HUBBLE SPACE TELESCOPE - Continuing to collect World Class
Science
DAILY REPORT #4865
PERIOD COVERED: 5am June 11 - 5am June 12, 2009 (DOY
162/0900z-163/0900z)
OBSERVATIONS SCHEDULED
ACS/WFC 11371
CCD Cross Talk
The goal of this program is to verify the amount of cross
talk in the
ACS WFC detectors in the post SM4 era. Before the failure
of ACS the
cross talk was very low at gain=1 e-/DN and almost not
existent at
gain=2 e-/DN. We plan to verify if the cross talk with the
new
electronics is still at levels that do not represent
concerns for
science. Both gain=1 and gain=2 will be tested. A bright
extended source
and several bright (likely saturated) stars will be used
for the test.
The sources will be positioned in different quadrants to
verify if any
specific amplifier is more affected to cross talks than
others.
The program consists of four visits two orbits each. Only
three visits
are supposed to be executed for a total of 6 orbits. The
structure of
each visit is identical, the only difference is the
correlated double
sapling technique.
Visit 01 and 02 should be executed program between
programs 11814
(iteration #6 of the CEB-R optimization campaign) and
program 11815
(iteration #7 of the CEB-R optimization campaign). The aim
of these
visits is to confirm with external observations the impact
of the new
electronics on the cross talk while we are still
optimizing the CEB-R.
Visit 03 or visit 04 should be executed anytime after the
end of the
CEB-R optimization campaign depending on which of the dual
slope
integrator or correlated double sampling is adopted.
ACS/SBC 11372
SBC UV Contamination Check
ACS/SBC throughput in the far-UV will be monitored during
the bright
earth avoidance period through use of two non-BEA visits,
each of one
orbit separated by one week allowing observations of NGC
6681. A waiver
for two non-BEA orbits during BEA was previously granted.
Exposures will
be taken in PR110L, F115LP, F125LP, F140LP, F150LP and
F165LP as in
recent UV Monitor program observations. These results will
be one of the
activities determining if the BEA can be ended. A third
visit just after
BEA ends will repeat the above monitoring and include one
orbit with
F122M. ON HOLD visits 4 and 5 would substitute for 1 and 2
if SM4 is
delayed.
COS/NUV 11468
DESCRIPTION: In order to determine the location of the
frame with respect to the FGS reference frames, NUV
MIRRORA images will
be obtained of an astrometric target and field.
Astrometric guide stars
and targets must be employed for this activity in order to
facilitate
the alignment with the FGS. Images will be obtained at the
initial
pointing and at positions offset in V2 and in V3. Starting
with the
original blind pointing, obtain MIRRORA image exposures in
a 5x5
POS-TARG grid centered on initial pointing; repeat the
image sequence at
two bracketing focus positions in same visit. Following
completion of
third pattern, return to nominal focus and perform 5x5
ACQ/SEARCH target
acquisition and obtain one TIME-TAG MIRRORA image and one
ACCUM
verification exposure. Next perform an ACQ/IMAGE target
acquisition
followed by an ACCUM verification exposure. Also obtain
ACCUM
verification exposure for each of the two alternate focus
positions used
previously. Using MIRRORB obtain ACCUM confirmation image
at nominal
focus and ACCUM images at alternate focus positions and
then perform an
ACQ/IMAGE and confirming image at nominal focus. Analyze
imagery, uplink
pointing offset as offset 11469A and adjust nominal focus
via patchable
constant uplinked with subsequent visit of this program;
update aperture
locations via modified SIAF file uplinked with subsequent
SMS. Use
updated focus and offset pointing as input for
NUV Optics Alignment and Focus) (note the SIAF update is
not a
prerequisite for COS 09 to proceed, but the pointing
offset and focus
update are).
STIS07/CCD 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.
STIS18/MA2/S/C 11351
NUV MAMA HV Recovery
This proposal addresses the concerns over Cesium migration
from the
NUV-MAMA photocathode into the pores of the microchannel
plate and lays
out the procedures necessary to permit a safe and
controlled recovery of
the NUV-MAMA detector to science. This procedure should
only be used
during the SMOV4 high voltage recommissioning phase for
the NUV-MAMA.
After, the normal ramping procedure should be used. This
proposal is
loosely based on proposal 10036, STIS MAMA Anomalous
Recovery, with the
differences summarized below: (1) additional plateaus
during voltage
commanding, (2) longer dwells after each 50 V step, (3)
intermediate
ramp re-structured into 2 parts, (4) change in yellow and
red limits and
the MCP Hi limit, setting new values for the next plateau,
and (5)
adding a fold test at 300V below the nominal MCP voltage.
The recovery
consists of four separate procedures (visits) and they
must be completed
successfully and in order. They are: (1) a signal
processing electronics
check, (2) 1st high voltage ramp-up to an intermediate MCP
voltage of
-1500 V with limits modifications and voltage plateaus,
(3) 2nd high
voltage ramp-up to an intermediate MCP voltage of -1750 V
(300 V below
the nominal MCP voltage) with limits modifications and
voltage plateaus
followed by a fold distribution test, and (4) a final high
voltage
ramp-up to the full operating voltage, again with limits
modifications
and voltage plateaus, followed by a fold distribution
test. During the
1st high voltage ramp-up, diagnostics are performed
followed by a dark
exposure. During the 2nd and 3rd high voltage ramp-ups,
diagnostics are
performed followed by a dark, flat field ACCUMs, and a
fold analysis
test. All required parameters are defined in 07-248 FUV and
NUV SMOV
Ramp-up Parameters Excel workbook. Supports Activity
STIS-18
WFC3/UVI 11422
SOFA Test
This proposal will verify the operation of all SOFA filter
wheels using
the default calsystem tungsten lamp. Internal flatfields
will be
obtained in one filter from each of the twelve filter
wheels,
establishing an initial baseline over a broad wavelength
range.
Subsequent proposals (e.g., WF19, proposal 11432) will
obtain full
internal flatfield coverage in all UVIS filters. Filters
for this
proposal were chosen based upon a balance of multiple
factors:
reasonable countrate with calsystem tungsten lamp (no long
exposure
times), science priority of the filter, overall coverage
of UVIS
wavelength regime, and slot location in the wheel. Exposures
will be
taken in the default full-frame, four-amp, unbinned
readout mode.
This proposal corresponds to SMOV activity id WFC3-09.
WFC3/S/C 11454
Activation Test
This program (WFC3 SMOV program WFC3-01) verifies that
WFC3 is in the
same condition after release from the Shuttle as during
the Functional
Test (FT), which was conducted with HST in the
Shuttle’s payload bay.
This analog test will be implemented in stored commanding
that will be
generated from a Phase II proposal, whereas the in-bay FT was
run with
real-time CCLs.
The purpose of the FT was to demonstrate that WFC3 is
viable for
scientific research. This was accomplished by
demonstrating that WFC3
can be commanded to the nominal scientific operating state
and can carry
out nominal scientific operations of the UVIS and IR
channels, including
operation of the thermoelectric coolers (TECs), corrector
and focus
mechanisms, UVIS shutter, SOFA and FSM filter wheels,
detectors, and
Control Section (CS). Only one Side of the CS is verified.
This test is compatible with execution during the post-FT,
Safe-Protect
period. Operability of the TECs is not demonstrated in
this test, but is
demonstrated in the SMOV Detector & TEC activation
programs, WFC3-04 and
WFC3-05.
WFC3/UVI 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: (None)
COMPLETED OPS NOTES: (None)
SCHEDULED
SUCCESSFUL
FGS
GSAcq
4
4
FGS
REAcq
3
3
OBAD with Maneuver
4
4
SIGNIFICANT EVENTS:
Flash Report:
At 162/2020 both WFC3 detectors had achieved their final
operational setpoints,
UVIS -83 C and IR -128 C.