HUBBLE
SPACE TELESCOPE - Continuing to collect World Class Science
DAILY
REPORT # 4508
PERIOD
COVERED: UT December 14,15,16, 2007 (DOY 348,349,350)
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.
FGS
11462
FGS1r,
FGS2r, and FGS3 Pre-SM4 Performance
This
proposal is the first of a pair of proposals that monitors the
characteristics
of HST's two " continuing"
Fine Guidance Sensors across
the
boundary of the servicing mission SM4. This proposal obtains the
pre-SM4
measurements. Proposal 11463 gathers the same data but for the
post-SM4
baseline. For each FGS, stars from a selected field in the
standard
astrometric Galactic cluster M35 are observed in Position mode.
This
provides a measurement of their relative positions, which in turn
provides
an effective means to detect and monitor any changes in the FGS
optical
distortions and plate scales. If out
of tolerance, the need for a
re-
calibration of the particular FGS's distortions will be indicated.
The
FGS-FGS alignments will also be monitored across the SM boundary.
This
will be done by using the same guide star pairs in the
corrresponding
proposal 11463. Finally, this proposal and 11463 include
Transfer
mode observations of selected M35 stars. These observations
will
obtain S-curves at the center and at two off-center field points in
each
FGS FOV. These data will provide insight as to whether or not the
relative
alignment of the FGS optical train with the HST OTA has
changed.
If changes larger than tolerance are observed, it will be
necessary
to activate the appropriate contingency proposal that will
obtain
S-curves are several locations in the FGS FOV to facilitate a
re-computation of the
optimal values of K-factors that are used in the
acquisition
and tracking of guide stars (and astrometry targets). This
proposal
requires a total of 4 HST orbit to support the FGS2r and FGS3
observations.
The FGS1r observations are available from the FGS Cycle 16
Astrometry
calibration plan.
FGS
11315
Monitoring
FGS1r's Interferometric Response as a Function of Spectral
Color
This
proposal uses FGS1r in Transfer mode to observe single stars to
obtain
the interference fringes of point sources. These data are used by
FGS
data analysis tools for studying binary and hierarchical multiple
star
systems. Visit 01 observes three stars in M35 over the FGS1r FOV as
a
precursor to a corresponding visit in FGS/SM4 proposal 11463.
NIC3
11306
Direct
radius measurement of the Neptune-size transiting exoplanet
GJ436b
We
propose to measure the radius of the first transiting Neptune-class
extrasolar
planet, GJ 436b. The transits of this 22-Earth-mass planet
around
a nearby M dwarf were recently detected by our team. Ground-based
photometric
observations indicate a planet size compatible with a
Neptune-like
structure or an "Ocean Planet". A direct radius
determination
from an HST infrared lightcurve will provide a much more
direct
measurement of the radius and density of the planet. GJ 436b is
the
nearest known transiting exoplanet, as well as the smallest and
lightest,
by a large margin. The high planet-to-star contrast in the
infrared
make it very favorable for detailed studies. NICMOS 1-2 microns
observations,
in addition to measuring its size, may reveal water
absorption
from its outer atmosphere.
ACS/SBC
11215
New
Sightlines for the Study of Intergalactic Helium: Dozens of
High-Confidence,
UV-Bright Quasars from SDSS/GALEX
The
reionization of IGM helium is thought to have occurred at redshifts
of
z=3 to 4. Detailed study of HeII Lyman-alpha absorption toward a
handful
of QSOs at 2.7<z<3.3 demonstrated the high potential of such IGM
probes,
but the critically small sample size limits confidence in
cosmological
inferences. The requisite unobscured sightlines to high-z
are
extremely rare, but SDSS provides 5800, z>3.1 QSOs potentially
suitable
for HeII studies. We've cross-correlated SDSS quasars with
GALEX
UV sources to obtain dozens of new, high confidence, candidate
sightlines
{z=3.1-4.9} potentially useful for detailed HeII studies with
HST.
We propose brief, 2-orbit reconnaissance ACS SBC prism exposures
toward
each of the best dozen new quasars, to definitively verify UV
flux
down to HeII. Our combined SDSS/GALEX selection insures a high
confirmation
rate, as the quasars are already known to be UV bright in
GALEX.
Our program will provide a statistical sample of HeII sightlines
extending
to high redshift, enabling future long exposure follow-up
spectra
with the SBC prism, or superb quality COS or STIS spectra after
SM4.
Stacks of our prism spectra will also directly yield ensemble
information.
Ultimately, the new sightlines will enable confident
measures
of the spectrum and evolution of the ionizing background, the
evolution
of HeII opacity, the epoch of helium reionization, and the
density
of IGM baryons.
FGS
11213
Distances
to Eclipsing M Dwarf Binaries
We propose
HST FGS observations to measure accurate distances of 5
nearby
M dwarf eclipsing binary systems, from which model-independent
luminosities
can be calculated. These objects have either poor or no
existing
parallax measurements. FGS parallax determinations for these
systems,
with their existing dynamic masses determined to better than
0.5%,
would serve as model-independent anchor points for the low-mass
end
of the mass-luminosity diagram.
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 W Vir
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/NIC2
11193
A
comprehensive study of the low-mass stellar population in the Galactic
starburst
region NGC 3603
NGC
3603, located in the Carina spiral arm, is one of the most luminous
giant
HII regions in the Milky Way, and as such it is often referred to
as
a prime template for extragalactic starbursts. While previous studies
were
focusing on the high and intermediate mass stellar content of the
central
starburst cluster, which powers the HII region, the effects of
the
starburst environment with its large number of ionizing O stars on
the
emerging low-mass population are unknown. As the most nearby, most
easily
accessible starburst, NGC 3603 provides the best testbed to study
the
long-lived, low-mass stars originating from a starburst environment.
Taking
advantage of the large field of view and high sensitivity of
WFPC2,
we want to survey the stellar population in an area of 10pc x
10pc
{6' x 6'} down to a mass limit of 0.2 to 0.5 Mo. This will enable
us
to derive the total cluster mass, look for spatial variations in the
initial
mass function, determine the age of the dispersed low-mass
population
in the HII region and search for evidence of sequential star
formation.
Ultimately, we aim at reconstructing the low-mass stellar
initial
mass function of the starburst epoch in NGC 3603, which in turn
will
advance our understanding of extragalactic starburst phenomena and
the
emerging low-mass stars as observed in ancient populations. The
observations
of NGC 3603 are part of our larger effort to study intense
star-forming
regions in the Milky Way, LMC and SMC.
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 Monte Carlo
technique to
optimally
schedule our observations.
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.
NIC3
11082
NICMOS
Imaging of GOODS: Probing the Evolution of the Earliest Massive
Galaxies,
Galaxies Beyond Reionization, and the High Redshift Obscured
Universe
(uses
ACS/SBC and WFPC2)
Deep
near-infrared imaging provides the only avenue towards
understanding
a host of astrophysical problems, including: finding
galaxies
and AGN at z > 7, the evolution of the most massive galaxies,
the
triggering of star formation in dusty galaxies, and revealing
properties
of obscured AGN. As such, we propose to observe 60 selected
areas
of the GOODS North and South fields with NICMOS Camera 3 in the
F160W
band pointed at known massive M > 10^11 M_0 galaxies at z > 2
discovered
through deep Spitzer imaging. The depth we will reach {26.5
AB
at 5 sigma} in H_160 allows us to study the internal properties of
these
galaxies, including their sizes and morphologies, and to
understand
how scaling relations such as the Kormendy relationship
evolved.
Although NIC3 is out of focus and undersampled, it is currently
our
best opportunity to study these galaxies, while also sampling enough
area
to perform a general NIR survey 1/3 the size of an ACS GOODS field.
These
data will be a significant resource, invaluable for many other
science
goals, including discovering high redshift galaxies at z > 7,
the
evolution of galaxies onto the Hubble sequence, as well as examining
obscured
AGN and dusty star formation at z > 1.5. The GOODS fields are
the
natural location for HST to perform a deep NICMOS imaging program,
as
extensive data from space and ground based observatories such as
Chandra,
GALEX, Spitzer, NOAO, Keck, Subaru, VLT, JCMT, and the VLA are
currently
available for these regions. Deep high-resolution
near-infrared
observations are the one missing ingredient to this
survey,
filling in an important gap to create the deepest, largest, and
most
uniform data set for studying the faint and distant universe. The
importance
of these images will increase with time as new facilities
come
on line, most notably WFC3 and ALMA, and for the planning of future
JWST
observations.
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
11022
WFPC2
Cycle 15 Decontaminations and Associated Observations
This
proposal is for the WFPC2 decons. Also included are instrument
monitors
tied to decons: photometric stability check, focus monitor,
pre-
and post-decon internals {bias, intflats, kspots, & darks}, UV
throughput
check, VISFLAT sweep, and internal UV flat check.
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.
FGS
10928
Calibrating
Cosmological Chronometers: White Dwarf Masses
We
propose to use HST/FGS1R to determine White Dwarf {WD} masses. The
unmatched
resolving power of HST/FGS1R will be utilized to follow up
four
selected WD binary pairs. This high precision obtained with
HST/FGS1R
simply cannot be equaled by any ground based technique. This
proposed
effort complements that done by CoI Nelan in which a sample of
WDs
is being observed with HST/FGS1R. This proposal will dramatically
increase
the number of WDs for which dynamical mass measurements are
possible,
enabling a better calibration of the WD mass-radius relation,
cooling
curves, initial to final mass relations, and ultimately giving
important
clues to the star formation history of our Galaxy and the age
of
its disk as well as in other galaxies.
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.
WFPC2
10877
A
Snapshot Survey of the Sites of Recent, Nearby Supernovae
During
the past few years, robotic {or nearly robotic} searches for
supernovae
{SNe}, most notably our Lick Observatory Supernova Search
{LOSS},
have found hundreds of SNe, many of them in quite nearby
galaxies
{cz < 4000 km/s}. Most of the objects were discovered before
maximum
brightness, and have follow-up photometry and spectroscopy; they
include
some of the best-studied SNe to date. We propose to conduct a
snapshot
imaging survey of the sites of some of these nearby objects, to
obtain
late-time photometry that {through the shape of the light and
color
curves} will help reveal the origin of their lingering energy. The
images
will also provide high-resolution information on the local
environments
of SNe that are far superior to what we can procure from
the
ground. For example, we will obtain color-color and color-magnitude
diagrams
of stars in these SN sites, to determine the SN progenitor
masses
and constraints on the reddening. Recovery of the SNe in the new
HST
images will also allow us to actually pinpoint their progenitor
stars
in cases where pre- explosion images exist in the HST archive.
This
proposal is an extension of our successful Cycle 13 snapshot survey
with
ACS. It is complementary to our Cycle 15 archival proposal, which
is
a continuation of our long-standing program to use existing HST
images
to glean information about SN environments.
NIC3
10874
Search
for Extremely Faint z>7 Galaxy Population with Cosmic Lenses
Deep
UDF/NICMOS observations find a significant decrease in the number
of
galaxy candidates between redshift z=6 and 7, but the sample at z>7
is
too small to draw conclusions. From our observations of 15 clusters
we
have found a number of bright z- dropouts, aided by the lensing
amplification.
We propose deep NICMOS observations of the best cases of
cluster
centers where a rare combination of a significant lensing effect
and
the richness in z-band dropouts in background may dramatically
increase
the discovery rate. The NICMOS images will reach an
unprecendented
depth of AB~27.8, or AB~30 in nonlensed intrinsic
magnitude,
and may find many faint {~0.05L*} galaxies at z=7-10, at a
level
that the UDF reaches for z~6 objects. We produce precision mass
distribution
maps from weak-lensing models, which enable us to derive
the
candidates' intrinsic magnitudes and their luminosity function. The
knowledge
of such faint galaxy population at z>7 will facilitate the
models
of the IGM reionization and future JWST planning.
ACS/SBC
10872
Lyman
Continuum Emission in Galaxies at z=1.2
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
escape
fractions of a few percent, up to 10%, with very few detections
{as
opposed to upper limits} having been reported. No detections have
been
reported in the epochs between z=0.1 and z=2. We propose to measure
the
fraction of escaping Lyman continuum radiation from 15 luminous
z~1.2
galaxies in the GOODS fields. Using the tremendous sensitivity of
the
ACS Solar- blind Channel, we will reach AB=30 mag., allowing us to
detect
an escape fraction of 1%. We will correlate the amount of
escaping
radiation with the photometric and morphological properties of
the
galaxies. A non-detection in all sources would imply that QSOs
provide
the overwhelming majority of ionizing radiation at z=1.3, and it
would
strongly indicate that the properties of galaxies at higher
redshift
have to be significantly different for galaxies to dominate
reionization.
The deep FUV images will also be useful for extending the
FUV
study of other galaxies in the GOODS fields.
WFPC2
10812
Space
Motions for the Draco and Sextans Dwarf Spheroidal Galaxies
We
will use the powerful astrometric capabilities of HST to measure
proper
motions for the Draco and Sextans dwarf spheroidal galaxies that
will
yield tangential velocities accurate to about 30 km/s. These two
galaxies
are the last inside a galactocentric radius of 200~kpc without
measured
proper motions. Knowing their orbits is critical for our
understanding
of the low-luminosity satellites of the Milky Way. In
particular
they are critical for understanding why Ursa Minor has
survived
tidal disruption on its plunging orbit and how Carina formed a
large
intermediate-age stellar population despite its small mass.
FLIGHT
OPERATIONS SUMMARY:
Significant
Spacecraft Anomalies: (The following are preliminary reports
of
potential non-nominal performance that will be investigated.)
HSTARS:
11100
- REACQ(2,1,2) fine lock backup on FGS 2
REACQ(2,1,2) at 348/19:23:02 acquired in fine lock backup on FGS 2
only,
with QF1STOPF and QSTOP flags set on FGS 1 at 19:27:37. No other
flags
were seen. Previous acquisition at 17:50:11 was successful.
11101
- GSAcq(2,3,2) failed to RGA Hold(gyro Control)
GSAcq(2,3,2) scheduled at 349/19:15:18 - 19:23:23 failed to RGA
Hold due
to (QF2STOPF) stop flag indication on FGS-2 during acquisition
walkdown.
Scheduled Astrometry FGS1 did not attempt. Pre-acquisition OBADs
had
(RSS) values of 931.61 and 4.46 arcseconds.
OBAD/MAP scheduled at 349/19:23:23 had 3-axis (RSS) value of 4.18
arcseconds.
11102
- GSAcq(1,2,1) failed to RGA Hold
At AOS (350/00:51:00) observed that GSAcq (1,2,1) scheduled from
00:41:58 - 00:49:52 had failed to RGA Hold due to QSTOP &
QF2STOPF flags
on FGS 2. No 486 ESB messages were received. Due to LOS, the data
from
OBAD 1 is unavailable till an engineering data dump is performed.
OBAD 2
data showed the following results: V1 1.39, V2 4.19, V3 3.00, RSS
5.34.
OBAD MAP at 01:38:52 showed the following results: V1 -2.38, V2
-11.86,
V3 9.58, RSS 15.43
REAcq(1,2,1) @ 350/02:06:00 was successful
11103
- GSAcq(2,1,2) results in finelock backup (2,0,2) using FGS-2
Upon acquisition of signal at 350/20:35:20, the GSAcq(2,1,2)
scheduled
at 350/19:33:11 - 19:41:16 had resulted to finelock backup (2,0,2)
using
FGS-2,due to stop flag (QF1STOPF) indication on FGS-1.
Pre-acquisition
OBAD1 had attitude error correction (RSS) value of 1824.19
arcseconds.
OBAD2 attitude error correction (RSS) not available pending future
ETR
Dump. Post-acq OBAD/MAP had (RSS) value of 19.65 arcseconds.
Subsequent
REacq(2,1,2) scheduled at 350/21:07:49 using same guide star pair
resulted to finelock backup (2,0,2) using FGS-2 due to stop flag
on
FGS-1.
11104
- GSAcq(1,2,2) resulted in Fine Lock Back-up (1,0,1)
GSAcq (1,2,2) scheduled from 09:36:13 - 09:43:26 resulted in Fine
Lock
Back-up (1,0,1) using FGS 1. This was due to QF2STOPF flag on FGS
2 and
QSTOP flag. At 09:39:50 received 486 ESB message 1808 "TxG
FHST Sanity
Check Failed". Pre-acquisition OBAD1 had attitude error correction
(RSS)
value of 2691.62 arcseconds. Pre-acquisition OBAD2 had attitude
error
correction (RSS) value of 5.39 arcseconds. Post acquisition OBAD
MAP was
not scheduled.
COMPLETED
OPS REQUEST: (None)
COMPLETED
OPS NOTES: (None)
SCHEDULED
SUCCESSFUL
FGS
GSacq
27
25
FGS
REacq
17
17
OBAD
with Maneuver 88
88
SIGNIFICANT
EVENTS:
FSW
3.1 Release B was successfully installed into HST486 EEPROM at
348/13:00:34.
The load completed successfully and the valid block
counter
was verified. The post installation EEPROM dump was completed at
348/15:16:59,
and the Compare Best Estimate of the dump file against the
EEPROM
load showed no miscompares and no missing blocks. FSW also
verified
the contents of the memory dump.