HUBBLE SPACE TELESCOPE

       DAILY REPORT #3099

PERIOD COVERED:  0000Z (UTC) 04/19/02 - 0000Z (UTC) 04/22/02

Daily Status Report as of 112/0000Z

1.0 OBSERVATIONS SCHEDULED AND ACCOMPLISHED:

    1.1 Completed Two Sets ACS/HRC/WFC 9018 (Flat Field Stability)

        The Advanced Camera for Surveys (HRC and WFC) was used to assess 
the stability and uniformity of the low-frequency flat fields {L-flat} of 
the WFC detector by using multiple pointing observations of the globular 
clusters 47 Tucanae {NGC104}, thus imaging moderately dense stellar 
fields.  By placing the same star over different portions of the detectors 
and measuring relative changes in its brightness it will be possible to 
determine local variations in the response of the detectors.  There were no 
reported problems.

    1.2 Completed Six 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 Nine 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 STIS/CCD 8906 (Hot Pixel Annealing)

        The Space Telescope Imaging Spectrograph (CCD) was used to measure 
the effectiveness of the CCD hot pixel annealing process by measuring the 
dark current behavior before and after annealing and by searching for any 
window contamination effects.  In addition, CTE performance is examined by 
looking for traps in a low signal level flat.  There were no reported problems.

    1.5 Completed WF/PC-2 8950 (SM3B Cool Down, Contamination Monitor, and 
Focus Check)

        The WF/PC-2 was used to monitor the planned cooldown to -88C, 
followed by UV monitors, focus checks, as well as decons and associated 
monitors.  No problems were noted.

    1.6 Completed Three Sets of 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 Three Sets of STIS/MA2 9573 (NUV-MAMA Daily Dark Monitor)

        The Space Telescope Imaging Spectrograph (MA2) was used to perform 
daily monitoring of the NUV MAMA detector dark noise in order to monitor 
the effects of thermal changes on the NUV dark rate.  No problems occurred.

    1.8 Completed STIS/MA2 8923 (FUV-MAMA Cycle 10 Flats)

        The Space Telescope Imaging Spectrograph (MA2) was used to obtain 
FUV-MAMA observations of the STIS internal Krypton lamp to construct an FUV 
flat applicable to all FUV modes.  No problems were encountered.

    1.9 Completed Fifteen 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 STIS/CCD 9077 (Survey of the LMC Planetary Nebulae)

        The Space Telescope Imaging Spectrograph (CCD) was used to perform 
a snapshot survey of all known LMC planetary nebulae {PNe} in order to 
study the co-evolution of the nebulae and their central stars, and to probe 
the chemical enrichment history of the LMC.  There were no reported problems.

    1.11 Completed STIS/CCD/MA1/MA2 9036 (An Ultraviolet Spectroscopic 
Survey of Star-Forming Galaxies in the Local Universe)

        The Space Telescope Imaging Spectrograph (CCD, MA1 and MA2) was 
used to perform a comprehensive STIS ultraviolet spectroscopic survey of 
star-forming galaxies in the local universe.  The sample covers a broad 
range of morphologies, chemical composition, and luminosity.  The 
observations will provide spectral coverage between 1200 and 3100 Angstrom, 
at a resolution of 100 to 200 kms and S/N of about 30.  The data set will 
allow the proposers to document and quantify the effects of massive stars 
on the interstellar medium and to infer implications for the evolution of 
the host galaxies.  The proposal completed with no anomalous activity.

    1.12 Completed Thirty-eight 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.  As described in 2.1 and HSTAR 8621, the 
acquisition for the twenty-third iteration of this proposal defaulted to 
fine lock backup on one FGS only, possibly affecting three 
observations.  Then, as described in 2.1 and HSTAR 8622, the acquisition 
for the thirty-second iteration of this proposal defaulted to fine lock 
backup on one FGS only, possibly affecting one observation.  The NICMOS 
suspend occurred during the thirty-fifth iteration.  Due to the suspend the 
final three iterations did not execute.  No other problems were encountered.

    1.13 Completed Two Sets of STIS/MA1/MA2 9151 (UV Snapshot Observation 
of Nearby Star Forming Galaxies)

        The Space Telescope Imaging Spectrograph (MA1 and MA2) was used to 
obtain FUV and NUV images of nearby emission- line galaxies with existing 
star-formation rate {SFR} measurements from their HAlpha flux.  Recently, 
the use of the UV flux as a measure of SFR has gained much popularity for 
estimating SFRs at different cosmic epochs.  However, the SFR estimated 
from UV flux could be greatly biased due to dust extinction.  The KPNO 
International Spectroscopic Survey {KISS} provides a large sample of nearby 
HAlpha-selected starforming galaxies for which rich optical spectra are 
available for measuring metallicity and dust extinction through line 
ratios.  By observing a subset of nearby emission-line galaxies in the KISS 
sample with the STIS FUV and NUV MAMA, a direct comparison between UV and 
Halpha SFR estimates will be possible.  This will allow us to understand 
the effect of dust extinction on UV flux for star- forming galaxies over a 
wide range of HAlpha luminosity, metallicity absolute magnitude, and B-V 
color .  A rough dust extinction curve will be constructed for such 
objects, making it possible to test plausible dust extinction curves used 
in previous SFR studies of the distant universe.  Also, high-resolution UV 
images will allow us to search for plausible local counterparts to high 
redshift galaxies whose rest-frame UV morphology is available from existing 
optical HST data.  There were no reported problems.

    1.14 Completed Four Sets of STIS/CCD 9139 (Variability in the UV 
Spectrum of 3C 279: Testing Models for the Gamma-Ray Emission in Blazars)

        The Space Telescope Imaging Spectrograph (CCD) was used to 
determine whether gamma- rays are produced on the scale of the broad line 
region, using multi-epoch UV snapshots of 3C 279 to find and characterize 
its LyAlpha variability.  This will validate the mirror model for 
generating the intense gamma-ray emission from blazars.  3C 279 is the 
best-studied blazar from radio to gamma-ray wavelengths, showing frequent 
large flares over days to months.  Variability in the UV continuum and 
LyAlpha will directly reveal any coupling between the jet ionizing flux and 
the broad-line region emission, providing clues to the physics and 
energetics of all radio-loud AGN.  All observations completed without 
reported incident.

    1.15 Completed Three Sets of STIS/CCD 9070 (A Census of Nuclear Star 
Clusters in Late-Type Spiral Galaxies: II. Spectroscopy and Stellar 
Populations)

        The Space Telescope Imaging Spectrograph (CCD) was used to 
investigate spiral galaxies that have a prominent star cluster in their 
dynamical center.  Statistics for cluster frequency, size, and luminosity 
remain incomplete.  The proposal completed as planned.

    1.16 Completed Two Sets of 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.

    1.17 Completed STIS/CCD 9110 (A Search for Kuiper Belt Object Satellites)

        The Space Telescope Imaging Spectrograph (CCD) was used to 
investigate whether the large number of collisions thought to have taken 
place in the primordial Kuiper belt suggest that many Kuiper belt objects 
{KBOs} could have suffered binary-forming collisions similar to that which 
formed the Pluto -- Charon binary.  Detection of such KBO satellites would 
allow measurement of  KBO masses, would help to understand the past 
collisional environment of the Kuiper belt, and would give a context to the 
otherwise unique-seeming formation of the Pluto -- Charon binary.  The 
proposal completed with no reported problems.

    1.18 Completed FGS/1 8897 (Long Term Monitoring of FGS1R in Position Mode)

        Fine Guidance Sensor #1R was used to monitor its long-term 
evolution, presumably due to disorption of water from the instrument's 
graphite epoxy composits.  This manifests principally as a change in the 
plate scale and secondarily as a change in the distortions.  These effects 
are well modeled by adjustments to the rhoA and kA parameters which are 
used to transform the star selector servo angles into FGS {x, y} detector 
space coordinates.  By observing the relative positions of stars in a 
standard cluster at a fixed telescope pointing and orientation, the 
evolution of rhoA and kA can be monitored and calibrated to preserve the 
astrometric integrity of the FGS.  There were no reported problems.

    1.19 Completed Three Sets of STIS/CCD/MA1/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.  As described in 2.1 and HSTAR 8622, the acquisition for the final 
iteration of this proposal defaulted to fine lock backup on one FGS only, 
possibly affecting two observations.  There was no other anomalous activity.

    1.20 Completed STIS/CCD 8962 (Contamination Monitor)

        The Space Telescope Imaging Spectrograph (CCD) was used to observe 
the flux standard GRW +70 5824 to assess whether FUV sensitivity is 
significantly below performance obtained during execution of 8961 {End of 
BEA Test} and prior to SM3B.  Significantly degraded sensitivity will 
trigger additional observations of flux standards to validate the initial 
result and/or track subsequent {de}contamination.  GRW +70 5824 is observed 
bimonthly in the same mode as part of the regular STIS monitoring 
program.  Measurement accuracy will be limited global sensitivity 
fluctuations {less than 5%}, rather than photon counting statistics.  No 
anomalous activity was observed.

    1.21 Completed STIS/CCD/MA1 8965 (MAMA Darks)

        The Space Telescope Imaging Spectrograph (CCD and MA1) was used to 
obtain the twice-weekly dark frames, as in the corresponding calibration 
program {program 8843 in Cycle 9}.  Standard calibration reference files 
are constructed for use in pipeline reduction of SMOV3B data.  Transition 
to analogous calibration program begins when normal science operation with 
the MAMA detectors begins.

    1.22 Completed STIS/MA1 8921 (MAMA Fold Distribution)

        The Space Telescope Imaging Spectrograph (MA1) was used to monitor 
the performance of MAMA microchannel plates using a MAMA fold analysis 
procedure.  The fold analysis provides a measurement of the distribution of 
charge cloud sizes incident upon the anode giving some measure of changes 
in the pulse-height distribution of the MCP and, therefore, MCP gain.  All 
observations completed normally.

    1.23 Completed ACS/WFC 9020 (Preliminary ACS Sensitivity)

        The Advanced Camera for Surveys (WFC) was used to observe a 
spectrophotometric standard star through each filter of each camera to 
assess the sensitivity of the instrument.  The star is placed at the center 
of the aperture, and two images are taken through each filter.  As 
described in 2.1 and HSTAR 8621, the acquisition for this proposal 
defaulted to fine lock backup on one FGS only, possibly affecting one 
observation.  There were no other reported problems.

    1.24 Completed Two Sets of 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.

    1.25 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.

    1.26 Completed Fourteen Sets of STIS/CCD 8900 (Performance Monitor)

        The Space Telescope Imaging Spectrograph (CCD) was used to measure 
the baseline performance and commandability of the CCD subsystem.  All 
exposures are internals.  The observations completed normally.

    1.27 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.

    1.28 Completed WF/PC-2 9180 (Gamma-ray Burst Progenitors: Probing Their 
Environment)

        The WF/PC-2 was used to perform a target of opportunity observation 
of gamma ray burster (GRB), GRB-011121.   GRB astronomy is a field maturing 
at a phenomenal rate.  Three important new observational and theoretical 
discoveries, formulated over the last twelve months, allow the proposer to 
address new, and in many cases, more sophisticated questions than could 
have been posed previously.  These developments: the discovery of X-ray 
lines in GRB 991216; the observation that N_H as deduced from X-ray 
afterglow are one to two orders of magnitude larger than the dust 
extinction inferred from optical afterglow; and the growing realization 
that the afterglow emission may exhibit features of dust echoes, appear to 
offer unexpected and new diagnostics that will directly inform us about the 
progenitor, the circum-progenitor material and the immediate interstellar 
environs.  There were no reported problems.

2.0 FLIGHT OPERATIONS SUMMARY:

    2.1 Guide Star Acquisitions:
       Scheduled Acquisitions: 32
    Successful: 32

        The acquisition at 110/221158Z defaulted to fine lock backup on 
FGS-2 only when the scan step limit was exceeded on FGS-3.  HSTAR 8621 was 
written.  The proposals detailed in 1.12 and 1.23 may have been affected.

        As described in HSTAR 8622, the acquisition at 111/120212Z 
defaulted to fine lock backup on FGS 1 only when the scan step limit was 
exceeded on FGS-3.  The proposals detailed in 1.12 and 1.19 may have been 
affected.
  Scheduled Re-acquisitions: 13
    Successful: 13

    2.2 FHST Updates:
    Scheduled: 66
    Successful: 63

      Per HSTAR 8619, the full maneuver updates at 110/082304Z and at 
110/082549Z failed due to tracker #1.  The subsequent acquisition, however, 
was successful.

        The roll delay update scheduled for 110/100342Z failed due to 
tracker #1.  The following full maneuver updates passed.  HSTAR 8620 was 
written.

    2.3 Operations Notes:

        The NICMOS instrument transitioned to SAA Operate, via SMS 
commanding, at 109/0908Z.

        The +Wing Solar Array Drive Mechanism shaft temperature monitor, 
telemetered through SADE-2, flagged out-of-limits high at 109/091008Z for 
several minutes with values ranging between 75 and 87 degC.  HSTAR 8618 was 
generated.

        Per an operations request, the NCS min/max buffer was reset at 
109/1830Z.

        TTRs were generated for required re-transmits during 486 loads at 
110/0825Z, at 110/1003Z and at 111/1202Z.  In each case, the CCS limit for 
SESBSLD was updated per ROP DF-18A.

        Per HSTAR 8623, the NICMOS instrument suspended at 111/170543Z.  A 
status buffer message indicated an Intel Exception debug error, a message 
seen before on 97/270 and 98/017.  At the time of this occurrence, the 
instrument was in observe and executing dark exposures (see 1.12).  Several 
following NICMOS observations did not execute (see 1.12).  A NICMOS memory 
dump was performed per ROP NS-9 at 111/2053Z.  The dump was analyzed by 
flight software personnel.  An operations note was utilized to set the 
NICMOS bad mode count off while NICMOS was safed.  NICMOS was recovered to 
SAA Operate at 112/000253Z per an operations request.  All NICMOS 
observations following the recovery have been successful.

        A TTR was created for a required re-transmit during a NSSC-1 load 
at 111/1944Z.  Following, ROP NS-5 was used to reset SI C&DH errors at 
111/1949Z.

        Using ROP SR-1A, the SSR EDAC error counter was cleared at 111/2217Z.

        SI C&DH errors were reset at 112/0021Z per ROP NS-5.

3.0 SIGNIFICANT FORTHCOMING EVENTS:

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

/CAW