HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 4266
PERIOD COVERED: UT December 22,23,24,25, 2006 (DOY 356,357,358,359)
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.
NIC3 11062
NICMOS non-linearity tests
This program incorporates a number of tests to analyse the count
rate
dependent non-linearity seen in NICMOS spectro-photometric
observations.
We will observe a field with stars of a range in luminosity in
NGC3603
with NICMOS in NIC1: F090M, F110W, F140W, F160W NIC2: F110W, F160W,
F187W, F205W, and F222M NIC3: F110W, F150W, F160W, F175W, and F222M.
We
will repeat the observations with flatfield lamp on, creating
artificially high count-rates, allowing tests of NICMOS linearity as
function of count rate. We first take exposures with the lamp off,
then
exposures with the lamp on, and repeat at the end with lamp off.
Finally, we continue with taking darks during occultation. We will
furthermore observe spectro-photometric standard P041C using the
G096,
G141, and G206 grisms in NIC3, and repeat the lamp off/on/off test
to
artificially create a high background.
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/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.
ACS/HRC 10991
Light Echoes from SN 2006X in M100
We propose a minimal investment of spacecraft time to discover and
confirm a light echo from Supernova 2006X in M100, the closest Type
Ia
in many years. Our spectroscopic and photometric data indicate that
this
SN sits behind a large amount of interstellar dust likely to produce
a
strong echo signal. This is one of very few cases where we will be
able
to study the three-dimensional environment of a SN Ia in full
detail,
and begin to understand how environmental effects play into the
evolutionary and observational factors which influence the utility of
SN
Ia as standard candles for probing cosmology. We propose an
efficient
program to definitively detect {or not} a light echo of reasonable
signal strength, to confirm that it is an echo by demonstrating
apparent
superluminal motion if it exists, to map the three-dimensional
geometry
of the reflecting interstellar structures, and to detail the
reflectance
properties of the dust which can be used to constrain ! its grain
size
and composition distribution.
ACS/WFC 10918
Reducing Systematic Errors on the Hubble Constant: Metallicity
Calibration of the Cepheid PL Relation
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 Cepheid PL relation over a
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.
ACS/HRC/WFC 10896
An Efficient ACS Coronagraphic Survey for Debris Disks around Nearby
Stars
We propose to finish our Cycle 11 optical survey for nearby debris
disks
using the ACS/HRC coronagraph. Out of 43 orbits originally proposed
for
the survey, 23 orbits were allocated, leading to a survey of 22
stars,
from which two new debris disks were imaged for the first time. Our
analysis of the initial survey gives an empirical estimate for the
detection rate of debris disks relative to heliocentric distance and
dust optical depth. Our target list for Cycle 15 is now optimized to
yield more frequent disk detections. Likewise our observing strategy
is
improved to maximize sensitivity per telescope orbit allocated.
Therefore we present the most efficient survey possible. The
scientific
motivation is to obtain scattered light images of previously
unresolved
debris disks to determine their viewing geometry and physical
architecture, both of which may characterize the underlying
planetary
system. We choose 25 debris disk targets for which we predict a
detection rate of 25% ? 5%. Four targets have extrasolar planets
from
which the viewing geometry revealed by a disk detection will resolve
the
v sin{i} ambiguity in the planet masses. These targets present the
remarkable opportunity of finally seeing a debris disk in system
with
known planets.
NIC3 10894
Probing the Birth of Super Star Clusters with NICMOS
The formation of ``super star clusters" represents an extreme mode
of
star formation in the local universe. Star clusters with radii < 5pc
and
masses exceeding 10^4 solar masses are now known to be common in
starbursts. These clusters are amazingly densely packed with massive
stars, and can have a violent impact on their host galaxies and the
surrounding IGM. The effects of massive star clusters perhaps were
even
more important in the earlier universe, when galaxy mergers and
starbursts were common, and the formation of massive globular
clusters
was ubiquitous. However, our knowledge of the formation and early
evolution of such massive clusters remains poorly understood, and
observations have only begun to probe these stages. The near-IR
fluxes
and colors of natal clusters change dramatically in their early
stages
of evolution, providing important diagnostics. We will use NICMOS to
explore the early evolution of massive star clusters through
observations of a sample of nearby starburst galaxies containing the
recently discovered ultra-young massive star clusters. First
identified
as compact optically- thick free-free radio sources, these natal
clusters are still embedded in their birth material and obscured at
optical wavelengths. Sensitive, high-resolution observations in the
near-IR are critical for investigating the properties of these
clusters
as they evolve from being completely obscured by their natal clouds
to
fully emerged and optically visible. NICMOS F160W, F205W, F187N, and
F190N {roughly H, K, and Pa-alpha} images will allow us to determine
their ages, extinctions, ionizing fluxes, embedded stellar masses,
and
the morphological relationship between radio, mid-IR, and optically
visible clusters. These results will ultimately provide insight into
the
earliest stages of super star cluster evolution and the properties
of
massive star formation throughout the universe.
ACS/WFC/WFPC2 10890
Morphologies of the Most Extreme High-Redshift Mid-IR-Luminous Galaxies
The formative phase 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,
restricting us to the study of 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 bright at mid-IR wavelengths
{F[24um]>0.8mJy}, but deep ground based imaging suggests extremely
faint
{and in some cases extended} optical counterparts {R~24-27}. Deep
K-band
images show barely resolved galaxies. Mid-infrared spectroscopy with
Spitzer/IRS reveals that they have redshifts z ~ 2-2.5, suggesting
bolometric luminosities ~10^{13-14}Lsun! We propose to obtain deep
ACS
F814W and NIC2 F160W images of these sources and their environs in
order
to determine kpc-scale morphologies and surface photometry for these
galaxies. The proposed observations will help us determine whether
these
extreme objects are merging systems, massive obscured starbursts
{with
obscuration on kpc scales!} or very reddened {locally obscured} AGN
hosted by intrinsically low-luminosity galaxies.
ACS/WFC 10886
The Sloan Lens ACS Survey: Towards 100 New Strong Lenses
As a continuation of the highly successful Sloan Lens ACS {SLACS}
Survey
for new strong gravitational lenses, we propose one orbit of ACS-WFC
F814W imaging for each of 50 high- probability strong galaxy-galaxy
lens
candidates. These observations will confirm new lens systems and
permit
immediate and accurate photometry, shape measurement, and mass
modeling
of the lens galaxies. The lenses delivered by the SLACS Survey all
show
extended source structure, furnishing more constraints on the
projected
lens potential than lensed-quasar image positions. In addition,
SLACS
lenses have lens galaxies that are much brighter than their lensed
sources, facilitating detailed photometric and dynamical observation
of
the former. When confirmed lenses from this proposal are combined
with
lenses discovered by SLACS in Cycles 13 and 14, we expect the final
SLACS lens sample to number 80--100: an approximate doubling of the
number of known galaxy-scale strong gravitational lenses and an
order-of-magnitude increase in the number of optical Einstein rings.
By
virtue of its homogeneous selection and sheer size, the SLACS sample
will allow an unprecedented exploration of the mass structure of the
early-type galaxy population as a function of all other observable
quantities. This new sample will be a valuable resource to the
astronomical community by enabling qualitatively new strong lensing
science, and as such we will waive all but a short {3-month}
proprietary
period on the observations.
ACS/WFC 10882
Emission Line Snapshots of 3CR Radio Galaxies
Radio galaxies are an important class of extragalactic objects: they
are
one of the most energetic astrophysical phenomena and they provide
an
exceptional probe of the evolving Universe, lying typically in high
density regions but well-represented across a wide redshift range.
In
earlier Cycles we carried out extensive HST observations of the 3CR
sources in order to acquire a complete and quantitative inventory of
the
structure, contents and evolution of these important objects. We
discovered new optical jets, dust lanes, and revealed point-like
nuclei
whose properties support AGN unified schemes. Here, we propose to
obtain
ACS emission line images at low and high excitation of 3CR sources
with
z<0.3, both low- and classical high- power radio galaxies, as a
major
enhancement to an already superb dataset. We aim to probe
fundamental
relationships between warm optical line-emitting gas, radio source
structure {jets and lobes} and X-ray coronal halos. We will combine
our
existing UV images with new emission- line images to establish
quantitative star formation characteristics and their relation to
dust
and merging, and with emission-line excitation maps, test theories
on
ionization beam patterns and luminosities from active nuclei. We
will
seek jet induced star formation and knowing optical emission-line
physics, investigate quantitative jet physics. The nuclear emission
line
properties of the galaxies will themselves be established and used
as
ingredients in continuing tests of unified AGN theories. The
resulting
database will be an incredibly valuable resource to the astronomical
community for years to come.
ACS/WFC 10875
A Snapshot Survey of The Most Massive Clusters of Galaxies
We propose the continuation of our highly successful Cycle14
snapshot
survey of a sample of 123 very X-ray luminous clusters in the
redshift
range 0.3-0.7. As demonstrated by the 21 snapshots obtained so far
in
Cycle14 these systems frequently exhibit strong gravitational lensing
as
well as spectacular examples of violent galaxy evolution. 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. Acknowledging the broad
community interest in this sample we waive our data rights for these
observations.
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.
ACS/WFC 10835
Probing The Globular Cluster / Low Mass X-ray Binary Connection in
Early-type Galaxies At Low X-ray
Combined high-resolution imaging from Hubble and Chandra {CXO} has
revolutionized our understanding of extragalactic low-mass X-ray
binaries {LMXBs} and globular clusters {GCs}, yet their connection
in
early-type galaxies has remained unstudied at the luminosities of
the
Galactic LMXBs in GCs. NGC 4278 and 3379 will be the first two
prototypical elliptical galaxies with deep CXO observations enabling
the
study of LMXBs at lower luminosities. We propose mosaic ACS
observations
of both galaxies {5 fields per galaxy} that will provide the most
comprehensive view into the connection between GCs and LMXBs in
early-type galaxies. We will detect ~860 and ~270 GCs in all of NGC
4278
and NGC 3379, respectively. These two galaxies will have among the
greatest number of detected GC-LMXBs to date {~130 & 50} and
will
include the faintest GC-LMXBs in a normal early-type galaxy. We will
measure the fraction of GCs which contain LMXBs, as a function of
X-ray
luminosity, galactocentric distance, color, and GC half-light
radius.
Using the radial profiles of optical light, GCs, and LMXBs, we will
determine the percentage of field LMXBs which may have originated in
GCs. We will use the measured GC properties over the entire extent
of
both galaxies to constrain theories of GC formation and evolution.
ACS/WFC 10809
The nature of "dry" mergers in the nearby Universe
Recent studies have shown that "dry" mergers of red,
bulge-dominated
galaxies at low redshift play an important role in shaping today's
most
massive ellipticals. These mergers have been identified in extremely
deep ground-based images of red sequence galaxies at z ~ 0.1. The
ground-based images reach surface brightness limits of AB ~ 29, but
lack
the resolution to study the morphologies of the galaxies inside the
effective radius. Here we propose to obtain ACS images of a
representative sample of 40 of these red sequence galaxies: 15
ongoing
dry mergers, 15 remnants, and 10 undisturbed objects. We will
measure
the isophote shapes and ellipticities of the galaxies, their dust
content, morphological fine structure {shells and ripples}, AGN
content,
and their location on the Fundamental Plane. By comparing galaxies
in
different stages of the merging process we can constrain the amount
of
gas associated with these red mergers, the effect of active nuclei,
and
track structural changes. As two galaxies can be observed in a
single
orbit 20 orbits are requested to observe the 40 galaxies.
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 Type Ia supernovae
at
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 Type Ia supernovae with NICMOS, reducing the
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 Type Ia supernovae at z > 1. Together, these
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 10787
Modes of Star Formation and Nuclear Activity in an Early Universe
Laboratory
Nearby compact galaxy groups are uniquely suited to exploring the
mechanisms of star formation amid repeated and ongoing gravitational
encounters, conditions similar to those of the high redshift
universe.
These dense groups host a variety of modes of star formation, and
they
enable fresh insights into the role of gas in galaxy evolution. With
Spitzer mid-IR observations in hand, we have begun to obtain high
quality, multi-wavelength data for a well-defined sample of 12
nearby
{<4500km/s} compact groups covering the full range of
evolutionary
stages. Here we propose to obtain sensitive BVI images with the
ACS/WFC,
deep enough to reach the turnover of the globular cluster luminosity
function, and WFPC2 U-band and ACS H-alpha images of Spitzer-
identified
regions hosting the most recent star formation. In total, we expect
to
detect over 1000 young star clusters forming inside and outside
galaxies, more than 4000 old globular clusters in >40 giant
galaxies
{including 16 early-type galaxies}, over 20 tidal features,
approximately 15 AGNs, and intragroup gas in most of the 12 groups.
Combining the proposed ACS images with Chandra observations, UV
GALEX
observations, ground-based H-alpha imaging, and HI data, we will
conduct
a detailed study of stellar nurseries, dust, gas kinematics, and AGN.
WFPC2 10748
WFPC2 CYCLE 14 Standard Darks
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/HRC 10556
Neutral Gas at Redshift z=0.5
Damped Lyman-alpha systems {DLAs} are used to track the bulk of the
neutral hydrogen gas in the Universe. Prior to HST UV spectroscopy,
they
could only be studied from the ground at redshifts z>1.65. However,
HST
has now permitted us to discover 41 DLAs at z<1.65 in our
previous
surveys. Followup studies of these systems are providing a wealth of
information about the evolution of the neutral gas phase component
of
the Universe. But one problem is that these 41 low-redshift systems
are
spread over a wide range of redshifts spanning nearly 70% of the age
of
the Universe. Consequently, past surveys for low-redshift DLAs have
not
been able to offer very good precision in any small redshift regime.
Here we propose an ACS-HRC- PR200L spectroscopic survey in the
redshift
interval z=[0.37, 0.7] which we estimate will permit us to discover
another 41 DLAs. This will not only allow us to double the number of
low-redshift DLAs, but it will also provide a relatively
high-precision
regime in the low-redshift Universe that can be used to anchor
evolutionary studies. Fortunately DLAs have high absorption
equivalent
width, so ACS-HRC-PR200L has high-enough resoultion to perform this
proposed MgII-selected DLA survey.
ACS/HRC 10508
Orbits, Masses, and Densities of Three Transneptunian Binaries
The subset of transneptunian objects {TNOs} having natural
satellites
offers unique opportunities for physical studies of these distant
relics
from the outer parts of the protoplanetary nebula. HST/ACS is
ideally
suited to determining orbits of TNO satellites, resulting in the
system
masses. In conjunction with thermal emission observations by
Spitzer,
which provides sizes, we can determine the densities of TNOs.
Densities
offer a powerful window into their bulk compositions and interior
structures.
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary
reports
of potential non-nominal performance that will be investigated.)
HSTARS:
10569 GSacq(2,3,2) failed to RGA control @ 356/1309z
GSacq(2,3,2) scheduled at 356/15:05:46 failed at 13:09:36 due to
scan
step limit
exceeded on FGS 2. OBAD1 showed errors of V1=-730.81,
V2=4478.69, V3=489.56 and RSS =4564.26. OBAD2 showed errors of
V1=-1.20,
V2=7.22,
V3=-4.65 and RSS= 8.68.
10570 REacq(2,1,1) failed to RGA control @ 356/1758z
REacq(2,1,1) scheduled at 356/17:54:55 failed at 117:58:02 due to
scan
step limit
exceeded on FGS 2. OBAD2 showed errors of V1=-0.89, V2=0.33,
V3=0.02
and RSS =0.95.
10571 GSAcq(1,3,1) failed to RGA Hold (Gyro Control) @ 356/2235z
The
GSAcq(1,3,1)scheduled at 356/22:31:28 - 22:39:33 failed to RGA Hold
due to
(QF3SRLEX) Search Radius Limit Exceeded on FGS-3. Pre-acquisition
OBADs
showed (RSS) attitude correction values of 1837.82 and 6.39
arcseconds. Post-acquisition OBAD/MAP had 3-axis (RSS) error value
of
5.61
arcseconds.
10572 REAcq (2,1,1) failed to RGA control @ 356/1946z
REAcq
(2,1,1) scheduled from 356/19:30:54-19:38:05 failed to RGA control
due to
Search Radius Limit Exceeded on FGS 2. Mnemonic QF2SRLEX was
observed.
OBAD #1 RSS: 823.77; OBAD #2 RSS: 5.22; OBAD MAP: Not
scheduled.
REAcq (2,1,1) scheduled from 356/21:06:53-21:14:04 failed to
RGA
control due to Search Radius Limit Exceeded on FGS 2. Mnemonic
QF2SRLEX
was observed. OBAD data unavailable due to LOS.
10573 GSacq (1,2,2) failed due to stop flag on FGS1 (RGA Hold)
@357/1557z
Upon
acquisition at 16:18:17 stop flags were set for FGS1.
Preacquisition OBADs RSS were 564.65 and 6.64 arcseonds. Post
acquisition Map RSS = 3.89 arc seconds.
10574 GSAcq (1,3,1) failed due to Search Radius Limit Exceeded on FGS 1 @
358/0652z
At AOS
358/06:52:01 GSAcq (1,3,1) scheduled from 358/05:27:13-05:34:16
had failed
due to Search Radius Limit Exceeded on FGS 1. OBAD #1:
unavailable due to LOS. OBAD #2: V1 -6.52, V2 28.27, V3 22.03, RSS
36.44.
OBAD Map: Not scheduled
10575 GSAcq (2,1,2) failed to RGA control @ 358/1022z
At AOS
358/10:22:17, GSAcq (2,1,2) had failed to RGA control. No 486
ESB's
noted. Due to LOS, OBAD data will not be available till the next
scheduled
engineering data dump. OBAD Map: V1 -0.57, V2 -1074.41, V3
1.44, RSS
1074.41.
10576 CSTRUCCP Limit Violation @ 359/1405z
At
359/14:05:10 and 359/14:07:27 mnemonic Structure Current Primary
(CSTRUCCP)
went out of limit with a value of 5.6 amps, one sample during
each
occurrence. The yellow high limit is 5.4 amps. The on-call SE was
notified.
COMPLETED OPS REQUEST: (None)
COMPLETED OPS NOTES: (None)
SCHEDULED SUCCESSFUL
FGS
GSacq
35
30
FGS
REacq
18
17
OBAD with Maneuver
96
96
SIGNIFICANT EVENTS: (None)
-Lynn
Lynn F. Bassford
CHAMP HST Missions Operations Manager
Lockheed Martin Mission Services (LMMS)
GSFC PH#: 301-286-2876
"The Hubble Space Telescope is the astronomical observatory and
key to unlocking the most cosmic mysteries of the past, present and
future." - 7/26/6