HUBBLE SPACE TELESCOPE

DAILY REPORT        # 3175

PERIOD COVERED: DOY 220

OBSERVATIONS SCHEDULED (see HSTARS below for possible observation problems)

STIS/CCD 8902

Dark Monitor-Part 2.

The Space Telescope Imaging Spectrograph (CCD) was used to monitor the darks.

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.

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.

WFPC2 8938

WFPC2 CYCLE 9 SUPPLEMENTAL DARKS pt3/3.

This dark calibration program obtains 3 dark frames every day to provide data
for monitoring and characterizing the evolution of hot pixels.

WF/PC-2 9091

Evolution of Star Forming Environments in H II Regions.

The WF/PC-2 was used to look for evaporating gaseous globules and silhouette
disks in two young clusters and along one molecular cloud wall.

ACS 9425

The Great Observatories Origins Deep Survey: Imaging with ACS

We propose a Treasury program of ACS imaging as part of the Great Observatories
Origins Deep Survey {GOODS}, covering 320{square}', or 32* the area of the two
original WFPC2 HDFs, to within 0.5--0.8 mag of their depth in four ACS bands,
BViz. The two GOODS fields, the Hubble Deep Field North and Chandra Deep Field
South, are the premier deep survey areas from X-- ray to radio wavelengths. ACS
data will provide unique angular resolution, sensitivity, and wavelength
coverage to close the gap between the deepest Chandra and SIRTF observations.
Supported by extensive imaging and spectroscopy from the VLT, Keck, Subaru,
NOAO, Gemini, VLA, JCMT, and other facilities, the combined GOODS data set will
make it possible to map the evolution of the Hubble sequence with redshift,
reconstruct the history of galaxy mass assembly, star formation and nuclear
activity from the epoch of reionization to the present, trace the growth of
density perturbations via cosmic shear, and, with properly phased z--band
observations, detect ~ 12 Type Ia supernovae at 1.2<z<1.8 to test the cosmic
acceleration and the presence of dark energy. All HST, SIRTF, Chandra, and
supporting GOODS data are non-- proprietary, with science--quality images and
catalogs released on a timescale of months. This will constitute the deepest,
largest, and most uniform panchromatic data set ever assembled to study the
distant universe.

ACS 9472

A Snapshot Survey for Gravitational Lenses among z >= 4.0 Quasars

Over the last few years, the Sloan Digital Sky Survey has revolutionized the
study of high-redshift quasars by discovering over 200 objects with redshift
greater than 4.0, more than doubling the number known in this redshift 
interval.
The sample includes eight of the ten highest redshift quasars known. We propose
a snapshot imaging survey of a well-defined sample of 250 z > 4.0 quasars in
order to find objects which are gravitationally lensed. Lensing models 
including
magnification bias predict that at least 4% of quasars in a flux-limited sample
at z > 4 will be multiply lensed. Therefore this survey should find of order 10
lensed quasars at high redshift; only one gravitationally lensed quasar is
currently known at z > 4. This survey will provide by far the best sample to
date of high-redshift gravitational lenses. The observed fraction of lenses can
put strong constraints on cosmological models, in particular on the 
cosmological
constant Lambda. In addition, magnification bias can significantly bias
estimates of the luminosity function of quasars and the evolution thereof; this
work will constrain how important an effect this is, and thereby give us a
better understanding of the evolution of quasars and black holes at early
epochs, as well as constrain models for black hole formation.

ACS 9480

Cosmic Shear With ACS Pure Parallels

Small distortions in the shapes of background galaxies by foreground mass
provide a powerful method of directly measuring the amount and distribution of
dark matter. Several groups have recently detected this weak lensing by
large-scale structure, also called cosmic shear. The high resolution and
sensitivity of HST/ACS provide a unique opportunity to measure cosmic shear
accurately on small scales. Using 260 parallel orbits in Sloan textiti {F775W}
we will measure for the first time: beginlistosetlength sep0cm 
setlengthemsep0cm
setlength opsep0cm em the cosmic shear variance on scales <0.7 arcmin, em the
skewness of the shear distribution, and em the magnification effect. 
endlist Our
measurements will determine the amplitude of the mass power spectrum
sigma_8Omega_m^0.5, with signal-to-noise {s/n} ~ 20, and the mass density
Omega_m with s/n=4. They will be done at small angular scales where non-linear
effects dominate the power spectrum, providing a test of the gravitational
instability paradigm for structure formation. Measurements on these scales are
not possible from the ground, because of the systematic effects induced by PSF
smearing from seeing. Having many independent lines of sight reduces the
uncertainty due to cosmic variance, making parallel observations ideal.

ACS/WFPC2 9481

Pure Parallel Near-UV Observations with WFPC2 within High-Latitude ACS Survey
Fields

In anticipation of the allocation of ACS high-latitude imaging survey{s}, we
request a modification of the default pure parallel program for those WFPC2
parallels that fall within the ACS survey field. Rather than duplicate the red
bands which will be done much better with ACS, we propose to observe in the
near-ultraviolet F300W filter. These data will enable study of the rest-frame
ultraviolet morphology of galaxies at 0<z<1. We will determine the 
morphological
k-correction, and the location of star formation within galaxies, using a 
sample
that is likely to be nearly complete with multi-wavelength photometry and
spectroscopic redshifts. The results can be used to interpret observations of
higher redshift galaxies by ACS.

ACS/WFPC2 9488

Cosmic Shear - with ACS Pure Parallel Observations

The ACS, with greater sensitivity and sky coverage, will extend our ability to
measure the weak gravitational lensing of galaxy images caused by the large
scale distribution of dark matter. We propose to use the ACS in pure parallel
{non- proprietary} mode, following the guidelines of the ACS Default Pure
Parallel Program. Using the HST Medium Deep Survey WFPC2 database we have
measured cosmic shear at arc-min angular scales. The MDS image parameters, in
particular the galaxy orientations and axis ratios, are such that any residual
corrections due to errors in the PSF or jitter are much smaller than the
measured signal. This situation is in stark contrast with ground-based
observations. We have also developed a statistical analysis procedure to derive
unbiased estimates of cosmic shear from a large number of fields, each of which
has a very small number of galaxies. We have therefore set the stage for
measurements with the ACS at fainter apparent magnitudes and smaller, 10
arc-second scales corresponding to larger cosmological distances. We will adapt
existing MDS WFPC2 maximum likelihood galaxy image analysis algorithms to work
with the ACS. The analysis would also yield an online database similar to that
in archive.stsci.edu/mds/

ACS/CAL 9558

ACS weekly Test

This program consists of basic tests to monitor, the read noise, the 
development
of hot pixels and test for any source of noise in ACS CCD detectors. This
programme will be executed once a day for the entire lifetime of ACS.

ACS 9665

Extreme Red Stars

ACS provides unprecedented sensitivity in the far red, this coupled with recent
astronomical pushes to ever cooler objects {e.g. new classifications for L 
and T
stellar dwarfs, and extremely high redshift galaxies} increases the need for
extending the photometric calibration to include such objects. We propose
observations of 4 stellar objects for which excellent ground based optical and
near-IR data exist that span V-I colors of 4.5 at M7 to > 6.0 at L5.

WFPC2 9676

POMS Test Proposal: WFII parallel archive proposal

This is the generic target version of the WFPC2 Archival Pure Parallel program.
The program will be used to take parallel images of random areas of the sky,
following the recommendations of the 2002 Parallels Working Group.

POMS 9677

POMS Test Proposal: WFII backup parallel archive proposal

This is a POMS test proposal designed to simulate scientific plans.

FLIGHT OPERATIONS SUMMARY:

HSTARS (For details see http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf)
HSTAR:  8755 - .GS Acquisition (2,1,2) @ 220/13:05:37Z resulted in FL backup
         on FGS 1 due to SSSL exceeded on FGS 1 @ 220/13:09:35Z. Under
         investigation.


COMPLETED OPS REQs: None

OPS NOTES EXECUTED: None


                       SCHEDULED     SUCCESSFUL    FAILURE TIMES
FGS GSacq             7                    7
FGS REacq             9                    9
FHST Update           14                 14
LOSS of LOCK

Operations Notes:
1. Commanded 2 'Tlm Fmt Change Via R/T Cmd', SSR ENG and SCI Dumps and a 
NSSC-1 Load.

SIGNIFICANT EVENTS

Configured CCS "G" String, CCS Release 4.0.1 - IP Packet Filter Mode as
Prime Ops @ 220/13:45Z.  Commanded two real-time telemetry format changes,
SSE engineering and science data playbacks, and NSSC-1 load uplink.
Returned to CCS "A" String Serial Conversion Device Mode @ 220/21:16Z.

Successfully completed Source/Destination Code Test 220/11:30Z - 13:20Z in
both GSTDN and JSC modes.  All steps were successful and all Source and
Destination codes matched up with the script.  Test was run twice, once
in IPMULTICAST mode and once in Serial mode.  No TSARs were written.

HST On-Orbit Checkout of real-time WSC interface scheduled daily 217 - 224
with GDOC, STOCC Ops (SIMOR), HITT, and CCS using CCS "G" String with CCS
Release 4.0.1 and PRD D06100R2.  The purpose of this testing is to verify
CCS Release 4.0.1 (IP) capability to interface through the IP Packet
Filters to WSC for real-time telemetry and commands.

HST "B" String Command Timing test scheduled 221/12:00Z - 21:00Z with GDOC,
SOC, HITT, and CCS using CCS "B" String with CCS Release 4.0.1 and PRD
D06100R2.