HUBBLE SPACE TELESCOPE - Continuing to collect World Class
Science
DAILY REPORT #4886
PERIOD COVERED: 5am July 13 - 5am July 14, 2009 (DOY
194/0900z-195/0900z)
OBSERVATIONS SCHEDULED
COS 11469
COS NUV Optics Alignment and Focus
This program has stringent guide star and timing
requirements. Refer to
the observing description section for complete details.
This program determines the fine focus using NUV MIRRORA
exposures of
the same target as COS08 (program 11468 -
This program must
commence execution approximately 48 hours after completion
of visit 1 of
COS08 and as soon as possible after the uplink in visit 2
of COS08.
Three fine focus visits are executed to establish on-orbit
nominal
focus. Two detailed verification visits are executed after
the three
focus-sweep visits. Approximately 48 hours after each
odd-numbered visit
an uplink of new information is required.
COS 11482
FUV Detector Dark
Measure the FUV detector dark rate by taking long science
exposures with
no light on the detector. The detector dark rate and
spatial
distribution of counts will be compared to pre-launch data
in order to
verify the nominal operation of the detector, and for use
in the CalCOS
calibration pipeline. Variations of count rate as a
function of orbital
position will be analyzed to find dependence of dark rate
on proximity
to the SAA.
This is SMOV Activity COS-24.
WFC3 11433
IR Internal Flat Fields
This proposal corresponds to WFC3-20, and depends on the
completion of
the IR initial alignment (proposal 11425, WFC3-12). In
this test, we
will study the stability and structure of the IR channel
flat field
images through all filter elements in the WFC3-IR channel.
Flat field
images for each filter will be combined in order to
produce a
calibration-quality flat field image. High signal
observations will
provide a map of the pixel-to-pixel flat field structure,
as well as
identify the positions of any dust particles.
WFC3 11442
WFC3 FGS-UVIS Alignment
Mapping of the WFC3 UVIS detector coordinate frame to the
FGS frame will
be determined from observations of an astrometric field
with the WFC3
UVIS channel. Image quality over the field will also be
assessed to
verify the final adjustments to the corrector mechanisms
from program
11434.
This proposal is Activity ID WF29.
WFC3 11443
WFC3 FGS-IR Alignment
Mapping of the WFC3 IR detector coordinate frame to the
FGS frame will
be determined from observations of an astrometric field
with the WFC3 IR
channel. Image quality over the field will also be
assessed to verify
the final adjustments to the corrector mechanisms from
program 11435.
WFC3 11450
UVIS Photometric Zero Points
This proposal obtains the photometric zero points in 16
WFC3/UVIS
priority-1 filters, 20 WFC3/UVIS priority-2 filters, and 1
WFC3/UVIS ERO
filter using a hot DA white dwarf. The observations are
repeated at
intervals of 1 day, 7 days, and 30 days, to monitor
photometric
stability in 8 of the priority-1 filters, with emphasis in
the UV where
contamination would have the strongest effects.
WFC3 11451
IR Photometric Zero Points
This proposal obtains the photometric zero points in all
15 WFC3/IR
filters using two stars with distinct temperatures (a hot
DA white dwarf
and a solar analog). The observations are repeated at
intervals of 1
day, 7 days, and 30 days, to monitor photometric stability
in all
filters.
WFC3 11808
WFC3 UVIS Bowtie Monitor
The UVIS detector was observed during ground testing to
occasionally
exhibit flat field and dark variations with a bowtie
pattern. These
variations are most significant as ~1% flat field (gain)
variations
across the field of view. It is believed that this
represents a state or
condition into which the detector can transition for
reasons and under
circumstances which are not currently understood. It is
also very
unlikely that most science observations will determine the
state (bowtie
or no-bowtie) of the detector. Ground test data indicates
that this
state is long lived (many hours to ~one day). Hysteresis
or memory of
past light exposure is also associated with this state.
Recent evidence suggests that exposing the detector to
~200k to 500k
electrons may quench this state. This proposal obtains an
internal flat
field sequence of three exposures: one at 10x full well
with two at 0.5x
full well immediately before and after. Each exposure is
3x3 binned to
reduce the data volume required.
These visits should be scheduled 2x per day until further
direction is
provided.
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are
preliminary reports
of potential non-nominal performance that will be
investigated.)
HSTARS: (None)
COMPLETED OPS REQUEST:
18602-0 - Adjust NCS CPL Setpoint @ 194/1351z
18621-0 - Update COS Aperture positions in FSW @ 194/1424z
COMPLETED OPS NOTES: (None)
SCHEDULED SUCCESSFUL
FGS GSAcq 04 04
FGS REAcq 10 10
OBAD with Maneuver 05 05
SIGNIFICANT EVENTS: (None)