HST Daily Report # 3293
HUBBLE SPACE TELESCOPE
DAILY REPORT # 3293
PERIOD COVERED: DOY 34
OBSERVATIONS SCHEDULED
NICMOS 8790
NICMOS Post-SAA calibration – CR Persistence Part 1.
A new procedure proposed to alleviate the CR-persistence problem of
NICMOS.
Dark
frames will be obtained immediately upon exiting the SAA contour 23, and
every
time a NICMOS exposure is scheduled within 50 minutes of coming out of
the SAA.
The darks will be obtained in parallel in all three NICMOS Cameras. The
POST-SAA
darks will be non-standard reference files available to users with a
USEAFTER
date/time mark.
ACS 9425
The Great Observatories Origins Deep Survey: Imaging with ACS
We propose a Treasury program of ACS imaging as part of the Great
ACS/WFPC2 9481
Pure Parallel Near-UV Observations with WFPC2 within High-Latitude ACS
In anticipation of the allocation of ACS high-latitude imaging survey{s},
NICMOS 9485
Completing A Near-Infrared Search for Very Low Mass Companions to Stars
Most stars are fainter and less massive than the Sun. Nevertheless, our
ACS/WFC 9492
Extragalactic Distances: the Need for Accurate Photometry of Blue
The investigation of the Wind Momentum-Luminosity Relationship {WLR} of
WFPC2 9592
WFPC2 CYCLE 11 Standard Darks
This dark calibration program obtains dark frames every week in order to
WFPC2 9594
WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt2/3
This dark calibration program obtains 3 dark frames every day to provide
WFPC2 9596
WFPC2 CYCLE 11 INTERNAL MONITOR
This calibration proposal is the Cycle 11 routine internal monitor for
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 9613
STIS CCD Spectroscopic Flats C11
Obtain CCD flats on the STIS CCD in spectroscopic mode.
STIS 9633
STIS parallel archive proposal – Nearby Galaxies – Imaging and
Using parallel opportunities with STIS which were not allocated by the
WFPC2 9634
POMS Test Proposal: WFII targeted parallel archive proposal
The parallel opportunities available with WFPC2 in the neighborhood of
ACS 9673
CCD Daily Monitor
This program consists of basic tests to monitor, the read noise, the
NICMOS 9702
NICMOS Parallel Thermal Background
NICMOS Camera 2 pure parallel exposures in the F222M and F237M filters to
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:
OPS NOTES EXECUTED:
PASS OPS REPORT:FHST MAP 11
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 6 6
FGS REacq 11 11
FHST Update 6 6
LOSS of LOCK
SIGNIFICANT EVENTS:
CCS “B” String has been released to CCS Developers to complete CCS
SAC Flight Controller training on SSSP1 for SCHEDMAN and MOCTDRS
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
Survey
Fields
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
within
10 pc of the Sun
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.
Supergiants
and Cepheids
blue
supergiant stars as an independent extragalactic distance indicator has
reached
a critical phase. Following our recent discovery and spectroscopic
follow-up of
several tens of stars outside of the Local Group in NGC 300 and NGC 3621,
we can
now calibrate the WLR in terms of spectral subtype and metallicity with a
higher
accuracy than hithertho possible with the statistically limited samples
available in the nearby galaxies studied so far. This, however, requires
high-resolution imaging to obtain accurate BVI photometry of a
significant
fraction of those stars for which we have spectroscopic information. This
can be
effectively accomplished with eight ACS/WFC fields in these two galaxies.
As a
further step, we can use the calibrated WLR to measure the first
independent
extragalactic distance. We then propose additional imaging of six ACS/WFC
fields
in M101 to select blue supergiant candidates for spectroscopic follow-up.
Having
recently discovered more than a hundred new Cepheids in NGC 300, the
high-resolution imaging proposed for the photometry of blue supergiants
can
also
be used, with no additional observing effort, to verify the effects of
blending
on the Cepheid distance to this galaxy, an important calibrator of
secondary
distance indicators.
provide
data for the ongoing calibration of the CCD dark current rate, and to
monitor
and characterize the evolution of hot pixels. Over an extended period
these
data
will also provide a monitor of radiation damage to the CCDs.
data
for monitoring and characterizing the evolution of hot pixels
WFPC2, to
be run weekly to monitor the health of the cameras. A variety of internal
exposures are obtained in order to provide a monitor of the integrity of
the CCD
camera electronics in both bays {gain 7 and gain 15}, a test for quantum
efficiency in the CCDs, and a monitor for possible buildup of
contaminants on
the CCD windows.
and 1×1
at gain = 4, to build up high-S/N superbiases and track the evolution of
hot
columns.
Spectroscopy
TAC, we
propose to obtain deep STIS imagery with both the Clear {50CCD} and
Long-Pass
{F28X50LP} filters in order to make color-magnitude diagrams and
luminosity
functions for nearby galaxies. For local group galaxies, we also include
G750L
slitless spectroscopy to search for e.g., Carbon stars, late M giants and
S-type
stars. This survey will be useful to study the star formation histories,
chemical evolution, and distances to these galaxies. These data will be
placed
immediately into the Hubble Data Archive.
bright
galaxies are treated in a slightly different way from the normal pure
parallels.
Local Group galaxies offer the opportunity for a closer look at young
stellar
populations. Narrow-band images in F656N can be used both to identify
young
stars via their emission lines, and to map the gas distribution in
star-forming
regions. Thus, the filter F656N is added to the four standard filters.
Near
more
distant galaxies, up to about 10 Mpc, we can map the population of
globular
clusters; for this purpose, F300W is less useful, and only F450W, F606W,
and
F814W will be used.
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
establish the stability of the HST+NCS+Instrument thermal emission. This
data
will be compared against the already available Camera 3 measurements in
F222M
which show an increased thermal background.
10.
of
potential non-nominal performance that will be investigated.) None
Release
4.0.2 deployment.
Scheduled completion is 2/19/03. A 48-hour loading test will be
conducted
with “B” String
starting Friday afternoon (1/7/02), running through the weekend. Ops
Check-out of CCS “B”
String with CCS Release 4.0.2 is scheduled to start Friday afternoon
(1/4/02) and continue
through the weekend.
processing
(SAC-05) Teams
A and D. Once training is complete, SCHEDMAN (updated to process SMA
TDRS
services) and
MOCTDRS processing will move to SSSP1.
