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Daily Report #5124



 
 
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Old June 24th 10, 02:57 PM posted to sci.astro.hubble
Cooper, Joe
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Default Daily Report #5124

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5124

PERIOD COVERED: 5am June 23 - 5am June 24, 2010 (DOY 174/09:00z-175/09:00z)

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 6 6
FGS REAcq 9 9
OBAD with Maneuver 6 6

SIGNIFICANT EVENTS: (None)



OBSERVATIONS SCHEDULED:

ACS/WFC 11655

Dynamics of the Galactic Bulge/bar

We request second-epoch ACS observations of four star fields in the
Galactic bar. These will allow us to measure proper motions for tens
of thousands of stars well below the turnoff, to construct a dynamical
model for the bulge/bar (in combination with data already in hand from
other HST fields, and from VLT spectroscopy), and hence to take a
unique look at the internal dynamical structure of the central regions
of our Galaxy. By relating the kinematics with stellar population we
can elucidate the formation history of the bulge and bar, and their
relation to the surrounding Galactic disk. This is a resubmission of
an approved Cycle 15 proposal that was hit by the ACS malfunction.

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 11541

COS-GTO: Cool, Warm, and Hot Gas in the Cosmic Web and in Galaxy Halos

COS G130M and G160M 20, 000 resolution observations will be obtained
for 17 QSOs to study cool, warm and hot gas in the cosmic web and in
galaxy halos. 5 QSOs with z from 0.177 to 0.574 and sum z = 1.68 will
be observed with S/N = 40-50 per resolution element. 12 QSOs with z =
0.286 to 0.669 and sum z = 5.57 will be observed with S/N = 30-40. The
observations will allow a wide range of IGM studies including
determining the frequency of occurrence of the different types of
absorption systems detected, along with studies of the physical
conditions and elemental abundances in the different systems. Special
emphasis will be given to a study of the properties of highly ionized
IGM as traced by O VI, O V, O IV, N V, and C IV. The high S/N of the
observations will allow a search for broad Lyman alpha absorption and
weak metal line absorption that can be crucial for the evaluation of
physical conditions and elemental abundances. Supporting ground based
observations will allow studies of the association of the absorbers
with galaxy structures along the 17 lines of sight. The overall goal
of the program will be to obtain the information that will allow an
assessment of the baryonic content of the IGM as revealed by UV and
EUV absorption lines seen in the spectra of QSOs.

COS/NUV/FUV 11698

The Structure and Dynamics of Virgo's Multi-Phase Intracluster Medium

The dynamical flows of the intracluster medium (ICM) are largely
unknown. We propose to map the spatial and kinematic distribution of
the warm ICM of the nearby Virgo cluster using the Cosmic Origins
Spectrograph. 15 sightlines at a range of impact parameters within the
virial radius of the cluster (0.2 - 1.7 Mpc) will be probed for
Lyman-alpha absorption and the data compared to blind HI, dust and
x-ray surveys to create a multi-phase map of the cluster's ICM.
Absorption line sightlines are commonly 40-100 kpc from a galaxy,
allowing the flow of baryons between galaxies and the ICM to be
assessed. The velocity distribution of the absorbers will be directly
compared to simulations and used to constrain the turbulent motions of
the ICM. This proposal will result in the first map of a cluster's
warm ICM and provide important tests for our theoretical understanding
of cluster formation and the treatment of gas cooling in cosmological
simulations.

STIS/CC 11693

Follow-up Observations of Debris Disks around Two Solar-Type Stars

Circumstellar debris disks offer direct views into the structure of
extrasolar planetary systems. Their constituent dust, seen in
scattered light and thermal emission, is created by the collisions of
asteroidal and cometary parent bodies. The distribution of this dust
provides information on the location of the parent bodies, and can be
strongly affected by planetary perturbations. Dynamical signatures of
planets can include asymmetries, warps, central clearings, and radial
gaps in a disk, and thus are key features to search for in resolved
images. Following up recent Spitzer measurements, we have now detected
two new, nearby debris disks in scattered light. Our initial ACS F606W
coronagraphic images show faint ringlike structures around the
solar-type stars HD 10647 (F9V) and HD 207129 (G0V); both are also
spatially resolved in Spitzer/MIPS 70 micron images. The HD 10647
disk, seen close to edge-on, represents the first disk ever imaged in
scattered light around a star known to have a radial velocity planet.
The inclined ring around HD 207129 is the faintest disk ever imaged in
scattered light, and seems in the MIPS image to be asymmetric like the
eccentric ring around Fomalhaut. We propose to obtain deep ACS
coronagraphic images of these two disks. Our goals are to get
definitive measurements of the dust spatial distributions (including
disk asymmetries and sharpness of the ring edges), and measure the
overall F606W-F814W color of each disk in order to constrain the dust
properties. The results will be a definitive exploration of the Kuiper
belts of two nearby, Sun-like stars. NOTE: HD 207129 was deleted from
this program.

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.

STIS/CCD/MA1/MA2 11860

MAMA Spectroscopic Sensitivity and Focus Monitor

The purpose of this proposal is to monitor the sensitivity of each
MAMA grating mode to detect any change due to contamination or other
causes, and to also monitor the STIS focus in a spectroscopic and an
imaging mode.

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/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/UVIS/IR 11644

A Dynamical-Compositional Survey of the Kuiper Belt: A New Window Into
the Formation of the Outer Solar System

The eight planets overwhelmingly dominate the solar system by mass,
but their small numbers, coupled with their stochastic pasts, make it
impossible to construct a unique formation history from the dynamical
or compositional characteristics of them alone. In contrast, the huge
numbers of small bodies scattered throughout and even beyond the
planets, while insignificant by mass, provide an almost unlimited
number of probes of the statistical conditions, history, and
interactions in the solar system. To date, attempts to understand the
formation and evolution of the Kuiper Belt have largely been dynamical
simulations where a hypothesized starting condition is evolved under
the gravitational influence of the early giant planets and an attempt
is made to reproduce the current observed populations. With little
compositional information known for the real Kuiper Belt, the test
particles in the simulation are free to have any formation location
and history as long as they end at the correct point. Allowing
compositional information to guide and constrain the formation,
thermal, and collisional histories of these objects would add an
entire new dimension to our understanding of the evolution of the
outer solar system. While ground based compositional studies have hit
their flux limits already with only a few objects sampled, we propose
to exploit the new capabilities of WFC3 to perform the first ever
large-scale dynamical-compositional study of Kuiper Belt Objects
(KBOs) and their progeny to study the chemical, dynamical, and
collisional history of the region of the giant planets. The
sensitivity of the WFC3 observations will allow us to go up to two
magnitudes deeper than our ground based studies, allowing us the
capability of optimally selecting a target list for a large survey
rather than simply taking the few objects that can be measured, as we
have had to do to date. We have carefully constructed a sample of 120
objects which provides both overall breadth, for a general
understanding of these objects, plus a large enough number of objects
in the individual dynamical subclass to allow detailed comparison
between and within these groups. These objects will likely define the
core Kuiper Belt compositional sample for years to come. While we have
many specific results anticipated to come from this survey, as with
any project where the field is rich, our current knowledge level is
low, and a new instrument suddenly appears which can exploit vastly
larger segments of the population, the potential for discovery -- both
anticipated and not -- is extraordinary.

WFC3/UVIS/IR 11909

UVIS Hot Pixel Anneal

The on-orbit radiation environment of WFC3 will continually generate
new hot pixels. This proposal performs the procedure required for
repairing those hot pixels in the UVIS CCDs. During an anneal, the
two-stage thermo-electric cooler (TEC) is turned off and the
four-stage TEC is used as a heater to bring the UVIS CCDs up to ~20
deg. C. As a result of the CCD warmup, a majority of the hot pixels
will be fixed; previous instruments such as WFPC2 and ACS have seen
repair rates of about 80%. Internal UVIS exposures are taken before
and after each anneal, to allow an assessment of the procedure's
effectiveness in WFC3, provide a check of bias, global dark current,
and hot pixel levels, as well as support hysteresis (bowtie)
monitoring and CDBS reference file generation. One IR dark is taken
after each anneal, to provide a check of the IR detector.


 




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