HUBBLE
SPACE TELESCOPE - Continuing to collect World Class Science
DAILY
REPORT # 4530
PERIOD
COVERED: UT January 18,19,20,21, 2007 (DOY 018,019,020,021)
OBSERVATIONS
SCHEDULED
NIC1/NIC2/NIC3
8795
NICMOS Post-SAA calibration - CR Persistence Part 6
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 i
mages.
Each observation will need its own CRMAP, as different SAA
passages
leave different imprints on the NICMOS detectors.
NIC3
11331
NICMOS
Cycle 16 Grism Calibration
A
series of pointed NICMOS observations of the spectroscopic flux
calibrator
P330E and two wavelength calibrators VY2-2 and HB12.
WFPC2
11312
The
Local Cluster Substructure Survey {LoCuSS}: Deep Strong Lensing
Observations
with WFPC2
LoCuSS
is a systematic and detailed investigation of the mass,
substructure,
and thermodynamics of 100 X-ray luminous galaxy clusters
at
0.15<z<0.3. The primary goal is to test our recent suggestion that
this
population is dominated by dynamically immature disturbed clusters,
and
that the observed mass-temperature relation suffers strong
structural
segregation. If confirmed, this would represent a paradigm
shift
in our observational understanding of clusters, that were hitherto
believed
to be dominated by mature, undisturbed systems. We propose to
complete
our successful Cycle 15 program {SNAP:10881} which prior to
premature
termination had delivered robust weak-lensing detections in 17
clusters,
and candidate strongly-lensed arcs in 11 of these 17. These
strong
and weak lensing signals will give an accurate measure of the
total
mass and structure of the dark matter distribution that we will
subsequently
compare with X-ray and Sunyaev Zeldovich Effect
observables.
The broader applications of our project include 1} the
calibration
of mass-temperature and mass-SZE scaling relations which
will
be critical for the calibration of proposed dark energy
experiments,
and 2} the low redshift baseline study of the demographics
of
massive clusters to aid interpretation of future high redshift {z>1}
cluster
samples. To complete the all-important high resolution imaging
component
of our survey, we request deep WFPC2 observations of 20
clusters
through the F606W filter, for which wide-field weak-lensing
data
are already available from our Subaru imaging program. The
combination
of deep WFPC2 and Subaru data for these 20 clusters will
enable
us to achieve the science program approved by the Cycle 15 TAC.
FGS
11301
Dynamical
Masses and Radii of Four White Dwarf Stars
This
proposal uses the FGS1r in TRANS mode to resolve a pair of double
degenerate
binary systems {WD1639+153 and WD 1818+26} in order to
determine
their orbital elements. In addition, the binaries and several
nearby
field stars are observed by FGS1r in POS mode to establish the
local
inertial reference frame of each binary, as well as its parallax
and
proper motion. This will allow for a direct measurement of the
distance
and radius of each of the four WD stars. When combined with the
orbital
elements, this leads to a dynamical mass measurement for each
WD,
and a four calibration points of the WD mass-radius relation.
WFPC2
11289
SL2S:
The Strong Lensing Legacy Survey
Recent
systematic surveys of strong galaxy-galaxy lenses {CLASS, SLACS,
GOODS,
etc.} are producing spectacular results for galaxy masses roughly
below
a transition mass M~10^13 Mo. The observed lens properties and
their
evolution up to z~0.2, consistent with numerical simulations, can
be
described by isothermal elliptical potentials. In contrast, modeling
of
giant arcs in X-ray luminous clusters {halo masses M >~10^13 Mo}
favors
NFW mass profiles, suggesting that dark matter halos are not
significantly
affected by baryon cooling. Until recently, lensing
surveys
were neither deep nor extended enough to probe the intermediate
mass
density regime, which is fundamental for understanding the assembly
of
structures. The CFHT Legacy Survey now covers 125 square degrees, and
thus
offers a large reservoir of strong lenses probing a large range of
mass
densities up to z~1. We have extracted a list of 150 strong lenses
using
the most recent CFHTLS data release via automated procedures.
Following
our first SNAPSHOT proposal in cycle 15, we propose to
continue
the Hubble follow-up targeting a larger list of 130 lensing
candidates.
These are intermediate mass range candidates {between
galaxies
and clusters} that are selected in the redshift range of 0.2-1
with
no a priori X-ray selection. The HST resolution is necessary for
confirming
the lensing candidates, accurate modeling of the lenses, and
probing
the total mass concentration in galaxy groups up to z~1 with the
largest
unbiased sample available to date.
WFPC2
11229
SEEDS:
The Search for Evolution of Emission from Dust in Supernovae with
HST
and Spitzer
The
role that massive stars play in the dust content of the Universe is
extremely
uncertain. It has long been hypothesized that dust can
condense
within the ejecta of supernovae {SNe}, however there is a
frustrating
discrepancy between the amounts of dust found in the early
Universe,
or predicted by nucleation theory, and inferred from SN
observations.
Our SEEDS collaboration has been carefully revisiting the
observational
case for dust formation by core- collapse SNe, in order to
quantify
their role as dust contributors in the early Universe. As dust
condenses
in expanding SN ejecta, it will increase in optical depth,
producing
three simultaneously observable phenomena: {1} increasing
optical
extinction; {2} infrared {IR} excesses; and {3} asymmetric
blue-shifted
emission lines. Our SEEDS collaboration recently reported
all
three phenomena occurring in SN2003gd, demonstrating the success of
our
observing strategy, and permitting us to derive a dust mass of up to
0.02
solar masses created in the SN. To advance our understanding of the
origin
and evolution of the interstellar dust in galaxies, we propose to
use
HST's WFPC2 and NICMOS instruments plus Spitzer's photometric
instruments
to monitor ten recent core-collapse SNe for dust formation
and,
as a bonus, detect light echoes that can affect the dust mass
estimates.
These space-borne observations will be supplemented by
ground-based
spectroscopic monitoring of their optical emission line
profiles.
These observations would continue our 2-year HST and Spitzer
monitoring
of this phenomena in order to address two key questions: Do
all
SNe produce dust? and How much dust do they produce? As all the SN
are
within 15 Mpc, each SN stands an excellent chance of detection with
HST
and Spitzer and of resolving potential light echoes.
WFPC2
11222
Direct
Detection and Mapping of Star Forming Regions in Nearby, Luminous
Quasars
We
propose to carry out narrow-band emission line imaging observations
of
8 quasars at z=0.05-0.15 with the WFPC2 ramp filters and with the
NICMOS
narrow-band filters. We will obtain images in the [O II], [O
III],
H-beta, and Pa-alpha emission line bands to carry out a series of
diagnostic
tests aimed at detecting and mapping out star-forming regions
in
the quasar host galaxies. This direct detection of star-forming
regions
will confirm indirect indications for star formation in quasar
host
galaxies. It will provide a crucial test for models of quasar and
galaxy
evolution, that predict the co-existence of starbursts and
"monsters"
and will solve the puzzle of why different indicators of star
formation
give contradictory results. A secondary science goal is to
assess
suggested correlations between quasar luminosity and the size of
the
narrow-line region.
FGS
11212
Filling
the Period Gap for Massive Binaries
The
current census of binaries among the massive O-type stars is
seriously
incomplete for systems in the period range from years to
millennia
because the radial velocity variations are too small and the
angular
separations too close for easy detection. Here we propose to
discover
binaries in this observational gap through a Faint Guidance
Sensor
SNAP survey of relatively bright targets listed in the Galactic O
Star
Catalog. Our primary goal is to determine the binary frequency
among
those in the cluster/association, field, and runaway groups. The
results
will help us assess the role of binaries in massive star
formation
and in the processes that lead to the ejection of massive
stars
from their natal clusters. The program will also lead to the
identification
of new, close binaries that will be targets of long term
spectroscopic
and high angular resolution observations to determine
their
masses and distances. The results will also be important for the
interpretation
of the spectra of suspected and newly identified binary
and
multiple systems.
FGS
11211
An
Astrometric Calibration of Population II Distance Indicators
In
2002 HST produced a highly precise parallax for RR Lyrae. That
measurement
resulted in an absolute magnitude, M{V}= 0.61+/-0.11, a
useful
result, judged by the over ten refereed citations each year
since.
It is, however, unsatisfactory to have the direct,
parallax-based,
distance scale of Population II variables based on a
single
star. We propose, therefore, to obtain the parallaxes of four
additional
RR Lyrae stars and two Population II Cepheids, or
stars.
The Population II Cepheids lie with the RR Lyrae stars on a
common
K-band Period-Luminosity relation. Using these parallaxes to
inform
that relationship, we anticipate a zero-point error of 0.04
magnitude.
This result should greatly strengthen confidence in the
Population
II distance scale and increase our understanding of RR Lyrae
star
and Pop II Cepheid astrophysics.
WFPC2
11202
The
Structure of Early-type Galaxies: 0.1-100 Effective Radii
The
structure, formation and evolution of early-type galaxies is still
largely
an open problem in cosmology: how does the Universe evolve from
large
linear scales dominated by dark matter to the highly non-linear
scales
of galaxies, where baryons and dark matter both play important,
interacting,
roles? To understand the complex physical processes
involved
in their formation scenario, and why they have the tight
scaling
relations that we observe today {e.g. the Fundamental Plane}, it
is
critically important not only to understand their stellar structure,
but
also their dark-matter distribution from the smallest to the largest
scales.
Over the last three years the SLACS collaboration has developed
a
toolbox to tackle these issues in a unique and encompassing way by
combining
new non-parametric strong lensing techniques, stellar
dynamics,
and most recently weak gravitational lensing, with
high-quality
Hubble Space Telescope imaging and VLT/Keck spectroscopic
data
of early-type lens systems. This allows us to break degeneracies
that
are inherent to each of these techniques separately and probe the
mass
structure of early-type galaxies from 0.1 to 100 effective radii.
The
large dynamic range to which lensing is sensitive allows us both to
probe
the clumpy substructure of these galaxies, as well as their
low-density
outer haloes. These methods have convincingly been
demonstrated,
by our team, using smaller pilot-samples of SLACS lens
systems
with HST data. In this proposal, we request observing time with
WFPC2
and NICMOS to observe 53 strong lens systems from SLACS, to obtain
complete
multi-color imaging for each system. This would bring the total
number
of SLACS lens systems to 87 with completed HST imaging and
effectively
doubles the known number of galaxy-scale strong lenses. The
deep
HST images enable us to fully exploit our new techniques, beat down
low-number
statistics, and probe the structure and evolution of
early-type
galaxies, not only with a uniform data-set an order of
magnitude
larger than what is available now, but also with a fully
coherent
and self-consistent methodological approach!
WFPC2
11178
Probing
Solar System History with Orbits, Masses, and Colors of
Transneptunian
Binaries
The
recent discovery of numerous transneptunian binaries {TNBs} opens a
window
into dynamical conditions in the protoplanetary disk where they
formed
as well as the history of subsequent events which sculpted the
outer
Solar System and emplaced them onto their present day heliocentric
orbits.
To date, at least 47 TNBs have been discovered, but only about a
dozen
have had their mutual orbits and separate colors determined,
frustrating
their use to investigate numerous important scientific
questions.
The current shortage of data especially cripples scientific
investigations
requiring statistical comparisons among the ensemble
characteristics.
We propose to obtain sufficient astrometry and
photometry
of 23 TNBs to compute their mutual orbits and system masses
and
to determine separate primary and secondary colors, roughly tripling
the
sample for which this information is known, as well as extending it
to
include systems of two near-equal size bodies. To make the most
efficient
possible use of HST, we will use a
optimally
schedule our observations.
WFPC2
11134
WFPC2
Tidal Tail Survey: Probing Star Cluster Formation on the Edge
The
spectacular HST images of the interiors of merging galaxies such as
the
Antennae and NGC 7252 have revealed rich and diverse populations of
star
clusters created over the course of the interaction. Intriguingly,
our
WFPC2 study of tidal tails in these and other interacting pairs has
shown
that star cluster birth in the tails does not follow a similarly
straightforward
evolution. In fact, cluster formation in these
relatively
sparse environments is not guaranteed -- only one of six
tails
in our initial study showed evidence for a significant population
of
young star clusters. The tail environment thus offers the opportunity
to
probe star cluster formation on the edge of the physical parameter
space
{e.g., of stellar and gas mass, density, and pressure} that
permits
it to occur. We propose to significantly extend our pilot sample
of
optically bright, gas-rich tidal tails by a factor of 4 in number to
include
a more diverse population of tails, encompassing major and minor
mergers,
gas-rich and gas-poor tails, as well as early, late, and merged
interaction
stages. With 21 orbits of HST WFPC2 imaging in the F606W and
F814W
filters, we can identify, roughly age-date, and measure sizes of
star
clusters to determine what physical parameters affect star cluster
formation.
WFPC2 imaging has been used effectively in our initial study
of
four mergers, and it will be possible in this program to reach
similar
limits of Mv=-8.5 for each of 16 more tails. With the much
larger
sample we expect to isolate which factors, such as merger stage,
HI
content, and merger mass ratio, drive the formation of star clusters.
WFPC2
11125
The
Dynamical Evolution of Globular Clusters
Globular
clusters evolve through dynamical interactions, with primordial
binaries
extending the time until core collapse by up to an order of
magnitude,
depending on the initial binary fraction. These dynamical
interactions
plus mass segregation causes the binary fraction to rise in
the
core but fall at larger radii. We hope to eventually test these
broad
predictions by comparing them to the binary properties for
globular
clusters at different states of evolution, defined by the ratio
of
their age to the dynamical relaxation time at the half-light radius.
The
most important unknown aspects in the modeling process are the
initial
conditions of binaries in the cluster. Here we propose to
determine
the initial binary fraction as a function of radius by
studying
three of the dynamically youngest globular clusters {NGC 5053,
NGC
5466, and NGC 5897}. The presence of binaries thickens the
Sequence
in a color-magnitude diagram, which can be detected with deep
multicolor
images.
WFPC2
11122
Expanding
PNe: Distances and Hydro Models
We
propose to obtain repeat narrowband images of a sample of eighteen
planetary
nebulae {PNe} which have HST/WFPC2 archival data spanning time
baselines
of a decade. All of these targets have previous high
signal-to-noise
WFPC2/PC observations and are sufficiently nearby to
have
readily detectable expansion signatures after a few years. Our main
scientific
objectives are {a} to determine precise distances to these
PNe
based on their angular expansions, {b} to test detailed and highly
successful
hydrodynamic models that predict nebular morphologies and
expansions
for subsamples of round/elliptical and axisymmetric PNe, and
{c}
to monitor the proper motions of nebular microstructures in an
effort
to learn more about their physical nature and formation
mechanisms.
The proposed observations will result in high-precision
distances
to a healthy subsample of PNe, and from this their expansion
ages,
luminosities, CSPN properties, and masses of their ionized cores.
With
good distances and our hydro models, we will be able to determine
fundamental
parameters {such as nebular and central star masses,
luminosity,
age}. The same images allow us to monitor the changing
overall
ionization state and to search for the surprisingly
non-homologous
growth patterns to bright elliptical PNe of the same sort
seen
by Balick & Hajian {2004} in NGC 6543. Non-uniform growth is a sure
sign
of active pressure imbalances within the nebula that require
careful
hydro models to understand.
WFPC2
11113
Binaries
in the Kuiper Belt: Probes of Solar System Formation and
Evolution
The
discovery of binaries in the Kuiper Belt and related small body
populations
is powering a revolutionary step forward in the study of
this
remote region. Three quarters of the known binaries in the Kuiper
Belt
have been discovered with HST, most by our snapshot surveys. The
statistics
derived from this work are beginning to yield surprising and
unexpected
results. We have found a strong concentration of binaries
among
low-inclination Classicals, a possible size cutoff to binaries
among
the Centaurs, an apparent preference for nearly equal mass
binaries,
and a strong increase in the number of binaries at small
separations.
We propose to continue this successful program in Cycle 16;
we
expect to discover at least 13 new binary systems, targeted to
subgroups
where these discoveries can have the greatest impact.
NIC2
11101
The
Relevance of Mergers for Fueling AGNs: Answers from QSO Host
Galaxies
The
majority of QSOs are known to reside in centers of galaxies that
look
like ellipticals. Numerical simulations have shown that remnants of
galaxy
mergers often closely resemble elliptical galaxies. However, it
is
still strongly debated whether the majority of QSO host galaxies are
indeed
the result of relatively recent mergers or whether they are
completely
analogous to inactive ellipticals to which nothing
interesting
has happened recently. To address this question, we recently
obtained
deep HST ACS images for five QSO host galaxies that were
classified
morphologically as ellipticals {GO-10421}. This pilot study
revealed
striking signs of tidal interactions such as ripples, tidal
tails,
and warped disks that were not detected in previous studies. Our
observations
show that at least some "elliptical" QSO host galaxies are
the
products of relatively recent merger events rather than old galaxies
formed
at high redshift. However, the question remains whether the host
galaxies
of classical QSOs are truly distinct from inactive ellipticals
and
whether there is a connection between the merger events we detect
and
the current nuclear activity. We must therefore place our results
into
a larger statistical context. We are currently conducting an HST
archival
study of inactive elliptical galaxies {
control
sample. We now propose to obtain deep HST/WFPC2 images of 13
QSOs
whose host galaxies are classified as normal ellipticals. Comparing
the
results for both samples will help us determine whether classical
QSOs
reside in normal elliptical galaxies or not. Our recent pilot study
of
five QSOs indicates that we can expect exciting results and deep
insights
into the host galaxy morphology also for this larger sample of
QSOs.
A statistically meaningful sample will help us determine the true
fraction
of QSO hosts that suffered strong tidal interactions and thus,
whether
a merger is indeed a requirement to trigger nuclear activity in
the
most luminous AGNs. In addition to our primary science observations
with
WFPC2, we will obtain NICMOS3 parallel observations with the
overall
goal to select and characterize galaxy populations at high
redshifts.
The imaging will be among the deepest NICMOS images: These
NICMOS
images are expected to go to a limit a little over 1 magnitude
brighter
than HUDF- NICMOS data, but over 13 widely separated fields,
with
a total area about 1.5 times larger than HUDF-NICMOS. This
separation
means that the survey will tend to average out effects of
cosmic
variance. The NICMOS3 images will have sufficient resolution for
an
initial characterization of galaxy morphologies, which is currently
one
of the most active and promising areas in approaching the problem of
the
formation of the first massive galaxies. The depth and area coverage
of
our proposed NICMOS observations will also allow a careful study of
the
mass function of galaxies at these redshifts. This provides a large
and
unbiased sample, selected in terms of stellar mass and unaffected by
cosmic
variance, to study the on-going star formation activity as a
function
of mass {i.e. integrated star formation} at this very important
epoch.
WFPC2
11070
WFPC2
CYCLE 15 Standard Darks - part II
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.
WFPC2
11038
Narrow
Band and Ramp Filter Closeout
These
observations are to improve calibration of narrow band and ramp
filters.
We also test for changes in the filter properties during
WFPC2's
14 years on-board HST.
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.
WFPC2
11002
A
Census of LIRGs in Clusters of Galaxies in the First Half of the
Universe
from the IRAC Shallow Survey
The
incidence of LIRGs and ULIRGs is roughly two orders of magnitude
higher
in the field at redshift z > 1, and at these redshifts such
objects
dominate the global star formation activity. Mergers which fuel
such
activity might be expected to enhance the frequency of LIRGs in
dense
environments. We propose to use MIPS to obtain a census of LIRGs
in
z > 1 galaxy clusters from a well defined sample found in the IRAC
Shallow
Survey. Supporting IRAC and HST ACS data are also requested.
FGS
10998
Exoplanet
XO-1b: light curve and parallax
We
propose to measure the radius of the recently-discovered transiting
extrasolar
planet XO-1b. XO-1b's nominal radius is 1.30 times the radius
of
Jupiter, which is nearly as large as HD 209458b {1.32 R_J}. We will
use
two independent methods to measure XO-1b's radius: 1} precision
light
curve analysis, and 2} measurement of its trigonometric parallax
combined
with its spectroscopically-determined effective temperature and
its
apparent magnitude.
WFPC2
10901
UV-Luminous
Globular Clusters in NGC 1399
Ultraviolet
observations have revealed remarkable diversity among old
stellar
populations in globular clusters and E/S0 galaxies. We recently
discovered
with HST/STIS that globular clusters in the giant elliptical
galaxy
M87 have the most heavily populated hot horizontal branches of
any
stellar systems yet studied. Their far-UV/optical colors are up to 1
mag
bluer than any Milky Way globular cluster and approach the
theoretical
limits for production of hot-HB stars in old stellar
populations.
The differences among the metal-poor clusters are
particularly
interesting, because it is thought that these objects
reflect
the earliest stages of galaxy formation at high redshifts. Here
we
propose deep ACS far-UV imaging of a second gE galaxy, NGC 1399, with
a
cluster system that is well-studied at longer wavelengths, to
determine
whether it shares characteristics with M87. These observations
bear
on aspects of advanced stellar evolution, on the histories of
globular
clusters in different environments, and on the interpretation
of
the "ultraviolet upturn'' phenomenon in elliptical galaxies and its
value
as a population probe in distant galaxies.
WFPC2
10896
An
Efficient ACS Coronagraphic Survey for Debris Disks around Nearby
Stars
We
propose to finish our Cycle 11 optical survey for nearby debris disks
using
the ACS/HRC coronagraph. Out of 43 orbits originally proposed for
the
survey, 23 orbits were allocated, leading to a survey of 22 stars,
from
which two new debris disks were imaged for the first time. Our
analysis
of the initial survey gives an empirical estimate for the
detection
rate of debris disks relative to heliocentric distance and
dust
optical depth. Our target list for Cycle 15 is now optimized to
yield
more frequent disk detections. Likewise our observing strategy is
improved
to maximize sensitivity per telescope orbit allocated.
Therefore
we present the most efficient survey possible. The scientific
motivation
is to obtain scattered light images of previously unresolved
debris
disks to determine their viewing geometry and physical
architecture,
both of which may characterize the underlying planetary
system.
We choose 25 debris disk targets for which we predict a
detection
rate of 25% ? 5%. Four targets have extrasolar planets from
which
the viewing geometry revealed by a disk detection will resolve the
v
sin{i} ambiguity in the planet masses. These targets present the
remarkable
opportunity of finally seeing a debris disk in system with
known
planets.
FLIGHT
OPERATIONS SUMMARY:
Significant
Spacecraft Anomalies: (The following are preliminary reports
of
potential non-nominal performance that will be investigated.)
HSTARS:
11152
- GSAcq(1,2,1) Fine Lock Backup on FGS 1
GSACQ(1,2,1) at 020/03:10:45 acquired in fine lock backup on FGS 1 only,
with QF2STOPF and QSTOP flags set on FGS 2 at 03:15:42. No other flags
were seen. REACQ(1,2,1) at 04:44:33 was successful on both FGS 1 and 2.
11153
- REAcq(2,1,2) failed due to Scan Step Limit Exceeded on FGS 2
At Acquisition of Signal @ 020/16:29:36 REAcq (2,1,2), scheduled from
020/15:22:06-15:29:35, had failed due to Scan Step Limit Exceeded on FGS
2. QF2SSLEX, QF2STOPF, QSTEPEXC & QSTOP flags were received.
Pre-acquisition OBAD #1 RSS = 9.09 a-s, OBAD #2 RSS = 5.67 a-s.
Post-acquisition OBAD Map was not scheduled. Next scheduled engineering
data dump will occur at 020/21:46:02.
REAcq (2,1,2) scheduled from 020/18:33:56-18:41:25 failed due to Scan
Step Limit Exceeded on FGS 2. QF2SSLEX, QF2STOPF, QSTEPEXC & QSTOP flags
were received. Pre-acquisition OBAD #1 RSS = 13.60 a-s, OBAD #2 RSS =
6.25 a-s. Post-acquisition OBAD Map = 11.68 a-s. This REAcq used the
same guide star pair as the REAcq @ 020/15:22:06. Initial analysis shows
FGS 2 achieved Fine Lock @ 18:36:56 but, lost it @ 18:37:28. SAC
processing shows a deviation of 8.15864 a-s.
11154
- GSAcq(2,3,2) failed
GSACQ(2,3,2) at 021/01:20:23 failed to RGA control with QF2STOPF and
QSTOP flags set at 01:24:24. No other flags were seen.
11156
- REacq results in high boresight jitter @2007/ 331/0244z Jitter
determined from control law position path following this reacquisition
was approximately 2X measured jitter following the Acq and first Reacq.
Star quality is suspected
COMPLETED
OPS REQUEST: (None)
COMPLETED
OPS NOTES: (None)
SCHEDULED SUCCESSFUL
FGS
GSacq 27 26
FGS
REacq 31 29
OBAD
with Maneuver 106 105
SIGNIFICANT
EVENTS:
Flash
Report: FSW/FGE Hybrid Mode Disabled:
Ops
Request 18175 was successfully completed at 021/15:01 to disable
FSW/FGE
hybrid mode.