Daily Report #4598

HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science

DAILY REPORT # 4598

PERIOD COVERED: UT April 25,26,27, 2008 (DOY 116,117,118)

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 images. Each observation will need its own CRMAP, as
different SAA passages leave different imprints on the NICMOS detectors.

NIC3 11334

NICMOS Cycle 16 Spectrophotometry

Observation of the three primary WD flux standards must be repeated to
refine the NICMOS absolute calibration and monitor for sensitivity
degradation. So far, NICMOS grism spectrophotometry is available for only
~16 stars with good STIS spectra at shorter wavelengths. There are more in
the HST CALSPEC standard star data base with good STIS spectra that would
also become precise IR standards with NICMOS absolute SED measurements.
Monitoring the crucial three very red stars (M, L, T) for variability and
better S/N in the IR. Apparent variability was discovered at shorter
wavelengths during the ACS cross-calibration work that revealed a ~2%
discrepancy of the cool star fluxes with respect to the hot primary WD
standards. About a third of these stars are bright enough to do in one
orbit, the rest require 2 orbits.

WFPC2/NIC2 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.

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 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 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!

NIC3/WFPC2 11192

NICMOS Confirmation of Candidates of the Most Luminous Galaxies at z 7

While the deepest pencil-beam near-IR survey suggested that the Universe was
too young to build up many luminous galaxies by z ~ 7--8 (Bouwens &
Illingworth 2006), there is also evidenc indicating the contrary. It is now
known that some galaxies with stellar masses of M1e10 Msun were already in
place by z ~ 6--7, which strongly suggests that their progenitors should be
significantly more luminous, and hence detectable in deep, wide-field
near-IR surveys (Yan et al. 2006). As galaxies at such a high redshift
should manifest themselves as "dropouts" from the optical, we have carried
out a very wide-field, deep near-IR survey in the GOODS fields to search for
z-band dropouts as candidates of galaxies at z 7. In total, six promising
candidates have been found in ~ 300 sq. arcmin to J_AB ~ 24.5 mag
(corresponding to restframe M(UV) -22.5 mag at z ~ 7). By contrast, the
galaxy luminosity function (LF) suggested in BI06 would predict at most 3--5
galaxies over the entire 2-pi sky at this brightness level. Here we propose
to observe these candidates with NIC3 in F110W and F160W to further
investigate their nature. If any of these candidates are indeed at z 7,
the result will lead to a completely new picture of star formation in the
early universe. If none of our candidates are consistent with being at z
7, then the depth and area of our near-IR survey (from which the candidates
are drawn) will let us set a very stringent upper limit on the bright end of
the galaxy LF at those redshift. As a result, our program will still be able
to provide new clues about the processes of early galaxy formation, such as
their dust contents and their merging time scale (Yan et al. 2006).

WFPC2 11160

Escape fraction and stellar populations in a highly magnified Lyman-Break
Galaxy

Understanding how star-forming galaxies contribute to cosmic reionization is
one of the frontiers of observational cosmology. A key ingredient in this
issue is measuring the escape fraction of Lyman-continuum photons in high
redshift galaxies (z3). Gravitationally lensed Lyman-break galaxies (LBGs)
act as important laboratories for studying the resolved physical properties
at sub-kpc scales with high signal-to-noise. Correlating the local escape
fraction with physical parameters derived from stellar population modeling
(such as the star formation rate, age and reddening) will offer new insights
into understanding the physical processes involved with the production of
ionizing photons. We propose here follow-up observations of the "Cosmic
Eye", a remarkable, highly magnified (x 30), Lyman-break galaxy at z~3.07
using WFPC2 and NICMOS. Deep ultraviolet WFPC2 imaging will provide a
detailed study of variations in the escape fraction, while WFPC2 and
NICMOS/NIC2 imaging will complement the current broad-band detections to
allow a precise modeling of the spatially-dependent spectral energy
distribution. This will allow the first comprehensive analysis between the
escape fraction, the local SED and the dynamics of a distant galaxy.

ACS/SBC 11158

HST Imaging of UV emission in Quiescent Early-type Galaxies

We have constructed a sample of early type galaxies at z~0.1 that have blue
UV-optical colors, yet also show no signs of optical emission, or extended
blue light. We have cross-correlated the SDSS catalog and the Galaxy
Evolution Explorer Medium Imaging Survey to select a sample of galaxies
where this UV emission is strongest. The origin of the UV rising flux in
these galaxies continues to be debated, and the possibility that some
fraction of these galaxies may be experiencing low levels of star formation
cannot be excluded. There is also a possibility that low level AGN activity
{as evidenced by a point source} is responsible We propose to image the UV
emission using the HST/SBC and to explore the morphology of the UV emission
relative to the optical light.

NIC2 11157

NICMOS Imaging Survey of Dusty Debris Around Nearby Stars Across the Stellar
Mass Spectrum

Association of planetary systems with dusty debris disks is now quite
secure, and advances in our understanding of planet formation and evolution
can be achieved by the identification and characterization of an ensemble of
debris disks orbiting a range of central stars with different masses and
ages. Imaging debris disks in starlight scattered by dust grains remains
technically challenging so that only about a dozen systems have thus far
been imaged. A further advance in this field needs an increased number of
imaged debris disks. However, the technical challenge of such observations,
even with the superb combination of HST and NICMOS, requires the best
targets. Recent HST imaging investigations of debris disks were
sample-limited not limited by the technology used. We performed a search for
debris disks from a IRAS/Hipparcos cross correlation which involved an
exhaustive background contamination check to weed out false excess stars.
Out of ~140 identified debris disks, we selected 22 best targets in terms of
dust optical depth and disk angular size. Our target sample represents the
best currently available target set in terms of both disk brightness and
resolvability. For example, our targets have higher dust optical depth, in
general, than newly identified Spitzer disks. Also, our targets cover a
wider range of central star ages and masses than previous debris disk
surveys. This will help us to investigate planetary system formation and
evolution across the stellar mass spectrum. The technical feasibility of
this program in two-gyro mode guiding has been proven with on-orbit
calibration and science observations during HST cycles 13, 14, and 15.

NIC2/NIC2 11155

Dust Grain Evolution in Herbig Ae Stars: NICMOS Coronagraphic Imaging and
Polarimetry

We propose to take advantage of the sensitive coronagraphic capabilities of
NICMOS to obtain multiwavelength coronagraphic imaging and polarimetry of
primordial dust disks around young intermediate-mass stars {Herbig Ae
stars}, in order to advance our understanding of how dust grains are
assembled into larger bodies. Because the polarization of scattered light is
strongly dependent on scattering particle size and composition,
coronagraphic imaging polarimetry with NICMOS provides a uniquely powerful
tool for measuring grain properties in spatially resolved circumstellar
disks. It is widely believed that planets form via the gradual accretion of
planetesimals in gas-rich, dusty circumstellar disks, but the connection
between this suspected process and the circumstellar disks that we can now
observe around other stars remains very uncertain. Our proposed
observations, together with powerful 3-D radiative transfer codes, will
enable us to quantitatively determine dust grain properties as a function of
location within disks, and thus to test whether dust grains around young
stars are in fact growing in size during the putative planet-formation
epoch. HST imaging polarimetry of Herbig Ae stars will complement and extend
existing polarimetric studies of disks around lower-mass T Tauri stars and
debris disks around older main-sequence stars. When combined with these
previous studies, the proposed research will help us establish the influence
of stellar mass on the growth of dust grains into larger planetesimals, and
ultimately to planets. Our results will also let us calibrate models of the
thermal emission from these disks, a critical need for validating the
properties of more distant disks inferred on the basis of spectral
information alone.

WFPC2/NIC3/ACS/SBC 11144

Building on the Significant NICMOS Investment in GOODS: A Bright, Wide-Area
Search for z=7 Galaxies

One of the most exciting frontiers in observational cosmology has been to
trace the buildup and evolution of galaxies from very early times. While
hierarchical theory teaches us that the star formation rate in galaxies
likely starts out small and builds up gradually, only recently has it been
possible to see evidence for this observationally through the evolution of
the LF from z~6 to z~3. Establishing that this build up occurs from even
earlier times {z~7-8} has been difficult, however, due to the small size of
current high-redshift z~7-8 samples -- now numbering in the range of ~4-10
sources. Expanding the size of these samples is absolutely essential, if we
are to push current studies of galaxy buildup back to even earlier times.
Fortunately, we should soon be able to do so, thanks to ~50 arcmin**2 of
deep {26.9 AB mag at 5 sigma} NICMOS 1.6 micron data that will be available
over the two ACS GOODS fields as a result of one recent 180- orbit ACS
backup program and a smaller program. These data will nearly triple the deep
near-IR imaging currently available and represent a significant resource for
finding and characterizing the brightest high-redshift sources -- since
high-redshift candidates can be easily identified in these data from their
red z-H colours. Unfortunately, the red z-H colours of these candidates are
not sufficient to determine that these sources are at z=7, and it is
important also to have deep photometry at 1.1 microns. To obtain this
crucial information, we propose to follow up each of these z-H dropouts with
NICMOS at 1.1 microns to determine which are at high redshift and thus
significantly expand our sample of luminous, z=7 galaxies. Since
preliminary studies indicate that these candidates occur in only 30% of the
NIC3 fields, our follow-up strategy is ~3 times as efficient as without this
preselection and 9 times as efficient as a search in a field with no
pre-existing data. In total, we expect to identify ~8 luminous z-dropouts
and possibly ~2 z~10 J-dropouts as a result of this program, more than
tripling the number currently known. The increased sample sizes are
important if we are to solidify current conclusions about galaxy buildup and
the evolution of the LF from z~8. In addition to the high redshift science,
these deep 1.1 micron data would have significant value for many diverse
endeavors, including {1} improving our constraints on the stellar mass
density at z~7-10 and {2} doubling the number of galaxies at z~6 for which
we can estimate dust obscuration.

WFPC2 11130

AGNs with Intermediate-mass Black Holes: Testing the Black Hole-Bulge
Paradigm, Part II

The recent progress in the study of central black holes in galactic nuclei
has led to a general consensus that supermassive {10^6-10^9 solar mass}
black holes are closely connected with the formation and evolutionary
history of large galaxies, especially their bulge component. Two outstanding
issues, however, remain unresolved. Can central black holes form in the
absence of a bulge? And does the mass function of central black holes extend
below 10^6 solar masses? Intermediate-mass black holes {10^6 solar masses},
if they exist, may offer important clues to the nature of the seeds of
supermassive black holes. Using the SDSS, our group has successfully
uncovered a new population of AGNs with intermediate-mass black holes that
reside in low-luminosity galaxies. However, very little is known about the
detailed morphologies or structural parameters of the host galaxies
themselves, including the crucial question of whether they have bulges or
not. Surprisingly, the majority of the targets of our Cycle 14 pilot program
have structural properties similar to dwarf elliptical galaxies. The
statistics from this initial study, however, are really too sparse to reach
definitive conclusions on this important new class of black holes. We wish
to extend this study to a larger sample, by using the Snapshot mode to
obtain WFPC2 F814W images from a parent sample of 175 AGNs with
intermediate- mass black holes selected from our final SDSS search. We are
particularly keen to determine whether the hosts contain bulges, and if so,
how the fundamental plane properties of the host depend on the mass of their
central black holes. We will also investigate the environment of this unique
class of AGNs.

WFPC2 11128

Time Scales Of Bulge Formation In Nearby Galaxies

Traditionally, bulges are thought to fit well into galaxy formation models
of hierarchical merging. However, it is now becoming well established that
many bulges formed through internal, secular evolution of the disk rather
than through mergers. We call these objects pseudobulges. Much is still
unknown about pseudobulges, the most pressing questions being: How, exactly,
do they build up their mass? How long does it take? And, how many exist? We
are after an answer to these questions. If pseudobulges form and evolve over
longer periods than the time between mergers, then a significant population
of pseudobulges is hard to explain within current galaxy formation theories.
A pseudobulge indicates that a galaxy has most likely not undergone a major
merger since the formation of the disk. The ages of pseudobulges give us an
estimate for the time scale of this quiescent evolution. We propose to use
24 orbits of HST time to complete UBVIH imaging on a sample of 33 nearby
galaxies that we have observed with Spitzer in the mid-IR. These data will
be used to measure spatially resolved stellar population parameters {mean
stellar age, metallicity, and star formation history}; comparing ages to
star formation rates allows us to accurately constrain the time scale of
pseudobulge formation. Our sample of bulges includes both pseudo- and
classical bulges, and evenly samples barred and unbarred galaxies. Most of
our sample is imaged, 13 have complete UBVIH coverage; we merely ask to
complete missing observations so that we may construct a uniform sample for
studying bulge formation. We also wish to compare the stellar population
parameters to a variety of bulge and global galaxy properties including star
formation rates, dynamics, internal bulge morphology, structure from
bulge-disk decompositions, and gas content. Much of this data set is already
or is being assembled. This will allow us to derive methods of pseudobulge
identification that can be used to accurately count pseudobulges in large
surveys. Aside from our own science goals, we will present this broad set of
data to the community. Thus, we waive proprietary periods for all
observations.

NIC3 11120

A Paschen-Alpha Study of Massive Stars and the ISM in the Galactic Center

The Galactic center (GC) is a unique site for a detailed study of a
multitude of complex astrophysical phenomena, which may be common to nuclear
regions of many galaxies. Observable at resolutions unapproachable in other
galaxies, the GC provides an unparalleled opportunity to improve our
understanding of the interrelationships of massive stars, young stellar
clusters, warm and hot ionized gases, molecular clouds, large scale magnetic
fields, and black holes. We propose the first large-scale hydrogen Paschen
alpha line survey of the GC using NICMOS on the Hubble Space Telescope. This
survey will lead to a high resolution and high sensitivity map of the
Paschen alpha line emission in addition to a map of foreground extinction,
made by comparing Paschen alpha to radio emission. This survey of the inner
75 pc of the Galaxy will provide an unprecedented and complete search for
sites of massive star formation. In particular, we will be able to (1)
uncover the distribution of young massive stars in this region, (2) locate
the surfaces of adjacent molecular clouds, (3) determine important physical
parameters of the ionized gas, (4) identify compact and ultra-compact HII
regions throughout the GC. When combined with existing Chandra and Spitzer
surveys as well as a wealth of other multi-wavelength observations, the
results will allow us to address such questions as where and how massive
stars form, how stellar clusters are disrupted, how massive stars shape and
heat the surrounding medium, and how various phases of this medium are
interspersed.

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.

FLIGHT OPERATIONS SUMMARY:

Significant Spacecraft Anomalies: (The following are preliminary reports of
potential non-nominal performance that will be investigated.)

HSTARS:

11273 - GSacq(2,1,2) fails to RGA control

Upon acquisition of signal at 117/00:45:45 a 486 ESB message "A07" ("FGS
Coarse Track failed - Time out waiting for Data Valid") was observed.
GSACQ(2,1,2) at 116/23:47:46 appears to have failed, #44 commands did not
update from previous values before loss of signal. No FGS flags were seen.
Further information after engineering recorder dump.

REACQ(2,1,2) at 117/01:20:17 failed to gyro control with a 486 ESB message
"A0A" (FGS Fine Lock failed-Timed out waiting for fine lock).

11276 - NICMOS 744 TPG Reset

At 118/14:49:48 STB message NICMOS 736 and 744 was received. NICMOS 744 is
Timing Pattern Generator reset due to a single event upset. This was
accompanied by NICMOS 639, NICMOS 592, NICMOS 588,and NICMOS 290. During the
time we received the STB message we were in observe. We were not in an SAA.
The on call SE was contacted. The STB was dumped and NS-11 was executed to
clear NERRCNT.

11278 - GSacq(2,3,2) resulted in Fine Lock Backup

The GSacq(2,3,2) scheduled at 118/21:38:29 resulted in fine lock backup
(2,0,2). Stop flags QF3STOPF and QSTOP were received on FGS 3 at 21:41:49.
The Map at 21:45:50 showed errors of V1=-8.11, V2=-9.74, V3=2.92, and
RSS=13.01.

COMPLETED OPS REQUEST: (None)

COMPLETED OPS NOTES: (None)

SCHEDULED SUCCESSFUL

FGS GSacq 27 26
FGS REacq 12 11
OBAD with Maneuver 74 72

SIGNIFICANT EVENTS: (None)