HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 4159
PERIOD COVERED: UT July 19, 2006 (DOY 200)
OBSERVATIONS SCHEDULED
ACS/HRC 10512
Search for Binaries Among Faint Jupiter Trojan Asteroids
We propose an ambitious SNAPSHOT program to survey faint Jupiter
Trojan
asteroids for binary companions. We target 150 objects, with the
expectation of acquiring data on about 50%. These objects span Vmag
=
17.5-19.5, a range inaccessible with ground-based adaptive optics.
We
now have a significant sample from our survey of brighter Trojans to
suggest that the binary fraction is similar to that which we find
among
brighter main-belt asteroids, roughly 2%. However, our observations
suggest a higher binary fraction for smaller main-belt asteroids,
probably the result of a different formation mechanism {evident also
from the physical characteristics of the binaries}. Because the
collision environment among the Trojans is similar to that of the
Main
Belt, while the composition is likely to be very different, sampling
the
binary fraction among the fainter Trojans should help us understand
the
collisional and binary formation mechanisms at work in various
populations, including the Kuiper Belt, and help us evaluate
theories
for the origin of the Trojans. Calibration of and constraints on
models
of binary production and collisional evolution can only be done
using
these large-scale, real-life physical systems that we are beginning
now
to find and utilize.
ACS/HRC 10598
ACS Imaging of Fomalhaut: A Rosetta Stone for Debris Disks Sculpted
by
Planets
The Sun and roughly 15% of stars are surrounded by dust disks
collisionally replenished by asteroids and comets. Disk structure can
be
directly tied to the dynamical influence of more massive bodies such
as
planets. For example, planetary perturbations offset the center of
our
zodiacal dust disk ~0.01 AU away from the Sun and also maintain a ~40
AU
radius inner edge to our Kuiper Belt. Here we propose follow-up
observation to the first optical detection of reflected light from
dust
grains surrounding the nearby star Fomalhaut using HST/ACS. We find
a
belt of material between 133 and 158 AU radius that has a center
position offset ~15 AU from the stellar position, and with a sharp
inner
edge. A tenuous dust component interior to the belt is also detected
in
the southeast. Given Fomalhaut's proximity to the Sun {7.7 pc},
these
images represent the closest and highest angular resolution view of
an
extrasolar analog to our Kuiper Belt. The center of symmetry offset
and
the sharp inner edge of Fomalhaut's belt are evidence for
planet-mass
objects orbiting the star as predicted by dynamical theory and
simulations. We propose comprehensive follow-up ACS imaging to fully
exploit this discovery and map the disk around its entire
circumference
with higher signal-to-noise and at multiple wavelengths. HST/ACS is
certainly the only facility capable of performing this relatively
wide
field optical study at high contrast ratios and diffraction-limited
resolution. The Cycle 14 data will provide key measurements of belt
width as a function of azimuth, the scattered light color of the
belt
versus the inner dust component, and the azimuthal structure of the
belt. These data will be used to constrain dynamical models of
resonances and shepherding that ultimately elucidate the dynamical
properties of planet-mass objects in the system.
ACS/HRC 10627
A Snapshot Survey of Post-AGB Objects and Proto-Planetary Nebulae
We propose an ACS/HRC snapshot survey of 50 post-AGB sources,
objects
which have evolved from the AGB but may or may not become planetary
nebulae {PNe}. This survey will complement existing HST images of
proto-planetary nebulae {PPNe} and PNe in addressing circumstellar
envelope morphology as a function of: 1} the progenitor star mass;
2}
the chemical composition; and 3} evolutionary stage. We will connect
the
observed diversity of nebualar shapes with the main physical and
chemical conditions characterizing post-AGB objects, to identify the
mechanism that breaks the symmetry of AGB mass loss. To our
knowledge,
no previous HST projects have been specifically designed to address
this
issue. From our database of 360 post-AGB candidates, we have
selected
approximately 50 targets, none of which have been or are being
observed
with HST, to sample different central star masses, chemical
compositions, and evolutionary stages, uniformly across the sky.
These
new data will also provide important constraints to a quantitative
analysis of Spitzer Space Telescope {SST} observations planned for a
similar sample of objects. We will model the HST images and SST
spectra
using our axisymmetric dust code 2-Dust, to derive dust density
distributions, pole to equator density ratios, dust shell masses,
inclination angles as well as dust composition.
ACS/HRC/WFC 10758
ACS CCDs daily monitor
This program consists of a set of basic tests to monitor, the read
noise, the development of hot pixels and test for any source of noise
in
ACS CCD detectors. The files, biases and dark will be used to create
reference files for science calibration. This programme will be for
the
entire lifetime of ACS. Changes from cycle 13:- The default gain for
WFC
is 2 e- /DN. As before bias frames will be collected for both gain 1
and
gain 2. Dark frames are acquired using the default gain {2}. This
program cover the period May, 31 2006- Oct, 1- 2006. The first half
of
the program has a different proposal number: 10729.
ACS/WFC 10626
A Snapshot Survey of Brightest Cluster Galaxies and Strong Lensing to
z
= 0.9
We propose an ACS/WFC snapshot survey of the cores of 150 rich
galaxy
clusters at 0.3 < z < 0.9 from the Red Sequence Cluster Survey
{RCS}. An
examination of the galaxian light in the brightest cluster galaxies,
coupled with a statistical analysis of the strong- lensing properties
of
the sample, will allow us to contrain the evolution of both the
baryonic
and dark mass in cluster cores, over an unprecedented redshift range
and
sample size. In detail, we will use the high-resolution ACS images
to
measure the metric {10 kpc/h} luminosity and morphological
disturbances
around the brightest clusters galaxies, in order to calibrate their
accretion history in comparison to recent detailed simulations of
structure formation in cluster cores. These images will also yield a
well-defined sample of arcs formed by strong lensing by these
clusters;
the frequency and detailed distribution {size, multiplicity,
redshifts}
of these strong lens systems sets strong constraints on the total
mass
content {and its structure} in the centers of the clusters. These
data
will also be invaluable in the study of the morphological evolution
and
properties of cluster galaxies over a significant redshift range.
These
analyses will be supported by extensive ongoing optical and
near-infrared imaging, and optical spectroscopy at Magellan, VLT and
Gemini telescopes, as well as host of smaller facilities.
CAL/ACS 10735
SBC MAMA Recovery
This proposal is designed for the initial turn-on of the ACS MAMA
detector and to permit recovery after an anomalous shutdown.
Anomalous
shutdowns can occur as a result of bright object violations which
trigger the Bright Scene Detection or Software Global Monitors.
Anomalous shutdowns can also occur as a result of MAMA hardware
problems. The Initial MAMA turn-on/recovery from anomalous shutdown
consists of three tests: a signal processing electronics check, high
voltage ramp-up to an intermediate voltage, and high voltage ramp-up
to
the full operating voltage. During each of the two high voltage
ramp-ups, diagnostics are performed during a dark ACCUM. The turn-on
is
followed by a MAMA Fold Analysis .
NIC1/NIC2/NIC3 8794
NICMOS Post-SAA calibration - CR Persistence Part 5
A new procedure proposed to alleviate the CR-persistence problem of
NICMOS. Dark frames will be obtained immediately upon exiting the
SAA
contour 23, and every time a NICMOS exposure is scheduled within 50
minutes of coming out of the SAA. The darks will be obtained in
parallel
in all three NICMOS Cameras. The POST-SAA darks will be non-
standard
reference files available to users with a USEAFTER date/time mark.
The
keyword 'USEAFTER=date/time' will also be added to the header of
each
POST-SAA DARK frame. The keyword must be populated with the time, in
addition to the date, because HST crosses the SAA ~8 times per day
so
each POST-SAA DARK will need to have the appropriate time specified,
for
users to identify the ones they need. Both the raw and processed
images
will be archived as POST-SAA DARKSs. Generally we expect that all
NICMOS
science/calibration observations started within 50 minutes of leaving
an
SAA will need such maps to remove the CR persistence from the
science
images. Each observation will need its own CRMAP, as different SAA
passages leave different imprints on the NICMOS detectors.
NIC2 10906
The Fundamental Plane of Massive Gas-Rich Mergers: II. The QUEST QSOs
We propose deep NICMOS H-band imaging of a carefully selected sample
of
23 local QSOs. This program is the last critical element of a
comprehensive investigation of the most luminous mergers in the
nearby
universe, the ultraluminous infrared galaxies {ULIRGs} and the
quasars.
This effort is called QUEST: Quasar / ULIRG Evolutionary STudy. The
high-resolution HST images of the QUEST QSOs will complement an
identical set of images on the ULIRG sample obtained during Cycle 12,
an
extensive set of ground-based data that include long-slit NIR
spectra
from a Large VLT Program, and a large set of mid-infrared spectra from
a
Cycle 1 medium-size program with Spitzer. This unique dataset will
allow
us to derive with unprecedented precision structual, kinematic, and
activity parameters for a large unbiased sample of objects spanning
the
entire ULIRG/QSO luminosity function. These data will refine the
fundamental plane of massive gas-rich mergers and enable us to
answer
the following quesitons: {1} Do ultraluminous mergers form
elliptical
galaxies, and in particular, giant ellipticals? {2} Do ULIRGs evolve
into optical bright QSOs? The results from this detailed study of
massive mergers in the local universe will be relevant to
understanding
the basic physical processes involved in creating massive early-type
host on the one hand, and growing/feeding embedded massive black
holes
on the other, in major galaxy mergers. This is an important question
since 50% of cosmic star formation at high-z and most of the big BHs
appear to be formed in this process.
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:
#17859-0 GenSlew for Proposal 10487 slot#3 @200/18:51z
#17860-0 GenSlew for Proposal 10487 slot#4 @200/18:53z
COMPLETED OPS NOTES: (None)
SCHEDULED
SUCCESSFUL
FGS
GSacq
13
13
FGS
REacq
00
00
OBAD with Maneuver
26
26
SIGNIFICANT EVENTS: (None)
-Lynn
Lynn F. Bassford
CHAMP HST Missions Operations Manager
Lockheed Martin Technical Operations
GSFC PH#: 301-286-2876
"The Hubble Space Telescope is the Babe Ruth of astronomical
observatories, the Muhammad Ali of cosmic photography
"
- Robert Roy Britt, space.com 7-14-4
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