Notice: For the foreseeable future, the daily reports may
contain
apparent discrepancies between some proposal descriptions
and the listed
instrument usage. This is due to the conversion of
previously approved
ACS WFC or HRC observations into WFPC2, or NICMOS
observations
subsequent to the loss of ACS CCD science capability in
late January.
HUBBLE SPACE TELESCOPE - Continuing to collect World Class
Science
DAILY REPORT # 4367
PERIOD COVERED: UT May 21, 2007 (DOY 141)
OBSERVATIONS SCHEDULED
WFPC2 10800
Kuiper Belt Binaries: Probes of Early Solar System
Evolution
Binaries in the Kuiper Belt are a scientific windfall: in
them we have
relatively fragile test particles which can be used as tracers
of the
early dynamical evolution of the outer Solar System. We
propose to
continue a Snapshot program using the ACS/HRC that has a
demonstrated
discovery potential an order of magnitude higher than the
HST
observations that have already discovered the majority of
known
transneptunian binaries. With this continuation we seek to
reach the
original goals of this project: to accumulate a
sufficiently large
sample in each of the distinct populations collected in
the Kuiper Belt
to be able to measure, with statistical significance, how
the fraction
of binaries varies as a function of their particular
dynamical paths
into the Kuiper Belt. Today's Kuiper Belt bears the
imprints of the
final stages of giant-planet building and migration;
binaries may offer
some of the best preserved evidence of that long-ago era.
WFPC2 10832
Solving the microlensing puzzle: An HST high-resolution
imaging approach
We propose to use the HST Advanced Camera for Surveys High
Resolution
Channel to obtain high resolution imaging data for 10
bona-fide LMC
microlensing events seen in the original MACHO survey. The
purpose of
this survey will be to assess whether or not the lens and
source stars
have separated enough to be resolved since the original
microlensing
event took place - about a decade has passed since the
original MACHO
survey and the HST WFPC2 follow-up observations of the
microlensing
events. If the components of the lensing event are
resolved, we will
determine the apparent magnitude and color of both the
lens and the
source stars. These data, in combination with Spitzer/IRAC
data and
Magellan near-IR JHK data, will be used to ascertain the
basic
properties of the lens stars. With the majority of the
microlensing
events in the original MACHO survey observed at the highest
spatial
resolution currently possible, we will be able to draw
important
conclusions as to what fraction of these events have
lenses which belong
to some population of dwarf stars in the disk and what
fraction must be
due to lenses in the halo or beyond. These data will
greatly increase
our understanding of the structure of the Galaxy by
characterizing the
stellar population responsible for the gravitational
microlensing.
ACS/SBC 10862
Comprehensive Auroral Imaging of Jupiter and Saturn during
the
International Heliophysical Year
A comprehensive set of observations of the auroral
emissions from
Jupiter and Saturn is proposed for the International
Heliophysical Year
in 2007, a unique period of especially concentrated
measurements of
space physics phenomena throughout the solar system. We
propose to
determine the physical relationship of the various auroral
processes at
Jupiter and Saturn with conditions in the solar wind at
each planet.
This can be accomplished with campaigns of observations,
with a sampling
interval not to exceed one day, covering at least one
solar rotation.
The solar wind plasma density approaching Jupiter will be
measured by
the New Horizons spacecraft, and a separate campaign near
opposition in
May 2007 will determine the effect of large-scale
variations in the
interplanetary magnetic field {IMF} on the Jovian aurora
by
extrapolation from near-Earth solar wind measurements. A
similar Saturn
campaign near opposition in Jan. 2007 will combine
extrapolated solar
wind data with measurements from a wide range of locations
within the
Saturn magnetosphere by Cassini. In the course of making
these
observations, it will be possible to fully map the auroral
footprints of
Io and the other satellites to determine both the local
magnetic field
geometry and the controlling factors in the
electromagnetic interaction
of each satellite with the corotating magnetic field and
plasma density.
Also in the course of making these observations, the
auroral emission
properties will be compared with the properties of the
near-IR
ionospheric emissions {from ground- based observations}
and non thermal
radio emissions, from ground-based observations for
Jupiter?s decametric
radiation and Cassini plasma wave measurements of the
Saturn Kilometric
Radiation {SKR}.
NIC2 10858
NICMOS Imaging of the z ~ 2 Spitzer Spectroscopic Sample
of
Ultraluminous Infrared Galaxies
We propose to obtain NICMOS images of the first large
sample of high-z
ultra-luminous infrared galaxies {ULIRGs} whose redshifts
and physical
states have been determined with Spitzer mid-IR spectra.
The detection
of strong silicate absorption and/or PAH emission lines
suggest that the
these sources are a mixture of highly obscured starbursts,
AGNs and
composite systems at z=2. Although some of the spectra
show PAH emission
similar to local starburst ULIRGs, their bolometric
luminosities are
roughly an order of magnitude higher. One important
question is if major
mergers, which are the trigger for 95% of local ULIRGs,
also drive this
enormous energy output observed in our z=2 sample. The
NICMOS images
will allow us to {1} measure surface brightness profiles
of z~2 ULIRGs
and establish if major mergers could be common among our
luminous
sources at these early epochs, {2} determine if starbursts
and AGNs
classified based on their mid-IR spetra would have
different
morphological signatures, thus different dynamic state;
{3} make
comparisons with the similar studies of ULIRGs at z ~ 0 -
1, thus infer
any evolutionary connections between high-z ULIRGs and the
formation of
normal, massive galaxies and quasars observed today.
WFPC2 10880
The host galaxies of QSO2s: AGN feeding and evolution at
high
luminosities
Now that the presence of supermassive black holes in the
nuclei of
galaxies is a well established fact, other questions
related to the AGN
phenomena still have to be answered. Problems of
particular interest are
how the AGN gets fed, how the black hole evolves and how
the evolution
of the black hole is related to the evolution of the
galaxy bulge. Here
we propose to address some of these issues using ACS/WFC +
F775W
snapshot images of 73 QSO2s with redshifts in the range
0.3<z<0.4. These
observations will be combined with similar archival data
of QSO1s and
ground based data of Seyfert and normal galaxies. First,
we will
intestigate whether interactions are the most important
feeding
mechanism in high luminosity AGNs. This will be done in a
quantitative
way, comparing the asymmetry indices of QSO2 hosts with
those of lower
luminosity AGNs and normal galaxies. Second, we will do a
detailed study
of the morphology of the host galaxies of both QSO types,
to determine
if they are similar, or if there is an evolutionary trend
from QSO2s to
QSO1s. The results from this project will represent an
important step in
the understanding of AGN evolution, and may also introduce
a substantial
modification to the Unified Model.
WFPC2 11024
WFPC2 CYCLE 15 INTERNAL MONITOR
This calibration proposal is the Cycle 15 routine internal
monitor for
WFPC2, to be run weekly to monitor the health of the
cameras. A variety
of internal exposures are obtained in order to provide a
monitor of the
integrity of the CCD camera electronics in both bays {both
gain 7 and
gain 15 -- to test stability of gains and bias levels}, a
test for
quantum efficiency in the CCDs, and a monitor for possible
buildup of
contaminants on the CCD windows. These also provide raw
data for
generating annual super-bias reference files for the
calibration
pipeline.
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.
WFPC2 11023
WFPC2 CYCLE 15 Standard Darks - part 1
This dark calibration program obtains dark frames every
week in order to
provide data for the ongoing calibration of the CCD dark
current rate,
and to monitor and characterize the evolution of hot
pixels. Over an
extended period these data will also provide a monitor of
radiation
damage to the CCDs.
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are
preliminary reports
of potential non-nominal performance that will be
investigated.)
HSTARS:
10820 - GSAcq (1,2,2) failed to RGA Hold (Gyro Control)
AT
AOS (141/13:29:30) GSAcq (1,2,2) had failed to RGA Hold (Gyro
Control) due to QSTOP flag on FGS 1.
OBAD #1 unavailable due to LOS
OBAD #2 RSS: 15.84
10821 - ACS 779 Fold Mechanism Move was Blocked
At
141/13:31:24 "Fold Mechanism Move Was Blocked P=0, T=1001. This was
the result of the failed GSAcq at 13:22:49 so the TDF was down when the
fold mechanism move to the SBC position was commanded. The move is
blocked and SBC MAMA HV will remain on. The MAMA HV staying on is a new
feature for ACS FSW CS4.01.
10824 - FHST OBAD1 Failure
During LOS OBAD1 scheduled at 142/04:18:07 using trackers 1 and 2
failed. Subsequent OBAD2 and guide star acquisition was successful.
10825 - REacq(1,2,1) failed due to search radius limit
exceeded
During LOS REacq(1,2,1) scheduled at 142/06:06:34 failed due to search
radius limit exceeded on FGS 1.
COMPLETED OPS REQUEST:
18083-1 - MSS/Gyro2 Initialization Test#35 @141/1301z
18084-0 - MSS/Gyro1 Initialization Test#11 @141/2126z
18085-0 - PCS KF OOT Support,141/1302z
18086-0 - PCS KF OOT Support,141/2134z
COMPLETED OPS NOTES: (None)
SCHEDULED
SUCCESSFUL
FGS
GSacq
09
07
FGS
REacq
03
03
OBAD with Maneuver
24
23
SIGNIFICANT EVENTS:
Evaluation of Universal Kalman Filter performance
continued. Multiple
text segments were executed, all of them successfully.
Details follow.
The KF was halted at 141/12:48. It was restarted at
141/12:50 with the
MSS and Gyro2 sensor inputs enabled. The initialization
occurred during
orbit day with the CSS input disabled. The initialization
was executed
during a vehicle slew and during a slow changing B-field.
All UKF
parameters showed nominal operation. The test was an
MSS/Gyro2
Initialization test case during a slow changing B-field (M_G2_IVS,
Test
#35). The filter was reconfigured back to MSS only input
at 141/13:00.
The KF was halted at 141/21:24. It was restarted at
141/21:26 with the
MSS and Gyro1 sensor inputs enabled. The initialization
occurred during
orbit day with the CSS input disabled. The initialization
was executed
during a vehicle slew and during a fast changing B-field.
All UKF
parameters showed nominal operation. The test was an
MSS/Gyro1
Initialization test case during a fast changing B-field
(M_G1_IVF, Test
#11). The filter was reconfigured back to MSS only input
at 141/22:06.