HUBBLE SPACE TELESCOPE - Continuing to collect World Class
Science
DAILY REPORT #4896
PERIOD COVERED: 5am July 27 - 5am July 28, 2009 (DOY
208/09:00z-209/09:00z)
OBSERVATIONS SCHEDULED
COS 11478
COS NUV Flat Fields
Acquire long NUV flat field exposures using the internal
deuterium
calibration lamp with the G185M grating. Use central
wavelengths of 1835
angstroms, 1850 angstroms, and 1864 angstroms. Based on
data taken
during thermal vacuum testing in 2003 (Test 1750), a total
of 65,000
seconds of data should be sufficient to obtain ~7.5x10^7
total counts in
the science region of the detector (> 200 counts per
pixel, or 1800
counts per 3 x 3 pixel resolution element).
This is SMOV4 Activity COS-18.
COS 11485
COS Internal FUV Wavelength Measurement
Obtain an initial set of FUV wavelength calibration
exposures with
internal PtNe lamp 1 for each FUV grating and central
wavelength
combination. A more limited set of exposures to test
operation of
internal PtNe lamp 2 will be obtained in separate program
11496. Lamp 1
exposures wil be used to establish the limits of the
initial wavelength
scales and to determine if adjustments are necessary.
COS 11487
COS FUV Internal/External Wavelength Scales
Observe external radial velocity standard targets in
TIME-TAG
(FLASH=YES) mode with all grating and central wavelength
combinations.
The purpose is to obtain zero-point offsets for the wavelength
scale
(internal wavecal lamp scale to external standard
wavelength scale) and
PSA dispersion relations for all central wavelengths.
Following this determination, adjustments of the nominal
science target
spectral range for each grating and central wavelength
combination will
be made via SMS patchable constant for nominal OSM1
positions
corresponding to each central wavelength. Subsequent to
this
modification of the wavelength scale (and its verification
via analysis
of COS30 - program 11488), FUV science-related operations
and
wavelength- dependent EROs can commence.
COS 11496
SMOV Verification of
Obtain an initial set of wavelength calibration exposures
with internal
PtNe lamp 2 at one central wavelength for each FUV and NUV
grating.
Additionally, obtain NUV test exposures with MIRRORA and
MIRRORB for
PtNe lamp 2. Initial lamp wavelength calibration exposures
will be
obtained in separate proposals.
The program also executes the COS NUV grating efficiency
test (GET) in
two sections separated by 20-25 minutes of lamp cooling
time. The
cooling time allows the lamp to cool back to its state
prior to the
first half of the test. .Each section of the test contains
of 10 NUV
exposures designed to get the same S/N of various emission
lines
throughout the NUV band.
STIS07 11404
CCD Dark and Bias Monitor for SMOV4/Cycle 17 Activity
STIS-07
Monitor the darks for the STIS CCD. 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.
WFC3 11447
WFC3 IR Dark Current, Readnoise, and Background
This proposal obtains full-frame, four-amp readout images.
Un-illuminated internals are taken at regularly spaced
intervals
throughout SMOV in order to assess and monitor readnoise
and dark
current (of both light-sensitive pixels and reference
pixels), and bad
(warm, hot, dead, variable) pixels. In addition, externals
aimed at
fields with sparse stellar density are taken to measure
diffuse
background light.
This program corresponds to WFC3-34.
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:
18652-0 - Genslew for proposal 11474 (slot #2) @ 208/1501z
18653-0 - Genslew for proposal 11474 (slot #3) @ 208/1503z
18654-0 - Genslew for proposal 11474 (slot #4) @ 208/1510z
18655-0 - Update COS OSM2 FSW mech positions for G285M @
208/2346z
18643-1 - NCS Restart and Cool Down (steps #1-11) @
209/01:34z
COMPLETED OPS NOTES: (None)
SCHEDULED
SUCCESSFUL
FGS GSAcq 4 4
FGS REAcq 11 11
OBAD with Maneuver 3 3
SIGNIFICANT EVENTS:
NCS pre-conditioning for DOY 209 planned restart was
completed with
the execution of the first eleven steps of OR 18643-1 NCS
Restart and
Cool down at 209/01:34z.