HUBBLE
SPACE TELESCOPE - Continuing to Collect World Class Science
DAILY
REPORT #5133
PERIOD
COVERED: 5am July 7 - 5am July 8, 2010 (DOY 188/09:00z-189/09:00z)
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
5
5
FGS
REAcq
9
9
OBAD
with Maneuver 4
4
SIGNIFICANT
EVENTS: (None)
OBSERVATIONS
SCHEDULED:
ACS/WFC
11996
CCD
Daily Monitor (Part 3)
This
program comprises basic tests for measuring the read noise and dark
current
of the ACS WFC and for tracking the growth of hot pixels. The
recorded
frames are used to create bias and dark reference images for
science
data reduction and calibration. This program will be executed
four
days per week (Mon, Wed, Fri, Sun) for the duration of Cycle 17. To
facilitate
scheduling, this program is split into three proposals. This
proposal
covers 308 orbits (19.25 weeks) from 21 June 2010 to 1 November
2010.
COS/FUV
11686
The
Cosmological Impact of AGN Outflows: Measuring Absolute Abundances
and
Kinetic Luminosities
AGN
outflows are increasingly invoked as a major contributor to the
formation
and evolution of supermassive black holes, their host
galaxies,
the surrounding IGM, and cluster cooling flows. Our HST/COS
proposal
will determine reliable absolute chemical abundances in six AGN
outflows,
which influences several of the processes mentioned above. To
date
there is only one such determination, done by our team on Mrk 279
using
16 HST/STIS orbits and 100 ksec of FUSE time. The advent of COS
and
its high sensitivity allows us to choose among fainter objects at
redshifts
high enough to preclude the need for FUSE. This will allow us
to
determine the absolute abundances for six AGN (all fainter than Mrk
279)
using only 40 HST COS orbits. This will put abundances studies in
AGN
on a firm footing, an elusive goal for the past four decades. In
addition,
prior FUSE observations of four of these targets indicate that
it
is probable that the COS observations will detect troughs from
excited
levels of C III. These will allow us to measure the distances of
the
outflows and thereby determine their kinetic luminosity, a major
goal
in AGN feedback research.
11686( 7) - 25-Sep-2009 13:44:14 - [ 2]
We
will use our state of the art column density extraction methods and
velocity-dependent
photoionization models to determine the abundances
and
kinetic luminosity. Previous AGN outflow projects suffered from the
constraints
of deciding what science we could do using ONE of the
handful
of bright targets that were observable. With COS we can choose
the
best sample for our experiment. As an added bonus, most of the
spectral
range of our targets has not been observed previously, greatly
increasing
the discovery phase space.
COS/NUV/ACS/WFC/FUV
11658
Probing
the Outer Regions of M31 with QSO Absorption Lines
We
propose HST-COS spectroscopy of 10 quasars behind M31. Absorption
lines
due to MgII, FeII, CIV, and a variety of other lines will be
searched
for and measured. Six quasars lie between 1 and 4.2 Holmberg
radii
near the major axis on the southwest side, where confusion with
Milky
Way gas is minimized. Two lie even farther out on the southwest
side
of the major axis. One lies within 1 Holmberg radius. Two of the 10
pass
through M31's high velocity clouds seen in a detailed 21 cm
emission
map. Exposure time estimates were based on SDSS magnitudes and
available
GALEX magnitudes. Thus, using the most well-studied external
spiral
galaxy in the sky, our observations will permit us to check,
better
than ever before, the standard picture that quasar metal-line
absorption
systems such as MgII and CIV arise in an extended gaseous
halo/disk
of a galaxy well beyond its observable optical radius. The
observations
will yield insights into the nature of the gas and its
connection
to the very extended stellar components of M31 that have
recently
been studied. Notably the observations have the potential of
extending
M31's rotation curve to very large galactocentric distances,
thereby
placing new constraints on M31's dark matter halo.
Finally,
we also request that the coordinated parallel orbits be
allocated
to this program so that we may image the resolved stellar
content
of M31's halo and outer disk.
STIS/CC
11845
CCD
Dark Monitor Part 2
Monitor
the darks for the STIS CCD.
STIS/CC
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.
WFC3/IR/S/C
11929
IR
Dark Current Monitor
Analyses
of ground test data showed that dark current signals are more
reliably
removed from science data using darks taken with the same
exposure
sequences as the science data, than with a single dark current
image
scaled by desired exposure time. Therefore, dark current images
must
be collected using all sample sequences that will be used in
science
observations. These observations will be used to monitor changes
in
the dark current of the WFC3-IR channel on a day-to-day basis, and to
build
calibration dark current ramps for each of the sample sequences to
be
used by Gos in Cycle 17. For each sample sequence/array size
combination,
a median ramp will be created and delivered to the
calibration
database system (CDBS).
WFC3/UV/ACS/WFC
11710
The
Extreme Globular Cluster System of Abell 1689: The Ultimate Test of
Universal
Formation Efficiency
The
stellar masses of the most luminous galaxies poorly represent the
masses
of the halos in which they reside. However, recent studies of the
very
rich globular cluster (GC) populations in the centers of galaxy
clusters
point toward an apparently linear scaling of the number of GCs
with
the total core mass of the galaxy cluster. Thus, unlike for the
stars
in cD galaxies, GC formation in these systems appears to have
proceeded
with a roughly universal mass conversion efficiency. GCs are
also
distinct in that their spatial distributions are more extended than
the
starlight, and recent simulations suggest that they follow the mass
density
profile of the merged dark matter halos that formed stars at
high
redshift. To provide a definitive test of the universal efficiency
hypothesis
requires measuring the number of GCs in the most massive
galaxy
clusters, where the number should be a factor of 5 or more
greater
than seen in M87. Likewise, the relationship between GCs and
mass
density can only be tested in systems where the total mass and mass
density
are well-determined. Fortunately, the imaging power of HST
brings
the GC population of Abell 1689, the most extreme high-mass
lensing
cluster, into range. Estimates of the size of the A1689 GC
population
from available data suggest an unprecedented 100, 000 GCs,
but
this number is based on the tip of the iceberg and is extremely
uncertain.
We propose to obtain the first accurate measurement of the
number
of GCs and their density profile in this extraordinary system -
the
most massive and most distant GC system ever studied - and thus make
the
ultimate test of the universal GC formation hypothesis. Our deep
I-band
image will also provide a stringent "null-detection" test of
several
known z>7 galaxy candidates and improve the mass model of the
system
by increasing the number of usable lensed background galaxies.
Finally,
we will take deep multi-band parallel observations with WFC3/IR
to
help in quantifying the abundance of rare faint red objects.
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).
WFC3/UVIS
11908
Cycle
17: UVIS Bowtie Monitor
Ground
testing revealed an intermittent hysteresis type effect in the
UVIS
detector (both CCDs) at the level of ~1%, lasting hours to days.
Initially
found via an unexpected bowtie-shaped feature in flatfield
ratios,
subsequent lab tests on similar e2v devices have since shown
that
it is also present as simply an overall offset across the entire
CCD,
i.e., a QE offset without any discernable pattern. These lab tests
have
further revealed that overexposing the detector to count levels
several
times full well fills the traps and effectively neutralizes the
bowtie.
Each visit in this proposal acquires a set of three 3x3 binned
internal
flatfields: the first unsaturated image will be used to detect
any
bowtie, the second, highly exposed image will neutralize the bowtie
if
it is present, and the final image will allow for verification that
the
bowtie is gone.