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#48647
Wed 02 Jun 2010 03:19:AM
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Joined: Feb 2001
Posts: 381,903
Launch Director
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OP
Launch Director
Joined: Feb 2001
Posts: 381,903 |
HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science
DAILY REPORT #5108
PERIOD COVERED: 5am June 1 - 5am June 2, 2010 (DOY 152/09:00z-153/09:00z)
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 8 8
FGS REAcq 5 5
OBAD with Maneuver 6 6
SIGNIFICANT EVENTS: (None)
OBSERVATIONS SCHEDULED:
ACS/WFC 11995
CCD Daily Monitor (Part 2)
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 320 orbits (20 weeks) from 1 February 2010 to 20 June
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. 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/FUV 11692
The LMC as a QSO Absorption Line System
We propose to obtain high resolution, high signal-to-noise observations
of QSOs behind the Large Magellanic Clouds. These QSOs are situated
beyond the star forming disk of the galaxy, giving us the opportunity to
study the distribution of metals and energy in regions lacking
significant star formation. In particular, we will derive the
metallicities and study the ionization characteristics of LMC gas at
impact parameters 3-17 kpc. We will compare our results with high-z QSO
absorption line systems.
FGS 11704
The Ages of Globular Clusters and the Population II Distance Scale
Globular clusters are the oldest objects in the universe whose age can
be accurately determined. The dominant error in globular cluster age
determinations is the uncertain Population II distance scale. We propose
to use FGS 1r to obtain parallaxes with an accuracy of 0.2
milliarcsecond for 9 main sequence stars with [Fe/H] < -1.5. This will
determine the absolute magnitude of these stars with accuracies of 0.04
to 0.06mag. This data will be used to determine the distance to 24
metal-poor globular clusters using main sequence fitting. These
distances (with errors of 0.05 mag) will be used to determine the ages
of globular clusters using the luminosity of the subgiant branch as an
age indicator. This will yield absolute ages with an accuracy 5%, about
a factor of two improvement over current estimates. Coupled with
existing parallaxes for more metal-rich stars, we will be able to
accurately determine the age for globular clusters over a wide range of
metallicities in order to study the early formation history of the Milky
Way and provide an independent estimate of the age of the universe.
The Hipparcos database contains only 1 star with [Fe/H] < -1.4 and an
absolute magnitude error less than 0.18 mag which is suitable for use in
main sequence fitting. Previous attempts at main sequence fitting to
metal-poor globular clusters have had to rely on theoretical
calibrations of the color of the main sequence. Our HST parallax program
will remove this source of possible systematic error and yield distances
to metal-poor globular clusters which are significantly more accurate
than possible with the current parallax data. The HST parallax data will
have errors which are 10 times smaller than the current parallax data.
Using the HST parallaxes, we will obtain main sequence fitting distances
to 11 globular clusters which contain over 500 RR Lyrae stars. This will
allow us to calibrate the absolute magnitude of RR Lyrae stars, a
commonly used Population II distance indicator.
FGS 11788
The Architecture of Exoplanetary Systems
Are all planetary systems coplanar? Concordance cosmogony makes that
prediction. It is, however, a prediction of extrasolar planetary system
architecture as yet untested by direct observation for main sequence
stars other than the Sun. To provide such a test, we propose to carry
out FGS astrometric studies on four stars hosting seven companions. Our
understanding of the planet formation process will grow as we match not
only system architecture, but formed planet mass and true distance from
the primary with host star characteristics for a wide variety of host
stars and exoplanet masses.
We propose that a series of FGS astrometric observations with
demonstrated 1 millisecond of arc per-observation precision can
establish the degree of coplanarity and component true masses for four
extrasolar systems: HD 202206 (brown dwarf+planet); HD 128311
(planet+planet), HD 160691 = mu Arae (planet+planet), and HD 222404AB =
gamma Cephei (planet+star). In each case the companion is identified as
such by assuming that the minimum mass is the actual mass. For the last
target, a known stellar binary system, the companion orbit is stable
only if coplanar with the AB binary orbit.
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.
WFC3/IR 11712
Calibration of Surface Brightness Fluctuations for WFC3/IR
We aim to characterize galaxy surface brightness fluctuations (SBF), and
calibrate the SBF distance method, in the F110W and F160W filters of the
Wide Field Camera 3 IR channel. Because of the very high throughput of
F110W and the good match of F160W to the standard H band, we anticipate
that both of these filters will be popular choices for galaxy
observations with WFC3/IR. The SBF signal is typically an order of
magnitude brighter in the near-IR than in the optical, and the
characterisitics (sensitivity, FOV, cosmetics) of the WFC3/IR channel
will be enormously more efficient for SBF measurements than previously
available near-IR cameras. As a result, our proposed SBF calibration
will allow accurate distance derivation whenever an early-type or
bulge-dominated galaxy is observed out to a distance of 150 Mpc or more
(i.e., out to the Hubble flow) in the calibrated passbands. For
individual galaxy observations, an accurate distance is useful for
establishing absolute luminosities, black hole masses, linear sizes,
etc. Eventually, once a large number of galaxies have been observed
across the sky with WFC3/IR, this SBF calibration will enable accurate
mapping of the total mass density distribution in the local universe
using the data available in the HST archive. The proposed observations
will have additional important scientific value; in particular, we
highlight their usefulness for understanding the nature of multimodal
globular cluster color distributions in giant elliptical galaxies.
WFC3/IR 11915
IR Internal Flat Fields
This program is the same as 11433 (SMOV) and depends on the completion
of the IR initial alignment (program 11425). This version contains three
instances of 37 internal orbits; to be scheduled early, middle, and near
the end of Cycle 17, in order to use the entire 110-orbit allocation.
In this test, we will study the stability and structure of the IR
channel flat field images through all filter elements in the WFC3-IR
channel. Flats will be monitored, i.e. to capture any temporal trends in
the flat fields, and delta flats produced. High signal observations will
provide a map of the pixel-to-pixel flat field structure, as well as
identify the positions of any dust particles.
WFC3/UVI 11556
Investigations of the Pluto System
We propose a set of high SNR observations of the Pluto system that will
provide improved lightcurves, orbits, and photometric properties of Nix
and Hydra. The key photometric result for Nix and Hydra will be a vastly
improved lightcurve shape and rotation period to test if the objects are
in synchronous rotation or not. A second goal of this program will be to
retrieve a new epoch of albedo map for the surface of Pluto. These
observations will also improve masses and in some case densities for the
bodies in the Pluto system.
WFC3/UVI 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<BR>and dark frames. A smaller set of 2Kx4K
subarray biases are acquired at less frequent intervals<BR>throughout
the cycle to support subarray science observations. The internals from
this proposal,<BR>along with those from the anneal procedure (11909),
will be used to generate the necessary superbias<BR>and superdark
reference files for the calibration pipeline (CDBS).
WFC3/UVI 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.
David Cottle
UBB Owner & Administrator
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