f the reddest galaxies. The nature of the extremely red galaxies 
remains unclear and our program of imaging and grism spectroscopy 
provides unique information regarding both the incidence of obscured 
star bursts and the build up of stellar mass at intermediate 
redshifts. In addition to carrying out the parallel program we will 
populate a public database with calibrated spectra and images, and
provide limited ground- based optical and near-IR data for the deepest 
parallel fields.

NICMOS 9485

Completing A Near-Infrared Search for Very Low Mass Companions to 
Stars within 10 pc of the Sun

Most stars are fainter and less massive than the Sun. Nevertheless, 
our knowledge of very low mass {VLM} red dwarfs and their brown dwarf 
cousins is quite limited. Unknown are the true luminosity function 
{LF}, multiplicity fraction, mass function, and mass-luminosity 
relation for red and brown dwarfs, though they dominate the Galaxy in 
both numbers and total mass. The best way to constrain these relations 
is a search for faint companions to nearby stars. Such a search has 
several advantages over field surveys, including greater sensitivity 
to VLM objects and the availability of precise parallaxes from which
luminosities and masses can be derived. We propose to complete our 
four-filter NICMOS snapshot search for companions to stars within 10 
pc. With a 10 sigma detection limit of M_J ~ 20 at 10 pc, we can 
detect companions between 10 and 100 AU that are at least 9 mag 
fainter than the empirical end of the main sequence and at least 6.5 
mag fainter than the brown dwarf Gl 229B. When completed, our search 
will be the largest, most sensitive, volume-limited search for VLM 
companions ever undertaken. Our four-filter search will permit
unambiguous identification of VLM-companion candidates for follow-up
observation. Together with IR speckle and deep imaging surveys, our 
program will firmly establish the LF for VLM companions at separations 
of 1-1000 AU and the multiplicity fraction of all stars within 10 pc.

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

WFPC2 9599

WFPC2 Cycle 11 UV Earth Flats

Monitor flat field stability. This proposal obtains sequences of earth 
streak flats to improve the quality of pipeline flat fields for the 
WFPC2 UV filter set. These Earth flats will complement the UV earth 
flat data obtained during cycles 8-10.

STIS 9605

CCD Dark Monitor-Part 1

Monitor the darks for the STIS CCD

STIS 9607

CCD Bias Monitor - Part 1

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.

ACS 9673

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

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.

STIS 9706

STIS Pure Parallel Imaging Program: Cycle 10

This is the default archival pure parallel program for STIS during 
cycle 10.


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