After discussions among members in the parallel working group,<br>
we recommend the following for the default Cycle 11 NICMOS parallel<br>
program, which will be scheduled and executed by STScI.  This program<br>
does not preclude GO proposals to utilize the NICMOS parallel<br>
opportunities for observations requiring different observing modes<br>
(e.g., NICMOS cameras 1 or 2, grism spectroscopy, intermediate<br>
or narrow band filters, etc.).<P>
The default Cycle 10 NICMOS parallel program will consist of broad band<br>
direct imaging using Camera 3 (NIC3), offering the widest sky coverage<br>
and greatest sensitivity for faint galaxies.  For visits with duration<br>
less than or equal to 1 orbit, observations will be made through F160W<br>
filter only.  For any visits longer than 2 orbits, the time will be split<br>
equally between F110W and F160W filters.  This will provide near infrared<br>
color information for the faint galaxy population, and allow searches for<br>
extrememely red galaxies and other interesting classes of objects.<P>

From experience with previous NICMOS parallel images, we find that FOM<br>
dithering is essential for achieving high quality data reduction.  The<br>
two-point dither pattern used in the cycle 7 NICMOS default program was<br>
not adequate to cleanly reject or average over image defects, particularly<br>
post-SAA cosmic ray persistence signal.  Experience from GO programs has<br>
shown that larger numbers of dither positions always enables better quality<br>
for reduced images.  The Cycle 11 default program should be designed to<br>
enable the maximum number of independent FOM dither positions whenever<br>
possible.  The sequence of the exposures in the F110W and F160W filters<br>
should be chosen to ensure the maximum number of FOM dither positions<br>
in each bandpass.<br>