HUBBLE SPACE TELESCOPE - Continuing to collect World Class
Science
DAILY REPORT #
4278
PERIOD COVERED: UT January 12,13,14,15, 2007 (DOY
012,013,014,015)
OBSERVATIONS SCHEDULED
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.
ACS/SBC 11074
ACS/SBC Darks in Support of Specific SBC Science
Observations
This program provides SBC DARK visits to be scheduled in
conjuction with
certain specific science observations which require the SBC
to be turned
on in the orbit preceeding the science observation.
ACS/HRC 11053
Earth Flats
Sky flats will be obtained by observing the bright Earth
with the HRC
and WFC. These observations will be used to verify the
accuracy of the
latest pipeline flats and to monitor any changes. Weekly
coronagraphic
monitoring is required to assess the changing position of
the spots.
ACS/WFC 11052
Internal Flat Fields
The stability of the CCD P-flat fields will be monitored
using the
calibration lamps and a sub- sample of the filter set. High
signal
observations will be used to assess the stability of the
pixel- to-pixel
flat field structure and to monitor the position of the dust
motes.
ACS/HRC 11041
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. For cycle 15 the program will cover
18 months
12.1.06->05.31.08 and it has been divied into three
different proposal
each covering six months. The three proposals are
11041-11042-11043.
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.
ACS/WFC 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 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.
ACS/WFC 10918
Reducing Systematic Errors on the Hubble Constant:
Metallicity
Calibration of the
Reducing the systematic errors on the Hubble constant is
still of
significance and of immediate importance to modern
cosmology. One of the
largest remaining uncertainties in the Cepheid- based
distance scale
{which itself is at the foundation of the HST Key Project
determination
of H_o} which can now be addressed directly by HST, is the
effect of
metallicity on the Cepheid Period-Luminosity relation. Three
chemically
distinct regions in M101 will be used to directly measure
and thereby
calibrate the change in zero point of the
range of metallicities that run from SMC-like, through
Solar, to
metallicities as high as the most metal- enriched galaxies
in the pure
Hubble flow. ACS for the first time offers the opportunity
to make a
precise calibration of this effect which currently accounts
for at least
a third of the total systematic uncertainty on Ho. The
calibration will
be made in the V and I bandpasses so as to be immediately
and directly
applicable to the entire HST Cepheid-based distance scale
sample, and
most especially to the highest-metallicity galaxies that were
hosts to
the Type Ia supernovae, which were then used to extend the
the distance
scale calibration out to cosmologically significant
distances.
WFPC2 10915
ACS Nearby Galaxy Survey
Existing HST observations of nearby galaxies comprise a
sparse and
highly non-uniform archive, making comprehensive comparative
studies
among galaxies essentially impossible. We propose to secure
HST's
lasting impact on the study of nearby galaxies by
undertaking a
systematic, complete, and carefully crafted imaging survey
of ALL
galaxies in the Local Universe outside the Local Group. The
resulting
images will allow unprecedented measurements of: {1} the
star formation
history {SFH} of a >100 Mpc^3 volume of the Universe with
a time
resolution of Delta[log{t}]=0.25; {2} correlations between
spatially
resolved SFHs and environment; {3} the structure and
properties of thick
disks and stellar halos; and {4} the color distributions,
sizes, and
specific frequencies of globular and disk clusters as a
function of
galaxy mass and environment. To reach these goals, we will
use a
combination of wide-field tiling and pointed deep imaging to
obtain
uniform data on all 72 galaxies within a volume-limited
sample extending
to ~3.5 Mpc, with an extension to the M81 group. For each
galaxy, the
wide-field imaging will cover out to ~1.5 times the optical
radius and
will reach photometric depths of at least 2 magnitudes below
the tip of
the red giant branch throughout the limits of the survey
volume. One
additional deep pointing per galaxy will reach SNR~10 for
red clump
stars, sufficient to recover the ancient SFH from the
color-magnitude
diagram. This proposal will produce photometric information
for ~100
million stars {comparable to the number in the SDSS survey}
and uniform
multi-color images of half a square degree of sky. The
resulting archive
will establish the fundamental optical database for nearby
galaxies, in
preparation for the shift of high-resolution imaging to the
near-infrared.
NIC3 10899
Identifying z>7 galaxies from J-dropouts
NICMOS Parallel Imaging campaigns covered enough sky {250
pointings}
with enough sensitivity in the 110W and 160W filters to
identify 6
extremely red resolved sources which are prime candidates
for J-band
dropouts. Their complete absence of detectable J band flux
can be caused
by an opaque Lyman cut-off at z=8-10. We propose to followup
these
candidates with NICMOS imaging and jointly propose Spitzer
IRAC
photometry. Deep F110W and Spitzer/IRAC 3.5/4.8 micron
imaging will
confirm if any of these candidates are indeed Lyman Break
galaxies
observed less than 500 Myrs after the Big Bang. Genuine LBGs
will remain
undetected in F110W, while being detected with flat spectra
in the IRAC
bands. The combined SED will provide information about the
stellar mass
of these galaxies, and the possible presence of evolved
stars or dust
reddening. The proposed observations will be sensitive
enough to detect
the F110W flux from galaxies as red as {J-H}=2.8 {AB mags, 5
sigma}. If
any of the candidates are detected with bluer colors, they
will most
likely be exceptional "Distant Red Galaxies" at z
of 4 to 6. The
proposed data will constrain the stellar populations of
these
extraordinarily red galaxies, which would be candidates for
the
earliest, most massive galaxies which formed.
NIC1 10879
A search for planetary-mass companions to the nearest L
dwarfs -
completing the survey
We propose to extend the most sensitive survey yet
undertaken for very
low-mass companions to ultracool dwarfs. We will use NICMOS
to complete
imaging of an all-sky sample of 87 L dwarfs in 80 systems
within 20
parsecs of the Sun. The combination of infrared imaging and
proximity
allows us to search for companions with mass ratios
q>0.25 at
separations exceeding ~3 AU, while probing companions with
q>0.5 at ~1.5
AU separation. This resolution is crucial, since no
ultracool binaries
are known in the field with separations exceeding 15 AU.
Fifty L dwarfs
from the 20-parsec sample have high-resolution imaging,
primarily
through our Cycle 13 HST proposal which identified six new
binaries,
including an L/T system. Here, we propose to target the
remaining 30
dwarfs
ACS/HRC 10878
An ACS Prism Snapshot Survey for z~2 Lyman Limit Systems
We propose to conduct a spectroscopic survey of Lyman limit
absorbers at
redshifts 1.7 < z < 2.2, using ACS/HRC and the PR200L
prism. We have
selected 100 quasars at 2.3 < z < 2.6 from the Sloan
Digital Sky Survey
Spectroscopic Quasar sample, for which no BAL signature is
found at the
QSO redshift and no strong metal absorption lines are
present at z > 2.3
along the lines of sight. The survey has three main
observational goals.
First, we will determine the redshift frequency dN/dz of the
LLS over
the column density range 16.3 <log N_HI < 20.3 cm^-2.
Second, we will
measure the column density frequency distribution f{N} for
the partial
Lyman limit systems {PLLS} over the column density range
16.3 < log N_HI
< 17.5 cm^-2. Third, we will identify new sightlines for
measurements of
the primordial D/H ratio. With this survey, we will also
constrain two
key quantities of cosmological relevance: First, the
measurements of
dN/dz for optically thick LLS and f{N} for the PLLS are
critical to
estimating the attenuation of extragalactic ionizing sources
{e.g.
QSOs}. Currently, uncertainties in dN/dz and f{N} are the
greatest
sources of uncertainty for inferring the shape and intensity
of the UV
background radiation field. Second, we will estimate the
amount of
metals in the LLS using the f{N} and ground based
observations of metal
line transitions. It is possible that a significant fraction
of the
"missing metals" at z~2 are associated with these
highly ionized
absorbers. Third, analysis of the LLS lends to
investigations of the
interface between galaxies {i.e. the damped Lyman alpha
systems} and the
intergalactic medium {i.e. the Lyman alpha forest}. This
survey is ideal
for a snapshot observing program, because the on-object
integration
times are less than 10 minutes, and the targets cover the
majority of
the northern sky.
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}.
NIC3 10861
An ACS Treasury Survey of the Coma cluster of galaxies
We propose to use the unique spatial resolution of HST and
ACS to
construct a Treasury imaging survey of the core and infall
region of the
richest local cluster, Coma. We will observe samples of
thousands of
galaxies down to magnitude B=27.3 with the aim of studying
in detail the
dwarf galaxy population which, according to hierarchical
models of
galaxy formation, are the earliest galaxies to form in the
universe. Our
initial scientific objectives are: 1} A study of the
structure of the
dwarf galaxies, including scaling laws, nuclear structure
and
morphology, to compare with hierarchical and evolutionary
models of
their formation. 2} A study of the stellar populations from
colors and
color gradients, and how the internal chemical evolution of
galaxies is
affected by interaction with the cluster gaseous and galaxy
environment.
3} To determine the effect of the cluster environment upon
morphological
features, disks, bulges and bars, by comparing these
structure in the
Coma sample with field galaxy samples. 4} Identification of
dwarf galaxy
samples for further study with the new generation of
multi-object and
integral-field spectrographs on 8-10 metre class telescopes
such as
Keck, Subaru, Gemini, and GTC. This is the first such survey
of a nearby
rich cluster. It will provide a key database for studies of
galaxy
formation and evolution, and a very needed reference for
comparison with
similar galaxy surveys both in lower density environments in
the nearby
universe, and in high density environments at high
redshifts.
NIC2 10849
Imaging Scattered Light from Debris Disks Discovered by the
Spitzer
Space Telescope around 21 Sun-like Stars
We propose to use the high-contrast capability of the NICMOS
coronagraph
to image a sample of newly discovered circumstellar disks
associated
with Sun-like stars. These systems were identified by their
strong
thermal infrared {IR} emission with the Spitzer Space
Telescope as part
of the Spitzer Legacy Science program titled "The
Formation and
Evolution of Planetary Systems" {FEPS, P.I.: M.Meyer}.
Modeling of the
thermal excess emission from the spectral energy
distributions alone
cannot distinguish between narrowly confined high-opacity
disks and
broadly distributed, low-opacity disks. By resolving light
scattered by
the circumstellar material, our proposed NICMOS observations
can break
this degeneracy, thus revealing the conditions under which
planet
formation processes are occuring or have occured. For three
of our
IR-excess stars that have known radial-velocity planets,
resolved
imaging of the circumstellar debris disks may further offer
an
unprecedented view of planet-disk interactions in an
extrasolar
planetary system. Even non-detections of the light scattered
by the
circumstellar material will place strong constraints on the
disk
geometries, ruling out disk models with high optical depth.
Unlike
previous disk imaging programs, our program contains a
well-defined
sample of ~1 solar mass stars covering a range of ages from
3 Myr to 3
Gyr, thus allowing us to study the evolution of disks from
primordial to
debris for the first time. The results from our program will
greatly
improve our understanding of the architecture of debris
disks around
Sun-like stars, and will create a morphological context for
the
existence of our own solar system. This proposal is for a
continuation
of an approved Cycle 14 program {GO/10527, P.I.: D. Hines}.
NIC2 10847
Coronagraphic Polarimetry of HST-Resolved Debris Disks
We propose to take full advantage of the recently
commissioned
coronagraphic polarimetry modes of ACS and NICMOS to obtain
imaging
polarimetry of circumstellar debris disks that were imaged
previously by
the HST coronagraphs, but without the polarizers. It is well
established
that stars form in gas-rich protostellar disks, and that the
planets of
our solar system formed from a circum-solar disk. However,
the
connection between the circumstellar disks that we observe
around other
stars and the processes of planet formation is still very
uncertain.
Mid-IR spectral studies have suggested that disk grains are
growing in
the environments of young stellar objects during the
putative
planet-formation epoch. Furthermore, structures revealed in
well
resolved images of circumstellar disks suggest gravitational
influences
on the disks from co-orbital bodies of planetary mass.
Unfortunately,
existing imaging data provides only rudimentary information
abou the
disk grains and their environments. Our proposed
observations, which can
be obtained only with HST, will enable us to quantitatively
determine
the sizes of the grains and optical depths as functions of
their
location within the disks {i.e., detailed tomography}. Armed
with these
well-determine physical and geometrical systemic parameters,
we will
develop a set of self-consistent models of disk structures
to
investigate possible interactions between unseen planets and
the disks
from which they formed. Our results will also calibrate
models of the
thermal emission from these disks, that will in turn enable
us to infer
the properties of other debris disks that cannot be
spatially resolved
with current or planned instruments and telescopes.
ACS/HRC/WFPC2/NIC3 10842
A Cepheid Distance to the Coma Cluster
We propose to use the Advanced Camera for Surveys to search
for Cepheid
variables in two spiral galaxies in the core of the Coma
cluster. A
direct application of the canonical primary distance
indicator at 100
Mpc will measure the far-field Hubble constant free of many
of the
systematic uncertainties which beset current determinations
relying on
secondary indicators. Establishing the far-field H_o with
Cepheids will
provide one of the strongest links in the extragalactic
distance scale
and will directly calibrate the fiducial fundamental plane
of elliptical
galaxies in Coma. With ACS/HRC, S/N=5 to 10 or better can be
reached for
Cepheids with periods of 40d to 70d at mean light in 5
orbits with the
F606W filter if H_o=72 km/s/Mpc. Efficient detection and
phasing can be
done with twelve epochs optimally spaced for periods of
40-70d.
NIC2, ACS/WFC 10802
SHOES-Supernovae, HO, for the Equation of State of Dark
energy
The present uncertainty in the value of the Hubble constant
{resulting
in an uncertainty in Omega_M} and the paucity of
redshifts exceeding 1 are now the leading obstacles to
determining the
nature of dark energy. We propose a single, integrated set
of
observations for Cycle 15 that will provide a 40%
improvement in
constraints on dark energy. This program will observe known
Cepheids in
six reliable hosts of
uncertainty in H_0 by a factor of two because of the smaller
dispersion
along the instability strip, the diminished extinction, and
the weaker
metallicity dependence in the infrared. In parallel with
ACS, at the
same time the NICMOS observations are underway, we will
discover and
follow a sample of
measurements, along with prior constraints from WMAP, will
provide a
great improvement in HST's ability to distinguish between a
static,
cosmological constant and dynamical dark energy. The Hubble
Space
Telescope is the only instrument in the world that can make
these IR
measurements of Cepheids beyond the Local Group, and it is
the only
telescope in the world that can be used to find and follow
supernovae at
z > 1. Our program exploits both of these unique
capabilities of HST to
learn more about one of the greatest mysteries in science.
ACS/HRC 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.
ACS/WFC 10760
Black Hole X-ray Novae in M31
We have been carring out a Chandra {GO+GTO} and HST {GO}
program to find
Black Hole X-ray Nova {BHXN} and their optical counterparts
in M31 for
several years. To date we have found >2 dozen BHXN and 3
HST optical
counterparts for these BHXN. Our results suggest a rather
high ratio of
BH to neutron star {NS} binaries, or a high duty cycle for
the BHXN. We
propose to continue this program, with the goal of
determining the
orbital period distribution and duty cycles of these BHXN.
Current
results yield 3 orbital periods and 2 upper limits. Our
proposed
observations will ~double the total number of periods and
therefore
yield sufficient numbers to make a first approximation of
the orbital
period distribution. The orbital period distribution is the
fundamental
observable parameter any binary stellar evolution models
must match, and
the duty cycle is very poorly known but directly influences
the binary
lifetime. M31 is the only galaxy in which this
extra-galactic study of
BHXN is feasible.
ACS/WFC 10582
Probing The Galaxy-wide Globular Cluster - Low Mass X-ray
Binary
Connection in Early-type Galaxies
The combination of high-resolution imaging from Hubble {HST}
and Chandra
{CXO} has completely revolutionized our understanding of
extragalactic
low-mass X-ray binaries {LMXBs} and globular clusters {GCs};
however,
studies have been limited by short X-ray exposures and
relatively small
fields. NGC 4697 amd NGC 4365 are relatively simple
elliptical galaxies
in the X- ray that will have deep CXO observations. We
propose ACS
observations in six flanking fields per galaxy to provide a
study of the
GC-LMXB connection in normal early-type galaxies with
unprecedented
depth, spatial resolution and areal coverage. Combined with
existing
central field observations, we will detect ~900 and ~2700
GCs GCs in
most of NGC 4697 and all of NGC 4365. These two galaxies
will have the
greatest number of detected GC-LMXBs to date {~70 &
120}. We will
measure the fraction of LMXBs found in GCs, and the fraction
of GCs
which contain LMXBs, as a function of X-ray luminosity,
galactocentric
distance, color, GC half-light radius, and local GC specific
frequency.
We will test existing models of GC formation/evolution and
LMXB
formation/evolution. Using the radial profile of optical
light, GCs, and
LMXBS, we will determine the percentage of field LMXBs which
may have
originated in GCs.
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are
preliminary reports
of potential non-nominal performance that will be
investigated.)
HSTARS:
10620 - GSAcq (1,3,1) resulted in Fine Lock Back-up (1,0,1)
GSAcq (1,3,1)scheduled from 012/14:13:46-14:21:09 resulted in Fine Lock
Back-up (1,0,1) on FGS 3. Mnemonics QF3STOPF and QSTOP were flagging.
OBAD #1: V1 617.97, V2 1631.32, V3 -84.35, RSS 1746.48
OBAD #2: V1 16.33, V2 2.00, V3 17.35, RSS 23.91
OBAD MAP: V1 2.97, V2 -4.90, V3 -0.72, RSS 5.77
10622 - REacq(2,1,2) failed due to search radius limit exceeded
REacq(2,1,2)scheduled at 012/20:46:51 failed during LOS. AT AOS
(21:01:15) flags were set indicating the REacq(2,1,2) failed due to
search radius limit exceeded on FGS 2.
OBAD1: V1=-35.26,V2=2294.77,V3=-20.20,RSS=2295.13
OBAD2: V1=-2.61,V2=-12.14,V3=0.49,RSS=12.42
The Map at 20:54:18 showed errors of V1=0.73,V2=71.41,V3=-5.36, RSS=71.62
10623 - GSacq(2,0,2) failed to RGA control
GSacq(2,0,2) scheduled at 013/01:53:51 failed due to receiving stop
flage QF2STOPF on FGS 2 at 01:56:24. The OBAD before the GSAcq showed
errors of V1=-3.24, V2=3.36, V3=-3.22, and RSS=5.67.
REAcq(2,0,2) scheduled at 03:22:38 failed at 03:27:48 due to search
radius limit exceeded (FGS 2).
The following mnemonics also flagged QF2SRKEX, QF2STOPF, SESBSLD,
QF2SSDIF AND QSRCHEXC.
The REacq(2,0,2) scheduled at 04:40:40 was successful
10624 - MAP 1,2 Failed Quaternion (ESB 1903)
At AOS (09:37:55) observed GOBSTAT = "AttDtErr" (Failed quaternion).
Dumped buffer and OBAD tables. Dump analyzer showed
"2007/013/09:26:24.663 Failed Quaternion 5 3 4 32767"
GSacq scheduled at 09:15:36 was successful.
OBAD_ERR_V1 = -48.52
OBAD_ERR_V2 = -27.45
OBAD_ERR_V3 = -67.37
OBAD_ERR_RSS = 87.45
OBAD data prior to Map failure is unavailable until engineering data is dumped.
10625 - GSAcq(1,2,1) failed to RGA Hold (Gyro Control)
GSAcq(1,2,1) scheduled at 013/12:26:58 - 12:35:03 failed to RGA Hold due
to search radius limit exceeded on FGS 1. 486 ESB "a05" (FGS Coarse
Track failed-Search Radius Limit Exceeded was received. Pre-acquisition
OBAD1 (RSS) attitude correction value not available due to LOS. OBAD2
had (RSS) value of 14.35 arcseconds.
Subsequent REacqs(1,2,1) scheduled at 013/14:03:56, 013/15:38:03 both
failed to RGA Hold (Gyro Control) due to search radius limit exceeded on
the primary FGS 1.
10626 - GSAcq(1,3,1) failed to RGA Hold (Gyro Control)
Upon acquisition of signal at 014/16:44:16, the GSAcq(1,3,1) scheduled
at 014/15:49:54 - 014/15:57:59 was observed to have failed to RGA Hold
due to search radius limit exceeded indication flag on FGS-1.
Pre-acquisition OBADs (RSS) attitude correction values not available due
to LOS. Post-acquisition OBAD/MAP had 3-axis error (RSS) value of 8.57
arcseconds. Subsequent REacq(1,3,1) at 014/17:25:03 also failed to RGA
Hold due to search radius limit exceeded on the primary FGS-1.
10627 - GSAcq(1,2,2) failed due to SRLEX on FGS 2
At AOS (11:19:39) discovered that GSAcq(1,2,2) had failed due to SRLEX
for FGS2.
Pre GSAcq OBAD unavailable until engineering dump is completed.
MAP RSS was 1.65 a/s.
10631 - GSAcq(2,3,2) failed to RGA Hold (Gyro
Control)
GSAcq(2,3,2) scheduled at 015/19:23:13 - 19:31:18 failed to RGA Hold due
to (QF2STOPF) stop flag indication on the primary FGS-2. Pre-acquisition
OBADs showed (RSS) attitude correction values of 5615.13 and 68.78
arcseconds. Post-acquisition OBAD/MAP not scheduled. Subsequent
REacqs(2,3,2) scheduled at 015/20:39:48, 015/22:18:52 and 015/23:58:10
all failed to RGA Hold due to stop flag and search radius limit exceeded
on the secondary FGS-3.
COMPLETED OPS REQUEST:
17543-2 - Dump OBAD tables after failed OBAD
COMPLETED OPS NOTES: (None)
SCHEDULED
SUCCESSFUL
FGS GSacq
31
26
FGS
REacq
28
18
OBAD with Maneuver 118
118
SIGNIFICANT EVENTS: (None)