HUBBLE
SPACE TELESCOPE - Continuing to collect World Class Science
DAILY
REPORT # 4539
PERIOD
COVERED: UT January 32,33,34, 2008 (DOY 032,033,034)
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.
S/C
11345
HST/PCS
1-Gyro On-orbit Checkout
This
proposal contains the part of the on-orbit test that cannot be
satisfied
by the science proposals. This includes testing certain M1G,
T1G
and F1G capabilities that could potentially compromise any science
data
collection, but are needed to validate the robustness of 1-gyro
science
mode.
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.
NIC3
11236
Did
Rare, Large Escape-Fraction Galaxies Reionize the Universe?
Lyman
continuum photons produced in massive starbursts may have played a
dominant
role in the reionization of the Universe. Starbursts are
important
contributors to the ionizing metagalactic background at lower
redshifts
as well. However, their contribution to the background depends
upon
the fraction of ionizing radiation that escapes from the intrinsic
opacity
of galaxies below the Lyman limit. Current surveys suggest that
the
escape fraction is close to zero in most galaxies, even among young
starbursts,
but is large in 15-25% of them. Non-uniform escape fractions
are
expected as a result of violent events creating clear paths in small
parts
of galaxies. The number of galaxies observed with high escape
fraction
will result from the combination of the intrinsic number with
clear
lines of sight and their orientation with respect to the observer.
We
propose to measure the fraction of escaping Lyman continuum radiation
in
a large sample (47) of z~0.7 starbursts in the COSMOS field. These
compact
UV-lumnious galaxies are good analogs to high redshift LBGs.
Using
the SBC/PR130L we can quickly (1-4 orbits) detect relative escape
fractions
(f_LC/f_1500) of 25% or more. This will be the first
measurement
of the escape fraction in sources between z=1 and the local
universe.
We expect ~10 detections. Stacking will set limits of <4% on
the
relative escape fraction in the rest. We will correlate the LC
detections
with the properties of the galaxies. By targeting z~0.7 in
COSMOS,
we will have tremendous ancillary information on those sources.
A
non-detection in all sources would be significant (99% confidence).
This
would imply that QSOs provide the overwhelming majority of ionizing
radtion
at z<1, requiring substantial evolution in the processes within
Lyman
break galaxies which allow large escape fractions at high
redshift.
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.
FGS
11210
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.
WFPC2/NIC3
11209
Determining
the Structural Parameters of the First Globular Cluster
Found
to Host an Black-Hole X-ray Binary
We
recently published the discovery of the first black hole X-ray binary
in
a globular cluster. This object is located in a bright globular
cluster
around the Virgo elliptical NGC 4472. Here we propose to obtain
HST
PC images of this black- hole hosting globular cluster and a sample
of
other NGC 4472 globulars. We will use these data to determine the
structural
parameters of both the globular cluster known to have a black
hole
and a control sample of other NGC 4472 clusters. This will test
recent
theoretical predictions how black holes affect the structural
parameters
of globular clusters, and more generally will allow for the
first
time constraints on any relationship between the presence of a
black
hole and the surface brightness profiles of globular clusters. The
deep
WFPC2 images outside of the galaxy's central regions will also be
invaluable
for studying how the sizes and luminosity function of
globular
clusters depend on distance from the center of the galaxy, and
thus
address questions about the origin of the size differences between
metal-rich
and metal-poor clusters and the shape of the globular cluster
luminosity
function. In addition, parallel NIC3 images will allow the
optical
to near-infrared colors of NGC 4472 globular cluster to be
determined
over a wide range of galactocentric radii.
WFPC2
11198
Pure
Parallel Imaging in the NDWFS Bootes Field
The
NOAO Deep-Wide Field Survey {NDWFS} Bootes field is the target of
one
of the most extensive multiwavelength campaigns in astronomy. In
addition
to ground-based optical and near-infrared imaging, deep radio
mapping,
and extensive spectroscopy, this entire region has been imaged
by
the Chandra, Spitzer {IRAC and MIPS}, and GALEX missions. Robust
photometric
redshifts {calibrated using over 20,000 spectroscopic
redshifts}
exist for all sources brighter than R=24.5 or than 13 uJy at
4.5
microns. To enhance the value of this data set, we propose pure
parallel
observations for all approved Cycle 16 programs in this region
that
lack coordinated parallel observations. The primary aim of this
program
will be to provide a database useful for the broad range of
science
programs underway in this region.
NIC3
11195
Morphologies
of the Most Extreme High-Redshift Mid-IR-luminous Galaxies
II:
The `Bump' Sources
The
formative phase of some of the most massive galaxies may be
extremely
luminous, characterized by intense star- and AGN-formation.
Till
now, few such galaxies have been unambiguously identified at high
redshift,
and thus far we have been restricted to studying the
low-redshift
ultraluminous infrared galaxies as possible analogs. We
have
recently discovered a sample of objects which may indeed represent
this
early phase in galaxy formation, and are undertaking an extensive
multiwavelength
study of this population. These objects are optically
extremely
faint {R>26} but nevertheless bright at mid-infrared
wavelengths
{F[24um] > 0.5 mJy}. Mid-infrared spectroscopy with
Spitzer/IRS
reveals that they have redshifts z~2, implying luminosities
~1E13
Lsun. Their mid-IR SEDs fall into two broad, perhaps overlapping,
categories.
Sources with brighter F[24um] exhibit power-law SEDs and SiO
absorption
features in their mid-IR spectra characteristic of AGN,
whereas
those with fainter F[24um] show a "bump" characteristic of the
redshifted
1.6um peak from a stellar population, and PAH emission
characteristic
of starformation. We have begun obtaining HST images of
the
brighter sources in Cycle 15 to obtain identifications and determine
kpc-scale
morphologies for these galaxies. Here, we aim to target the
second
class {the "bump" sources} with the goal of determining if these
constitute
morphologically different objects, or simply a "low-AGN"
state
of the brighter class. The proposed observations will help us
determine
whether these objects are merging systems, massive obscured
starbursts
{with obscuration on kpc scales!} or very reddened {locally
obscured}
AGN hosted by intrinsically low-luminosity galaxies.
WFPC2/NIC2
11173
Completing
an Accurate Map of M31 Microlensing
The
halo microlensing masses detected in the MACHO survey (claimed to
compose
about 20% of the Galaxy's mass) represent a major enigma in
astrophysics,
one that must be effectively cross-examined by an
independent
test. We have completed a large, densely-sampled survey of
M31
that can reveal in another galaxy such a halo microlensing signal if
it
exists. In a previous HST/ACS+WFPC2 program (GO 10273, Cycle 13, 16
orbits)
we were able to learn considerably more about a subsample of
these
M31 microlensing events. We were pleased to find that in most
cases
we could isolate the source star for each event, find its baseline
flux
and colors (essential for ruling out classes of confusing variable
stars),
test for misidentification of background supernovae, and measure
the
Einstein parameters, which constrain the range of most likely lens
mass.
(These Cycle 13 results are published in The Astrophysical Journal
Letters.)
We propose to finish the job, taking a similar series of
exposures
to more than double the sample of well-constrained
microlensing
events, which together with the larger ground-based sample
for
which we are completing our analyses will provide 20-30 M31 bona
fide
microlensing events observed by HST. This will be done via a series
of
targeted PC exposures, meant to maximize the number of candidates
studied,
one (or two) at a time. A sample of this size and quality
should
be sufficient to settle the issue of a significant contribution
to
the halos of galaxies by stellar-mass lenses. Furthermore, if there
is
a surplus of such microlensing events above what might be expected
from
stars alone, the higher quality of information will allow us to
more
accurately describe the spatial distribution of these lenses. We
will
also complete several unique studies of M31 stellar populations,
both
in support of the microlensing measurement and in their own right.
NIC3
11153
The
Physical Nature and Age of Lyman Alpha Galaxies
In
the simplest scenario, strong Lyman alpha emission from high redshift
galaxies
would indicate that stellar populations younger than 10 Myrs
dominate
the UV. This does not, however, constrain the stellar
populations
older than 100 Myrs, which do not contribute to UV light.
Also,
the Lyman alpha line can be boosted if the interstellar medium is
both
clumpy and dusty. Different studies with small samples have reached
different
conclusions about the presence of dust and old stellar
populations
in Lyman alpha emitters. We propose HST- NICMOS and
Spitzer-IRAC
photometry of 35 Lyman-alpha galaxies at redshift
4.5<z<6.5,
in order to determine their spectral energy distribution
{SED}
extending through rest-frame optical. This will allow us to
measure
accurately {1} The total stellar mass in these objects,
including
old stars which may have formed at redshifts {z > 8} not
easily
probed by any other means. {2} The dust extinction in the
rest-frame
UV, and therefore a correction to their present
star-formation
rates. Taken together, these two quantities will yield
the
star-formation histories of Lyman alpha galaxies, which form fully
half
of the known galaxies at z=4-6. They will tell us whether these are
young
or old galaxies by straddling the 4000A break. Data from NICMOS is
essential
for these compact and faint {i=25-26th magnitude AB} high
redshift
galaxies, which are too faint for good near-IR photometry from
the
ground.
NIC2
11142
Revealing
the Physical Nature of Infrared Luminous Galaxies at 0.3
We
aim to determine physical properties of IR luminous galaxies at
0.3<z<2.7
by requesting coordinated HST/NIC2 and MIPS 70um observations
of
a unique, 24um flux-limited sample with complete Spitzer mid-IR
spectroscopy.
The 150 sources investigated in this program have S{24um}
>
0.8mJy and their mid-IR spectra have already provided the majority
targets
with spectroscopic redshifts {0.3<z<2.7}. The proposed
150~orbits
of NIC2 and 66~hours of MIPS 70um will provide the physical
measurements
of the light distribution at the rest-frame ~8000A and
better
estimates of the bolometric luminosity. Combining these
parameters
together with the rich suite of spectral diagnostics from the
mid-IR
spectra, we will {1} measure how common mergers are among LIRGs
and
ULIRGs at 0.3<z<2.7, and establish if major mergers are the drivers
of
z>1 ULIRGs, as in the local Universe. {2} study the co-evolution of
star
formation and black-hole accretion by investigating the relations
between
the fraction of starburst/AGN measured from mid-IR spectra vs.
HST
morphologies, L{bol} and z. {3} obtain the current best estimates of
the
far-IR emission, thus L{bol} for this sample, and establish if the
relative
contribution of mid-to-far IR dust emission is correlated with
morphology
{resolved vs. unresolved}.
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.
NIC3
11107
Imaging
of Local Lyman Break Galaxy Analogs: New Clues to Galaxy
Formation
in the Early Universe
We have
used the ultraviolet all-sky imaging survey currently being
conducted
by the Galaxy Evolution Explorer {GALEX} to identify for the
first
time a rare population of low-redshift starbursts with properties
remarkably
similar to high-redshift Lyman Break Galaxies {LBGs}. These
"compact
UV luminous galaxies" {UVLGs} resemble LBGs in terms of size,
SFR,
surface brightness, mass, metallicity, kinematics, dust, and color.
The
UVLG sample offers the unique opportunity of investigating some very
important
properties of LBGs that have remained virtually inaccessible
at
high redshift: their morphology and the mechanism that drives their
star
formation. Therefore, in Cycle 15 we have imaged 7 UVLGs using ACS
in
order to 1} characterize their morphology and look for signs of
interactions
and mergers, and 2} probe their star formation histories
over
a variety of timescales. The images show a striking trend of small-
scale
mergers turning large amounts of gas into vigorous starbursts {a
process
referred to as dissipational or "wet" merging}. Here, we propose
to
complete our sample of 31 LBG analogs using the ACS/SBC F150LP {FUV}
and
WFPC2 F606W {R} filters in order to create a statistical sample to
study
the mechanism that triggers star formation in UVLGs and its
implications
for the nature of LBGs. Specifically, we will 1} study the
trend
between galaxy merging and SFR in UVLGs, 2} artificially redshift
the
FUV images to z=1-4 and compare morphologies with those in similarly
sized
samples of LBGs at the same rest-frame wavelengths in e.g. GOODS,
UDF,
and COSMOS, 3} determine the presence and morphology of significant
stellar
mass in "pre- burst" stars, and 4} study their immediate
environment.
Together with our Spitzer {IRAC+MIPS}, GALEX, SDSS and
radio
data, the HST observations will form a unique union of data that
may
for the first time shed light on how the earliest major episodes of
star
formation in high redshift galaxies came about. This proposal was
adapted
from an ACS HRC+WFC proposal to meet the new Cycle 16 observing
constraints,
and can be carried out using the ACS/SBC and WFPC2 without
compromising
our original science goals.
WFPC2
11103
A
Snapshot Survey of The Most Massive Clusters of Galaxies
We
propose the continuation of our highly successful SNAPshot survey of
a
sample of 125 very X-ray luminous clusters in the redshift range
0.3-0.7.
As demonstrated by the 25 snapshots obtained so far in Cycle14
and
Cycle15 these systems frequently exhibit strong gravitational
lensing
as well as spectacular examples of violent galaxy interactions.
The
proposed observations will provide important constraints on the
cluster
mass distributions, the physical nature of galaxy-galaxy and
galaxy-gas
interactions in cluster cores, and a set of optically bright,
lensed
galaxies for further 8-10m spectroscopy. All of our primary
science
goals require only the detection and characterization of
high-surface-brightness
features and are thus achievable even at the
reduced
sensitivity of WFPC2. Because of their high redshift and thus
compact
angular scale our target clusters are less adversely affected by
the
smaller field of view of WFPC2 than more nearby systems.
Acknowledging
the broad community interest in this sample we waive our
data
rights for these observations. Due to a clerical error at STScI our
approved
Cycle15 SNAP program was barred from execution for 3 months and
only
6 observations have been performed to date - reinstating this SNAP
at
Cycle16 priority is of paramount importance to reach meaningful
statistics.
NIC3
11080
Exploring
the Scaling Laws of Star Formation
As
a variety of surveys of the local and distant Universe are
approaching
a full census of galaxy populations, our attention needs to
turn
towards understanding and quantifying the physical mechanisms that
trigger
and regulate the large-scale star formation rates {SFRs} in
galaxies.
WFPC2
11037
Red
Filters Closeout
This
calibration program observes three very red stars {M, L, T dwarfs}
in
the five reddest broad and medium filters {F785LP, F791W, F814W,
F850LP,
and F1042M} on WF3 in order to allow cross-calibration to ACS,
and
in future WFC3. The far-red QE curves will also be tested. Similar
observations
on PC1 were made in WFPC2/CAL 10078 and 10366.
WFPC2
11029
WFPC2
CYCLE 15 Intflat Linearity Check and Filter Rotation Anomaly
Monitor
Intflat
observations will be taken to provide a linearity check: the
linearity
test consists of a series of intflats in F555W, in each gain
and
each shutter. A combination of intflats, visflats, and earthflats
will
be used to check the repeatability of filter wheel motions.
{Intflat
sequences tied to decons, visits 1-18 in prop 10363, have been
moved
to the cycle 15 decon proposal xxxx for easier scheduling.} Note:
long-exposure
WFPC2 intflats must be scheduled during ACS anneals to
prevent
stray light from the WFPC2 lamps from contaminating long ACS
external
exposures.
WFPC2
11027
Visible
Earth Flats
This
proposal monitors flatfield stability. This proposal obtains
sequences
of Earth streak flats to construct high quality flat fields
for
the WFPC2 filter set. These flat fields will allow mapping of the
OTA
illumination pattern and will be used in conjunction with previous
internal
and external flats to generate new pipeline superflats. These
Earth
flats will complement the Earth flat data obtained during cycles
4-14.
WFPC2
11020
Cycle
15 Focus Monitor
The
focus of HST is measured primarily with ACS/HRC over full CVZ orbits
to obtain
accurate mean focus values via a well sampled breathing curve.
Coma
and astigmatism are also determined from the same data in order to
further
understand orbital effects on image quality and optical
alignments.
To monitor the stability of ACS to WFPC2 relative focii,
we've
carried over from previous focus monitor programs parallel
observations
taken with the two cameras at suitable orientations of
previously
observed targets, and interspersed them with the HRC CVZ
visits.
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.
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}.
FLIGHT
OPERATIONS SUMMARY:
Significant
Spacecraft Anomalies: (The following are preliminary reports
of
potential non-nominal performance that will be investigated.)
HSTARS:
11171
- GSAcq(2,3,2) results in fine lock backup (2,0,2) using FGS2
Following successful transition back to TGS operations, the
GSAcq(2,3,2)
scheduled at 032/10:33:13- 10:41:18 resulted to fine lock backup
(2,0,2)
using FGS2 due to (QF3STOPF) stop flag indication on FGS3.
Pre-acquisition OBADs had (RSS) values of 1939.41 and 10.44
arcseconds.
Post-acq OBAD/MAP (RSS) value is not available in FN FORMAT.
11172
- GSacq(1,2,1) failed to RGA control.
GSacq(1,2,1) scheduled at 032/12:04:52 failed to RGA control. Stop
flag
QF1STOPF was received at 12:08:03. OBAD2 had an RSS value 12.03
a-s. The
map at 12:12:28 showed errors of V1 = 4.49, V2= 6.94, V3= -4.60,
and
RSS= 9.46.
11173
- ACS 779 Fold Mechanism Move was Blocked.
Several ACS 779 Status Buffer Messages ("Fold Mechanism Move
was
Blocked") was received following the failure of the
GSacq(1,2,1) at
032/12:04:52, which caused the TDF to be down when the Fold
mechanism
move was commanded.
COMPLETED
OPS REQUEST: (None)
COMPLETED
OPS NOTES: (None)
SCHEDULED
SUCCESSFUL
FGS
GSacq
29
28
FGS
REacq
14
14
OBAD
with Maneuver 86
86
SIGNIFICANT
EVENTS: (None)