HST Daily Report # 3304
HUBBLE SPACE TELESCOPE
DAILY REPORT # 3304
PERIOD COVERED: DOY 51
OBSERVATIONS SCHEDULED
STIS 9455
Mid-Ultraviolet Spectral Templates for Old Stellar Systems
We propose a three-year program to provide both observational and
theoretical
mid-ultraviolet {2300A — 3100A} spectral templates for interpreting the
age and
metallicity of globular clusters and elliptical galaxies from spectra of
their
integrated light. The mid-UV is the region most directly influenced by
stellar
age, and is observed directly in optical and infrared studies of
high-redshift
quiescent systems. The reliability of age and metallicity determinations
remains
questionable until non-solar metallicities and abundance ratios are
considered,
and stars spanning the color-magnitude diagram are included, as we
propose
here.
With archival HST STIS spectra we have improved the list of mid-UV atomic
line
parameters, then calculated spectra from first principles which match
observed
spectra of standard stars up to one- fourth solar metallicity. We will
extend
both observations and calculations to stars of solar metallicity and
beyond, and
to those in short-lived stages hotter than the main-sequence turnoff,
stars not
currently well-represented in empirical libraries. The necessary
line-list
improvements will come from new high-resolution mid-UV spectra of nine
field
stars. A key application of the results of this program will be to the
old
systems now being discovered as `Extremely Red Objects’ at high
redshifts.
Reliable age-dating of these places constraints on the epoch when large
structures first formed in the universe.
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},
ACS 9583
The Great Observatories Origins Deep Survey: Imaging with ACS
{GOODS}, covering 320{square}’, or 32* the area of the two original WFPC2
WFPC2 9594
WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt2/3
This dark calibration program obtains 3 dark frames every day to provide
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 1×1, 1×2, 2×1, and 2×2 bin settings at gain=1,
STIS 9612
STIS CCD Hot Pixel Annealing Cycle 11
The effectiveness of the CCD hot pixel annealing process is assessed by
ACS 9658
ACS Earth Flats
This program will obtain sequences of flat field images by observing the
ACS 9673
CCD Daily Monitor
This program consists of basic tests to monitor, the read noise, the
WFPC2 9676
POMS Test Proposal: WFII parallel archive proposal
used to take parallel images of random areas of the sky, following the
STIS 9706
STIS Pure Parallel Imaging Program: Cycle 10
This is the default archival pure parallel program for STIS during cycle
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary reports
COMPLETED OPS REQs: None
OPS NOTES EXECUTED: None
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 06 06
FGS REacq 10 10
FHST Update 02 02
LOSS of LOCK
SIGNIFICANT EVENTS: None
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
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
data
for monitoring and characterizing the evolution of hot pixels
and 1×1
at gain = 4, to build up high-S/N superbiases and track the evolution of
hot
columns.
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.
bright
Earth. Several UV filters from the interim calibration program {9564}
require
additional exposures to obtain the required illumination. A few UV
filters from
this program will be repeated to monitor for changes in the flat fields
and to
verify the interim results. Since no streaks are observed in the UV, the
wavelength coverage is extended to longer wavelengths in order to explore
the
severity of streaks in the flats from clouds in the FOV. We have added
exposures
for the HRC in the visible filters to verify the results derived from the
L-flat
campaign and to explore the severity of streaks. We have also added
exposures on
WFC using the minimum exposure time and using filters which will not
saturate
the brightest WFC pixel by more than 10 times the full well.
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
recommendations of the 2002 Parallels Working Group.
10.
of
potential non-nominal performance that will be investigated.)
