.  The main scientific objective is to obtain 
accurate abundance measurements for several key cometary species: CO from 
the CO 4PG bands, cotwo from the CO Cameron bands, stwo from the stwo B-X 
bands, cstwo from CS emissions, and water from OH emissions.  The UV 
Cameron band emission is currently the only way to probe cotwo in 
comets.  No anomalous activity occurred.

    1.13 Completed WF/PC-2 8939 (Cycle 10 Internal Monitor)

        The WF/PC-2 was used to calibrate the internal monitor, to be run 
weekly to monitor the health of the cameras.  No problems were encountered.

    1.14 Completed ACS/WFC 9575 (Default {Archival} Pure Parallel Program)

        The Advanced Camera for Surveys (WFC) was used to test ACS pure 
parallels in POMS.  There were no reported problems.

    1.15 Completed FGS/1 9581 (A BEA Science Program: A High Angular 
Resolution Survey of Some of the Galaxy's Most Massive Stars)

        Fine Guidance Sensor #1R was used to make optimal use of otherwise 
unused telescope time while HST's pointing is restricted to the BEA cone 
during the first 12 days of SMOV3B.  The launch date of Feb 29 placed two 
of the Galaxy's most active star forming regions, Trumplers 14 and 16 in 
the Carina Nebula, within the BEA for the entire 12 day period.  FGS1r was 
used to conduct a high angular resolution survey of the most massive and 
luminous stars in these two magnificent clusters to establish the incidence 
of binarity at the high mass end of the HR diagram. This survey will close 
the detection gap between spectroscopic and speckle surveys in which 
duplicity can be concealed and will dramatically improve our knowledge of 
the IMF at the high mass end of the main sequence as well as the luminosity 
function {LF} of star forming regions which produce such high mass 
stars.  Finally, this survey will identify targets for an approved SIM Key 
Science project to dynamically determine O-star masses.  There was no 
anomalous activity.

    1.16 Completed STIS/MA2 9573 (NUV-MAMA Daily Dark Monitor)
Abstract

        The Space Telescope Imaging Spectrograph (CCD and MA2) was used to 
perform daily monitoring of the NUV MAMA detector dark noise, monitoring 
the effects of thermal changes on the NUV dark rate.  No anomalous activity 
was noted.

    1.17 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.

    1.18 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.

    1.19 Completed Three Sets of ACS/WFC/HRC 9075 (Cosmological Parameters 
from Type Ia Supernovae at High Redshift)

        The Advanced Camera for Surveys (WFC and HRC) was used to obtain a 
Hubble diagram of Type Ia supernovae {SNe Ia} that will be of long lasting 
value as a record of the expansion history of the universe.  No problems 
were encountered.

    1.20 Completed STIS/CCD 9131 (Imaging the Host Galaxies of High 
Redshift Type Ia Supernovae)

        The Space Telescope Imaging Spectrograph (CCD) was used to complete 
the snapshot survey of distant galaxies of known redshift which hosted 
supernovae {SNe} of Type Ia found via the Supernova Cosmology Project 
{SCP}.  No problems were seen.

    1.21 Completed WF/PC-2 9319 (POMS Test Proposal: WFII Backup Parallel 
Archive Proposal II)

        The WF/PC-2 was used to execute a POMS test proposal, designed to 
simulate future scientific plans.  The proposal completed without incident.

    1.22 Completed STIS/CCD 8916 (Spectroscopic Sensitivity Workout: 
First-order Modes)

        The Space Telescope Imaging Spectrograph (CCD) was used to measure 
the basic sensitivity for all supported MAMA and CCD first-order 
spectroscopic modes.  Sensitivity measurements are done for all supported 
tilts of the gratings, at a S/N suitable to any particular setting, in 
order to get all measurements done in a reasonable number of orbits but 
still get a very accurate sensitivity measurement.  There were no reported 
problems.

2.0 FLIGHT OPERATIONS SUMMARY:

    2.1 Guide Star Acquisitions:
       Scheduled Acquisitions: 11
    Successful: 11

  Scheduled Re-acquisitions:  4
    Successful:  4

    2.2 FHST Updates:
    Scheduled: 25
    Successful: 25

    2.3 Operations Notes:

        Using ROP SR-3, the SSR pointers were set at 112/0959Z.

        The engineering status buffer limit for SESBSLD was adjusted at 
112/1552Z and at 113/0345Z per ROP DF-18A.

        A 486 software dump was performed at 112/1754Z and at 112/1901Z, 
using ROP DF-01A.

        A TTR was generated when there was a required re-transmit during a 
NSSC-1 load at 112/2042Z.

        An operations request was utilized at 112/2113Z to transition the 
NCC PID control from the weighted neon temperatures to NICMOS dewar 
temperature.  The primary PID set-point was changed from 73.0 degK to 74.8 
degK and the NICMOS temperature valid flag in the NSSC-1 was set to 
indicate a valid dewar temperature, allowing the PID to actively manage the 
system using the primary control point.

        The ephemeris table was uplinked at 113/0143Z as directed by ROP 
DF-07A.

        The SSR-3 EDAC error counter was cleared at 113/0237Z per ROP DF-09A.

        HSTAR 8625 was written when the 486 status buffer issued a message 
indicating an FGS coarse mode angle check failure at 113/034137Z following 
a successful a primary acquisition at 13/033852Z.

3.0 SIGNIFICANT FORTHCOMING EVENTS:

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

/CAW