HUBBLE
SPACE TELESCOPE - Continuing to Collect World Class Science
DAILY
REPORT #5167
PERIOD
COVERED: 5am August 24 - 5am August 25, 2010 (DOY 236/09:00z-237/09:00z)
FLIGHT
OPERATIONS SUMMARY:
Significant
Spacecraft Anomalies: (The following are preliminary reports
of
potential non-nominal performance that will be investigated.)
HSTARS:
For
DOY 221:
12362
- GSAcq(2,1,1) at 221/23:59:30z required two attempts to achieve CT-DV on FGS2.
Observations possibly affected: STIS 12 Proposal ID#11568
COMPLETED
OPS REQUEST: (None)
COMPLETED
OPS NOTES: (None)
SCHEDULED
SUCCESSFUL
FGS
GSAcq
04
04
FGS
REAcq
11
11
OBAD
with Maneuver
03
03
SIGNIFICANT
EVENTS: (None)
OBSERVATIONS
SCHEDULED:
STIS/CCD
11845
CCD
Dark Monitor Part 2
Monitor
the darks for the STIS CCD.
STIS/CCD
11847
CCD
Bias Monitor-Part 2
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.
STIS/MA1/MA2
11857
STIS
Cycle 17 MAMA Dark Monitor
This
proposal monitors the behavior of the dark current in each of the
MAMA
detectors.
The
basic monitor takes two 1380s ACCUM darks each week with each
detector.
However, starting Oct 5, pairs are only included for weeks
that
the LRP has external MAMA observations planned. The weekly pairs of
exposures
for each detector are linked so that they are taken at
opposite
ends of the same SAA free interval. This pairing of exposures
will
make it easier to separate long and short term temporal variability
from
temperature dependent changes.
For
both detectors, additional blocks of exposures are taken once every
six
months. These are groups of five 1314s FUV-MAMA Time-Tag darks or
five
3x315s NUV ACCUM darks distributed over a single SAA-free interval.
This
will give more information on the brightness of the FUV MAMA dark
current
as a function of the amount of time that the HV has been on, and
for
the NUV MAMA will give a better measure of the short term
temperature
dependence.
WFC3/IR/ACS/WFC
12331
Massive
Star CSI: Has The Progenitor of SN2008S Vanished?
SN2008S
in NGC6946 is the prototype of a new class of optical
transients.
Its luminosity was low for a Type II supernova, and the
progenitor
star was identified as a completely dust obscured log
(L/Lsun)=4.5,
T=440K massive star (~10 Msun) in archival Spitzer data.
It
is uncertain whether this is a new class of low-luminosity supernova
(e.g.
an electron capture supernova) or a new class of massive star
outburst.
The transient has now faded to the point where the source is
again
invisible in the optical. Near-IR detections are consistent with a
somewhat
hotter source, T~1200K, somewhat brighter than the progenitor
and
still fading at ~3 mag/year. Using two epochs of IRAC observations
to
constrain the mid-IR emission, and two epochs of HST H-band/J-band
observations
to constrain emission from cool stars, we will solve this
mystery
by either identifying and characterizing the surviving
progenitor
or ruling out its survival.
WFC3/UV
11638
Illuminating
the HI Structure of a Proto-cluster Region at z=2.84
We
propose very deep intermediate-band Lyman alpha imaging in the field
of
a newly-discovered proto-cluster region surrounding the extremely
luminous
QSO HS1549+19 at z=2.844. The large structure, initially
discovered
in a spectroscopic survey of galaxies in fields surrounding
the
brightest QSOs at z=2.5-2.8, represents an ideal laboratory for
studying
the response of the intergalactic medium to a source of
ionizing
photons that exceeds the UV background by factors >1000. Within
a
single pointing of WFC3-UVIS there are already more than 45 known
Lyman
alpha emitters, most of which are already spectroscopically
confirmed,
and at least 3 of which are giant ``Lyman alpha blobs''. Many
of
the objects have properties similar to those expected from the
process
of fluorescence, in which Lyman alpha emission is induced by the
UV
radiation field of the QSO in any HI gas that dense enough to remain
partially
self-shielded. Fortuitously, the F467M filter (Stromgren "b")
in
WFC3-UVIS is a perfect match to Lyman alpha at z=2.844. In
combination
with an equally deep broad-band continuum image, the
observations
will allow the construction of a Lyman alpha map tracing
dense
gas throughout the inner parts of a proto-cluster region at
sub-kpc
resolution. The ability to measure the spatial sub-structure and
surface
brightness distribution of Lya emission, relative to known
protocluster
galaxies and AGN, will illuminate the “cosmic web'' in a
dense
region caught in a violent stage of formation.
WFC3/UVIS
11905
WFC3
UVIS CCD Daily Monitor
The
behavior of the WFC3 UVIS CCD will be monitored daily with a set of
full-frame,
four-amp bias and dark frames. A smaller set of 2Kx4K
subarray
biases are acquired at less frequent intervals throughout the
cycle
to support subarray science observations. The internals from this
proposal,
along with those from the anneal procedure (Proposal 11909),
will
be used to generate the necessary superbias and superdark reference
files
for the calibration pipeline (CDBS).