HUBBLE SPACE TELESCOPE - Continuing to collect World
Class Science
DAILY REPORT #4883
PERIOD COVERED: 5am July 8 - 5am July 9, 2009 (DOY
189/0900z-190/0900z)
OBSERVATIONS SCHEDULED
ACS 11369
ACS CCD Functional Test for WFC
During the ACS Repair (ACS-R) conducted during Hubble
Servicing Mission
4 (SM4), astronauts will install a CCD Electronics Box
Replacement
(CEB-R) and Low-Voltage Power Supply Replacement (LVPS-R). A
rudimentary
aliveness/functional test (AT/FT) will be conducted on-orbit
during SM4.
Shortly after SM4, the more comprehensive CCD function test (FT)
defined
in this program will be conducted as part of SMOV. This program
is
modeled after the original CCD functional test (HST program 9005,
PI
Mark Clampin) conducted following the initial installation of ACS
during
Hubble Servicing Mission 3B. This WFC-only proposal has a companion
HRC
proposal 11396.
ACS 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.
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 - COS to FGS Alignment
(NUV)).
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.
WFC3 11426
UVIS SMOV Contamination Monitor
The UV throughput of WFC3 during SMOV is monitored via
weekly standard
star observations in a subset of key filters (as many as will
fit into a
single orbit but to include at a minimum F218W, F225W, F275W,
and
F606W). The data will provide a measure of throughput levels as
a
function of time and wavelength, allowing for detection of the
presence
of possible contaminants. In addition, a small set of internal
exposures
are included with the externals, to provide verification of
detector
stability.
This proposal corresponds to activity WFC3-13.
WFC3 11434
WFC3 UVIS Fine Alignment
The corrector mechanism will be used to bring the UVIS
channel of WFC3
into optimal alignment with the OTA using analysis of star
images over
the field. Two visits are required; corrector offsets will be
uplinked
after each visit via realtime command.
This proposal is activity id WFC3-21
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:
11922 - STIS suspended during checkout of MIE
at 190/06:19:48z.
11923 - REAcq(2,3,3) failed to RGA control at
190/08:35:52z.
Observations affected: ACS 137-140 Proposal
ID#11510,
WFC3 55-57 Proposal ID#11432
COMPLETED OPS REQUEST:
18598-1 - Update COS
Aperture and OSM Positions in FSW @ 189/1502z
18599-3 - Transition STIS from
Suspend to Operate & Check MIE @ 190/0620z
18608-0 - Dump STIS Memory
after Suspend on day 190 @ 190/0704z
COMPLETED OPS NOTES: (None)
SCHEDULED SUCCESSFUL
FGS
GSAcq
9
9
FGS REAcq
8 7
OBAD with Maneuver
7
7
SIGNIFICANT EVENTS:
Flash Report:
During Ops Request 18599 to verify the
functionality of the STIS MIE and
recover STIS to Operate mode, STIS
Suspended at 190/06:19:48z due to a
STIS STB 100 "Invalid CS FSW Mode for
more than 10 minor frames".
Science loss due to HSTAR #11917: STIS #23-27 for
Proposal #11404 & STIS
#28 for Proposal
#11567.