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14 May 2003

HUBBLE SPACE TELESCOPE

DAILY REPORT       # 3362

PERIOD COVERED: DOY 133

Part 2 of 3

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/

STIS 9507

STIS/UV snapshot survey of bright AGN

We propose a UV spectroscopic snapshot survey of bright AGN,
quadrupling the number of Seyferts UV spectra and adding dozens of
new quasars, aimed at the following goals: beginenumerate em Finding
the relationship between the intrinsic luminosity of the AGN and the
maximum velocity {and width} of the outflow emanating from it, and
determining the frequency of outflows in low-z AGN as a function of
luminosity. em Surveying IGM absorption line systems in numerous new
sight-lines. em Identifying promising targets for observations with
the future highly sensitive Cosmic Origin Spectrograph. endenumerate
A 35-minute snapshot with exposures in either the G140L or G230L will
yield spectra with a minimum S/N > 15 per resolution element at all
wavelengths for all our potential targets. This will allow us to be
sensitive to absorption lines to a limiting equivalent width of 0.3
Angstrom at the 3 Sigma level. In order to facilitate rapid
observational followup, we waive the data proprietary period
entirely.
 
WFPC2 9594

WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt2/3

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

STIS 9604

STIS CCD Performance Monitor

This activity measures the baseline performance and commandability of
the CCD subsystem. Only primary amplifier D is used. Bias and Flat
Field exposures are taken in order to measure bias level, read noise,
CTE, and gain. Numerous bias frames are taken to permit construction
of "superbias" frames in which the effects of read noise have been
rendered negligible. Full frame and binned observations are made,
with binning factors of 2 x 1, 1 x 2, 2 x 2, 4 x 1, and 4 x 2. Dark
images are taken in 2x2 binning mode; 1x1 binning darks are being
taken in the nominal CCD Dark Monitor. Bias frames are taken in
subarray readouts to check the bias level for ACQ and ACQ/PEAK
observations. All exposures are internals. 

STIS 9606

CCD Dark Monitor-Part 2

Monitor the darks for the STIS CCD.

STIS 9608

CCD Bias Monitor - Part 2

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.

STIS 9612

STIS CCD Hot Pixel Annealing Cycle 11

The effectiveness of the CCD hot pixel annealing process is assessed
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. Follows on from proposal 8906. 

STIS 9613

STIS CCD Spectroscopic Flats C11

Obtain CCD flats on the STIS CCD in spectroscopic mode.

STIS 9614

STIS CCD Imaging Flats C11

Investigate flat-field stability over a monthly period.

STIS 9615

Cycle 11 MAMA Dark Monitor

This test performs the routine monitoring of the MAMA detector dark
noise. This proposal will provide the primary means of checking on
health of the MAMA detectors systems through frequent monitoring of
the background count rate. The purpose is to look for evidence of
change in dark indicative of detector problem developing.

ACS 9661

ACS Polarization Calibration

This proposal aims to calibrate the polarization modes most heavily
used in Cycle 11. We need L-flat observations, observations of a
polarized star and an unpolarized star, and an observation of an
extended polarized source. 

ACS 9674

CCD Daily Monitor

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.

 - Continued -

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