HUBBLE SPACE TELESCOPE

       DAILY REPORT #2944

PERIOD COVERED:  0000Z (UTC) 08/24/01 - 0000Z (UTC) 08/27/01

Daily Status Report as of 239/0000Z

1.0 OBSERVATIONS SCHEDULED AND ACCOMPLISHED:

    1.1 Completed STIS/CCD/MA2 8569 (A New Survey for Low-Redshift Damped 
Lyman-Alpha Lines in QSO MgII Systems)

        The Space Telescope Imaging Spectrograph (CCD and MA2) was used to 
support studies which have shown that most of the observable neutral gas 
mass in the Universe resides in QSO damped LyAlpha {DLA} systems.  However, 
at low redshift, DLA can only be found by searching in the UV with HST.  By 
boot-strapping from the MgII statistics, we will be able to further improve 
the determination of the low- redshift statistical properties of DLA {their 
incidence and cosmological mass density} and open up new opportunities for 
studies at low redshift.  The observations completed nominally.

    1.2 Completed Three Sets of STIS/MA1/MA2 8843 (Cycle 9 MAMA Dark 
Measurements)

        The Space Telescope Imaging Spectrograph (MA1 and MA2) was used to 
perform the routine monitoring of the MAMA detector dark noise.  The 
proposal completed nominally.

    1.3 Completed WF/PC-2 9124 (Mid-UV SNAPSHOT Survey of Nearby 
Irregulars: Galaxy Structure and Evolution Benchmark)

        The WF/PC-2 was used to investigate the relation between star 
formation and the global physical characteristics of galaxies to interpret 
the morphologies of distant galaxies in terms of their evolutionary 
status.  Distant galaxies are primarily observed in their rest frame 
mid-ultraviolet.  They resemble nearby late-type galaxies, but are they 
really physically similar classes of objects?  It is proposed to address 
this question through a SNAPSHOT survey in the 2 mid-UV filter F300W of 98 
nearby late-type, irregular and peculiar galaxies.  No problems were reported.

    1.4 Completed STIS/MA1/MA2 8917 (MAMA Dispersion Solution Check)

        The Space Telescope Imaging Spectrograph (MA1 and MA2) was used to 
determine wavelength dispersion solutions on a yearly basis as part of a 
long-term monitoring program {implemented as Program 7651 in Cycle 7, 
Program 8430 in Cycle 8 and 8859 in Cycle 9}.  No anomalous activity was 
reported.

    1.5 Completed STIS/CCD/MA1 9098 (The Spectrum and the Light Curve of 
the Nearest Millisecond Pulsar)

        The Space Telescope Imaging Spectrograph (CCD and MA1) was used to 
observe PSR J0437--4715 that is the nearest and the brightest millisecond 
{recycled} pulsar, and the only one that has been well studied at X-ray/EUV 
energies, where it has a strong pulsed signal.  It is the most promising 
candidate for detecting the first optical counterpart of a millisecond 
pulsar.  Thge observations completed with no reported problems.

    1.6 Completed Eleven 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 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.

    1.8 Completed STIS/CCD/MA1 8956 (Pre-SM Calibration)

        The Space Telescope Imaging Spectrograph (CCD and MA1) was used in 
an exercise to prepare for the SMOV-3B program.  Prior to SMOV3B, one 
iteration of proposal 8960 {Jitter Test} for WD 2126+734 will be 
performed.  Also one iteration of 8961 {End of BEA Test} for each new flux 
standard {WD 2126+734, WD 0320-539, WD 0710+741, and WD 0214+568} needed to 
completely cover all possible Bright Earth Avoidance {BEA} dates will be 
exercised.  Finally, one extra standard is added {WD 1407-475} to fill the 
gap around June when WD 0214+568 is too close to the Sun.  This iteration 
of the proposal completed with no reported problems.

    1.9 Completed 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.  As described in 2.1 and HSTAR 8315, the acquisition and the 
re-acquisition for this proposal defaulted to fine lock backup on one FGS 
only, possibly affecting all observations.  Otherwise, the proposal 
completed uneventfully.

    1.10 Completed WF/PC-2 9138 (Host Galaxies of Gravitationally Lensed 
Quasars)

        The WF/PC-2 was used to perform imaging studies of quasar host 
galaxies at high redshift that are biased toward detecting luminous 
hosts.  Gravitational lensing combined with optical and near-IR imaging 
enhances their detectivity and has nearly doubled the number of known hosts 
at z>1.  Lens studies have successfully imaged hosts with lower 
luminosities at farther distances beneath a larger fraction of quasars than 
imaging of non- lensed quasars.  We propose deep WFPC2 follow-up imaging of 
five lensed systems in the F555W and F814W filters, which offer unique 
opportunities for detailed studies of faint, high-redshift, quasar 
hosts.  As described in 2.1 and HSTAR 8315, the acquisition and the 
re-acquisition for this proposal defaulted to fine lock backup on one FGS 
only, possibly affecting all observations.  Otherwise, the proposal 
completed as planned.

    1.11 Completed FGS/1 8616 (Masses of Pre-Main Sequence Binaries)

        Fine Guidance Sensor #1 was used to continue mapping the orbits of 
young star binaries in the Taurus and Ophiuchus star forming regions.  Our 
goal is to measure their masses dynamically.  This is important because 
there are still no low mass young stars with reliably known masses so 
calculations of their evolution to the main sequence are 
uncalibrated.  There were no reported problems.

    1.12 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.

    1.13 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.

    1.14 Completed Five Sets of STIS/CCD 8864 (CCD Dark Monitor-Part 2)

        The Space Telescope Imaging Spectrograph (CCD) was used to monitor 
the darks for the CCD.  The proposal completed nominally.

    1.15 Completed Three Sets of STIS/CCD 8865 (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, to build up high-S/N superbiases and track the evolution of hot 
columns.  The proposal completed with no anomalous activity.

    1.16 Completed Two Sets of STIS/CCD/MA1/MA2 9176 (LMC Eclipsing 
Binaries with Cepheid Components: The Key to the Extragalactic Distance Scale)

        The Space Telescope Imaging Spectrograph (CCD, MA1 and MA2) was 
used to determine the distance to the LMC and to observe the Cepheid P-L 
that law 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.

    1.17 Completed Two Sets of WF/PC-2 8059 (POMS Test Proposal: Targeted 
Parallel Archive Proposal)

        The WF/PC-2 was used to observe the parallel opportunities 
available in the neighborhood of bright galaxies are treated in a slightly 
different way from the normal pure parallels.  Local Group galaxies offer 
the opportunity for a closer look at young stellar 
populations.  Narrow-band images in F656N can be used both to identify 
young stars via their emission lines, and to map the gas distribution in 
star-forming regions.  The observations completed nominally.

    1.18 Completed Five Sets of WF/PC-2 8828 (Cycle 9 Supplemental Darks pt3/3)

        The WF/PC-2 was used to obtain three dark frames every day to 
provide data for monitoring and characterizing the evolution of hot 
pixels.  The proposal completed with no reported problems.

    1.19 Completed FGS/1 9168 (The Distances to AM CVn Stars)

        Fine Guidance Sensor (FGS) #1 was used to determine the parallaxes 
and proper motions of the five brightest of the seven known AM CVn 
systems.  AM CVn systems are binaries where mass is transferred from a 
completely hydrogen-deficient, degenerate mass donor to a white dwarf 
primary through a helium accretion disk.  A better understanding of these 
systems is crucial for a number of reasons: (1) to study the late stages of 
binary evolution, (2) to study the effect of chemical composition on the 
physics of accretion discs, (3) to estimate their contribution to the 
Supernovae Ia rate, and (4) to estimate their contribution to the 
gravitational radiation background.  All observations completed with no 
reported problems.

    1.20 Completed Two Sets of 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.

    1.21 Completed STIS/CCD/MA1 9137 (Quasar Absorbers and Large Scale 
Structure)

        The Space Telescope Imaging Spectrograph (CCD and MA1) was used to 
perform spectroscopy of 15 bright  quasars in a 22 square degree region 
that has well-sampled galaxy redshifts.  No problems were encountered.

    1.22 Completed Two Sets of STIS/CCD 9148 (Light Echos and the Nature of 
Type Ia Supernovae)

        The Space Telescope Imaging Spectrograph (CCD) was used to take 
STIS snapshot images of a subset of 43 well observed Type Ia supernovae 
{SNIa}, most of which have been discovered in late type galaxies over the 
last 40 years to make a systematic search for light echos around SN 
Ia.  STIS will also observe a sample of 10 SN II and SN Ib/c, which are 
believed to be the result of massive star core collapse and, therefore, to 
be thin-disk population objects, in order to make an empirical calibration 
of the accuracy of our method for determining scale heights.  The SN Ia 
sample will provide a direct as well as accurate estimate of the scale 
height of SN Ia which is an important clue to the progenitors of these 
events.  The proposal completed nominally.

    1.23 Completed Two Sets of STIS/CCD 8924 (PSF and LP Filter Curve 
Calibration)

        The Space Telescope Imaging Spectrograph (CCD) was used in an 
attempt to tie down the wavelength dependence of the CCD imaging 
sensitivity.  To do this, it is necessary to have good photometric imaging 
data in both 50CCD and F28X50LP for stars of a variety of colors for which 
the spectral energy distribution is known with great accuracy.  To fill in 
a color gap in the data that meets these requirements, the proposer will 
obtain spectra of a late F star for which extensive imaging data is 
available, and also will obtain both spectra and deep dithered CCD images 
of an early K star.  No problems occurred.

    1.24 Completed Three 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.

    1.25 Completed STIS/CCD 9128 (A Snapshot Survey of Absorption Lines 
from High Velocity Clouds in the Milky Way)

        The Space Telescope Imaging Spectrograph (CCD) was used to search 
for Mg II and Mg I absorption from Galactic High Velocity Clouds {HVCs} 
along the sightlines of 51 of the brightest QSOs, BL Lacs and Seyfert 2 
galaxies in the sky.  The observations completed with no rpeorted problems.

    1.26 Completed STIS/CCD/MA1/MA2 8857 (MAMA Sensitivity and Focus 
Monitor C9)

        The Space Telescope Imaging Spectrograph (CCD, MA1 and MA2) was 
used to monitor the sensitivity of each MAMA grating mode to detect any 
change due to contamination or other causes.  There were no problems.

    1.27 Completed STIS/CCD/MA1 9154 (Spatial Distribution Of The Gas 
Inside The Beta Pic Disk)

        The Space Telescope Imaging Spectrograph (CCD and MA1) was used to 
investigate the gas and dust disk surrounding Beta Pictoris that will give 
clues to the understanding of the late stages of planetary 
formation.  There was no anomalous activity.

    1.28 Completed STIS/CCD 9121 (Evolution of the Host Galaxies in Low- 
Power AGN)

        The Space Telescope Imaging Spectrograph (CCD) was used to study 
the evolution of low-power AGN host galaxies to z~1.3, allowing the direct 
study of how the formation and life cycles of radio-loud AGN depend on 
intrinsic power.  There were no reported problems.

    1.29 Completed WF/PC-2 9135 (A New High-Z Galaxy Cluster with 
Extraordinary Lensed Arcs From Multiple Sources)

        The WF/PC-2 was used to observe strong lensing by a relatively high 
redshift {z~0.7} cluster in the Red-Sequence Cluster.  This lens system has 
more bright arcs, with better cluster azimuthal coverage than examples of 
lower z lenses previously imaged.  At least 4 separate arcs are detected in 
our initial survey data, at 3-4 different cluster-centric radii and hence 
likely corresponding to at least 3 different background sources at 3 
different redshifts.  Moreover, these arcs are relatively bright and hence 
redshifts should be readily obtainable using 8m class telescopes.  All 
observations completed normally.

    1.30 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.

2.0 FLIGHT OPERATIONS SUMMARY:

    2.1 Guide Star Acquisitions:
       Scheduled Acquisitions: 21
Successful: 21

        The acquisition at 236/143500Z and the re-acquisition at 236/1605Z 
defaulted to fine lock backup on FGS-3 only.  HSTAR 8315 was written.  The 
proposals detailed in 1.9 and 1.10 may have been affected.
  Scheduled Re-acquisitions: 23
Successful: 23

    2.2 FHST Updates:
Scheduled: 51
Successful: 51

    2.3 Operations Notes:

        Using ROP SR-1A, the SSR EDAC error counter was cleared nine times.

        ROP DF-18A was utilized twice to reset the 486 engineering status 
buffer.

        Two TTRs were written when re-transmits were required at 236/1306Z 
and at 236/2010Z during NSSC-1 loads.  In each case, SI C&DH errors were 
reset per ROP NS-5.

        Re-dumps of science data were executed at 238/2336Z and at 
238/2338Z as directed by ROP SR-1A.

3.0 SIGNIFICANT FORTHCOMING EVENTS:

        GSFC Internal Simulation #13 (Rendezvous/Capture) will occur today, 
beginning at 8:00 am and continuing until approximately 6:00 pm.

        Continuation of normal science observations and calibrations.

/CAW