Notice: Due to the conversion of some ACS WFC or HRC
observations into
WFPC2, or NICMOS observations after
the loss of ACS CCD science
capability in January, there may be an
occasional discrepancy between a
proposal's listed (and correct) instrument
usage and the abstract that
follows it.
HUBBLE SPACE TELESCOPE - Continuing to collect World Class
Science
DAILY REPORT # 4448
PERIOD COVERED: UT September 14, 15 & 16, 2007 (DOY
257, 258 & 259)
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 DARKs. 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 11225
The Wavelength Dependence of Accretion Disk Structure
We can now routinely measure the size of quasar accretion
disks using
gravitational microlensing
of lensed quasars. The next step to testing
accretion disk models is to measure the
size of accretion disks as a
function of wavelength, particularly at
the UV and X-ray wavelengths
that should probe the inner, strong
gravity regime. Here we focus on two
four-image quasar lenses that already have
optical {R band} and X-ray
size measurements using microlensing. We will combine the HST
observations with ground-based monitoring to
measure the disk size as a
function of wavelength from the near-IR
to the UV. We require HST to
measure the image flux ratios in the
ultraviolet continuum near the
Lyman limit of the quasars. The selected targets have
estimated black
hole masses that differ by an order
of magnitude, and we should find
wavelength scalings
for the two systems that are very different because
the Blue/UV wavelengths should
correspond to parts of the disk near the
inner edge for the high mass system
but not in the low mass system. The
results will be modeled using a
combination of simple thin disk models
and complete relativistic disk
models. While requiring only 18 orbits,
success for one system requires
observations in both Cycles 16 and 17.
WFPC2 11217
The Light Echoes around V838 Monocerotis
V838 Monocerotis, which burst
upon the astronomical scene in early 2002,
is a completely unanticipated new
object. It underwent a large-amplitude
and very luminous outburst, during
which its spectrum remained that of
an extremely cool supergiant. A rapidly evolving set of light echoes
around V838 Mon was discovered soon
after the outburst, and quickly
became the most spectacular display of
the phenomenon ever seen. These
light echoes provide the means to
accomplish three unique types of
measurements based on continued HST imaging
during the event: {1} Study
effects of MHD turbulence at high
resolution and in 3 dimensions; {2}
Construct the first unambiguous and fully 3-D map of a circumstellar
dust envelope in the Milky Way; {3}
Study dust physics in a unique
setting where the spectrum and light
curve of the illumination, and the
scattering angle, are unambiguously known.
We have also used our HST
data to determine the distance to
V838 Mon through direct geometric
techniques. Because of the extreme rarity
of light echoes, this is
almost certainly the only opportunity
to achieve such results during the
lifetime of HST. We propose two visits
during Cycle 16, in order to
continue the mapping of the circumstellar dust and to accomplish the
other goals listed above.
WFPC2 11203
A Search for Circumstellar Disks
and Planetary-Mass Companions around
Brown Dwarfs in Taurus
During a 1-orbit program in Cycle 14, we used WFPC2 to obtain
the first
direct image of a circumstellar
disk around a brown dwarf. These data
have provided fundamental new
constraints on the formation process of
brown dwarfs and the properties of
their disks. To search for additional
direct detections of disks around
brown dwarfs and to search for
planetary-mass companions to these objects, we
propose a WFPC2 survey of
32 brown dwarfs in the Taurus star-forming region.
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!
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 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.
NIC2 11101
The Relevance of Mergers for Fueling AGNs:
Answers from QSO Host
Galaxies
The majority of QSOs are known
to reside in centers of galaxies that
look like ellipticals.
Numerical simulations have shown that remnants of
galaxy mergers often closely resemble
elliptical galaxies. However, it
is still strongly debated whether
the majority of QSO host galaxies are
indeed the result of relatively recent
mergers or whether they are
completely analogous to inactive ellipticals to which nothing
interesting has happened recently. To
address this question, we recently
obtained deep HST ACS images for five
QSO host galaxies that were
classified morphologically as ellipticals {GO-10421}. This pilot study
revealed striking signs of tidal
interactions such as ripples, tidal
tails, and warped disks that were not
detected in previous studies. Our
observations show that at least some
"elliptical" QSO host galaxies are
the products of relatively recent
merger events rather than old galaxies
formed at high redshift.
However, the question remains whether the host
galaxies of classical QSOs are truly distinct from inactive ellipticals
and whether there is a connection
between the merger events we detect
and the current nuclear activity.
We must therefore place our results
into a larger statistical context.
We are currently conducting an HST
archival study of inactive elliptical
galaxies {AR-10941} to form a
control sample. We now propose to
obtain deep HST/WFPC2 images of 13
QSOs whose host
galaxies are classified as normal ellipticals. Comparing
the results for both samples will
help us determine whether classical
QSOs reside in normal elliptical
galaxies or not. Our recent pilot study
of five QSOs
indicates that we can expect exciting results and deep
insights into the host galaxy morphology
also for this larger sample of
QSOs. A statistically meaningful sample
will help us determine the true
fraction of QSO hosts that suffered
strong tidal interactions and thus,
whether a merger is indeed a
requirement to trigger nuclear activity in
the most luminous AGNs. In addition to our primary science observations
with WFPC2, we will obtain NICMOS3
parallel observations with the
overall goal to select and characterize
galaxy populations at high
redshifts. The imaging will be among the
deepest NICMOS images: These
NICMOS images are expected to go to a limit a little over
1 magnitude
brighter than HUDF-NICMOS data, but over
13 widely separated fields,
with a total area about 1.5 times
larger than HUDF-NICMOS. This
separation means that the survey will tend
to average out effects of
cosmic variance. The NICMOS3 images will
have sufficient resolution for
an initial characterization of
galaxy morphologies, which is currently
one of the most active and
promising areas in approaching the problem of
the formation of the first massive
galaxies. The depth and area coverage
of our proposed NICMOS
observations will also allow a careful study of
the mass function of galaxies at
these redshifts. This provides a large
and unbiased sample, selected in
terms of stellar mass and unaffected by
cosmic variance, to study the on-going
star formation activity as a
function of mass {i.e. integrated star
formation} at this very important
epoch.
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 11079
Treasury Imaging of Star Forming Regions in the Local
Group:
Complementing the GALEX and NOAO Surveys
We propose to use WFPC2 to image the most interesting
star-forming
regions in the Local Group galaxies, to
resolve their young stellar
populations. We will use a set of filters
including F170W, which is
critical to detect and characterize the
most massive stars, to whose hot
temperatures colors at longer wavelengths
are not sensitive. WFPC2's
field of view ideally matches the
typical size of the star-forming
regions, and its spatial resolution
allows us to measure individual
stars, given the proximity of these
galaxies. The resulting H-R diagrams
will enable studies of
star-formation properties in these regions, which
cover largely differing metallicities {a factor of 17, compared to the
factor of 4 explored so far} and
characteristics. The results will
further our understanding of the
star-formation process, of the
interplay between massive stars and
environment, the properties of dust,
and will provide the key to
interpret integrated measurements of
star-formation indicators {UV, IR, Halpha} available for several
hundreds more distant galaxies. Our
recent deep surveys of these
galaxies with GALEX {FUV, NUV} and
ground-based imaging {UBVRI, Halpha,
[OIII] and [SII]} provided the identification of the most
relevant SF
sites. In addition to our scientific
analysis, we will provide catalogs
of HST photometry in 6 bands,
matched corollary ground-based data, and
UV, Halpha and IR integrated
measurements of the associations, for
comparison of integrated star-formation
indices to the resolved
populations. We envisage an EPO component.
NIC1/NIC2/NIC3 11060
NICMOS Photometric Stability Monitoring
This NICMOS calibration proposal carries out photometric monitoring
observations during Cycle 15. The format is
the same as the Cycle 14
version of the program {10725}, but a
few modifications were made with
respect to the Cycle 12 program 9995
and Cycle 13 program 10381.
Provisions had to be made to adopt
to 2-gyro mode {G191B2B was added as
extra target to provide target
visibility through most of the year}.
Where before 4 or 7 dithers were made in a filter before
we moved to the
next filter, now we observe all
filters at one position before moving to
the next dither position. While the
previous method was chosen to
minimize the effect of persistence, we
now realize that persistence may
be connected to charge trapping
and by moving through the filter such
that the count rate increases, we
reach equilibrium more quickly between
charge being trapped and released. We
have also increased exposure times
where possible to reduce the charge
trapping non- linearity effects.
WFPC2 11038
Narrow Band and Ramp Filter Closeout
These observations are to improve calibration of narrow
band and ramp
filters. We also test for changes in
the filter properties during
WFPC2's 14 years on-board HST.
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.
NIC3 10921
Tangential Velocities of Objects in the Orion Nebula and
Locating the
Embedded Outflow Sources.
The Orion Nebula is arguably the Rosetta Stone for studying a very young
star cluster and how the radiation
and outflowing plasma from its stars
interact with ambient material. It has
been the subject of numerous HST
imaging studies, which means that there
is good opportunity for
determining tangential velocities by
obtaining second epoch images
during Cycle 15, which may be the last
cycle for which the WFPC2 is
available. These velocities in the
plane-of-the-sky will allow us to
determine the patterns of outflow from
micro-jets smaller than the Solar
System to jet driven shocks more than a parsec from their
sources.
Combined with radial velocities, we'll obtain spatial
velocities, which
are critical to determining where
the embedded sources are located that
produce the numerous HH objects coming
from the Orion-S and BN-KL
regions. We'll also be able to
determine the physics that is operating
in the LL Ori
type of outflows {where a bipolar jet is being distorted
by a slow wind coming from the
nebula}. We will also be able to search
for runaway stars caused by the
disintegration of young multiple-star
systems. All of this is possible
because the long-time base of the WFPC2
and ACS observations allow a new
level of astrometric precision to be
obtained and to be done efficiently by
making coordinated parallel
observations with all images.
NIC1 10889
The Nature of the Halos and Thick Disks of Spiral Galaxies
We propose to resolve the extra-planar stellar populations
of the thick
disks and halos of seven nearby,
massive, edge-on galaxies using ACS,
NICMOS, and WFPC2 in parallel. These
observations will provide accurate
star counts and color-magnitude
diagrams 1.5 magnitudes below the tip of
the Red Giant Branch sampled along
the two principal axes and one
intermediate axis of each galaxy. We will
measure the metallicity
distribution functions and stellar density
profiles from star counts
down to very low average surface brightnesses, equivalent to ~32 V-mag
per square arcsec.
These observations will provide the definitive HST
study of extra-planar stellar
populations of spiral galaxies. Our
targets cover a range in galaxy mass,
luminosity, and morphology and as
function of these galaxy properties we
will provide: - The first
systematic study of the radial and isophotal shapes of the diffuse
stellar halos of spiral galaxies - The
most detailed comparative study
to date of thick disk morphologies
and stellar populations - A
comprehensive analysis of halo and thick disk
metallicity distributions
as a function of galaxy type and
position within the galaxy. - A
sensitive search for tidal streams - The
first opportunity to directly
relate globular cluster systems to
their field stellar population We
will use these fossil records of the
galaxy assembly process preserved
in the old stellar populations to
test halo and thick disk formation
models within the hierarchical galaxy
formation scheme. We will test
LambdaCDM predictions on sub-galactic
scales, where it is difficult to
test using CMB and galaxy redshift surveys, and where it faces its most
serious difficulties.
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.
ACS/SBC 10864
Mapping the Gaseous Content of Protoplanetary
and Young Planetary
Systems with ACS
One of the key problems in planetary system formation is understanding
how rapidly, and over what time
interval Jovian planets can form. Dust
in the protoplanetary
disk is critical in planetesimal formation, but it
is the gas which produces giant
planets, and which is essential for
their migration. However, compared to
data on the circumstellar dust,
information on the gas component is sparse,
especially in the
planet-formation zone. This severely limits our
ability to put
observational constraints on giant planet
formation, except to note that
the process must be largely
complete by 12 Myr, given the paucity of
Herbig Ae or
classical T Tauri stars older than 10-12 Myr. In the FUV,
photo-excited molecular hydrogen transitions
have the requisite contrast
to the stellar photosphere,
accretion shock, and reflection nebulosity,
and can be traced 50-100 AU from
the exciting stars in both envelopes
and outflow cavities and protoplanetary disks. Central disk cavities, an
expected consequence of planet
formation, larger than 0.1" are directly
detectable in HST FUV spectra, while
smaller cavities may be detected by
comparison with protoplanetary
disks which are still accreting onto
their stars. We propose augmenting
existing HST coronagraphic imagery of
6 Herbig Fe and T Tauri disks with ACS Solar-Blind Channel Lyman alpha
imagery and slitless
spectroscopy simultaneously sampling the disk in
molecular hydrogen and small-grain
reflection nebulosity. These data
will be used to quantify the amount
of vertical stratification in these
disks, to map the mass-loss geometry
from the star, and to determine
whether removal of molecular material
precedes, lags, or is contemporary
with clearing of the dust.
NIC2 10527
Imaging Scattered Light from Debris Disks Discovered by
the Spitzer
Space Telescope Around 20
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 emission with the
Spitzer Space Telescope as part of
the Spitzer Legacy Science program
titled, "The Formation and Evolution
of Planetary Systems {FEPS}."
Modelling of the thermal excess emission
in the form of spectral energy
distributions alone cannot distinguish
between narrowly confined high opacity
disks and broadly distributed,
low opacity disks. However, our
proposed NICMOS observations can, by
imaging the light scattered from this
material. Even non- detections
will place severe constraints on the
disk geometry, ruling out models
with high optical depth. Unlike
previous disk imaging programs, our
program contains a well defined sample
of solar mass stars covering a
range of ages from ~10Myrs to a few Gyrs, allowing us to study the
evolution of disks from primordial to
debris for the first time. These
results will greatly improve our
understanding of debris disks around
Sun-like stars at stellar ages nearly 10x
older than any previous
investigation. Thus we will have fit a
crucial piece into the puzzle
concerning the formation and evolution of
our own solar system.
NIC2 10487
A Search for Debris Disks in the Coeval Beta Pictoris Moving Group
Resolved observations of debris disks present us with the
opportunity of
studying planetary evolution in other
solar systems. We propose to
search for debris disks in the Beta Pictoris moving group {8-20 Myrs,
10-50 pc away} , which provides a
coeval sample of multiple spectral
types, and it has already produced
two magnificent resolved debris
disks: AU Mic
and Beta Pic. Such coeval sample will provide us with
a
snapshop of the crucial time in disk
evolution in which the disk makes
the transition from optically thick
to optically thin, and it will be
useful to study the stellar mass
dependence of the disk evolution.
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are
preliminary reports
of potential non-nominal
performance that will be investigated.
HSTARS:
10993 - REACQ(1,2,2) failed, scan
step limit exceeded on FGS 1
REACQ(1,2,2) at 257/20:50:56 failed due to scan step limit
exceeded on
FGS 1 at 22:55:06. Initial GSACQ(1,2,2)
at 21:17:23 was successful.
10994 - GSAcq(2,1,1) failed to RGA Hold (Gyro Control)
Upon acquisition of signal (AOS) at 260/01:50:01, the GSAcq(2,1,1)
scheduled at 260/01:39:25 - 01:47:29 had failed to RGA Hold
due to a
Search Radius Limit Exceeded Error on FGS-2.
Pre-acquisition OBADs attitude correction values not
available due to
LOS. Post-acq OBAD/MAP has (RSS)
value of 66.26 arcseconds.
Subsequent REacq(2,1,1) at 260/04:50:04 failed to RGA Hold due to a
Search Radius Limit Exceeded Error on FGS-2. REacqs
at 260/0314:51,
260/06:28:38 were successful.
COMPLETED OPS REQUEST: (None)
COMPLETED OPS NOTES: (None)
SCHEDULED
SUCCESSFUL
FGS GSacq
18
17
FGS REacq
24
22
OBAD with Maneuver
82
82
SIGNIFICANT EVENTS:
Flash Report: NICMOS Defocus Test
The 1st observation for the NICMOS on-orbit PAM defocus
test was
successfully completed Thursday. STScI has performed a quick-look
analysis of the science data and they
are happy with the initial
results. A second flash report will be sent out after
the second set of
observations.
-
____________________________________________________________
Lynn F. Bassford
Hubble Space Telescope
CHAMP
CHAMP Flight Operations Team Manager
Lockheed Martin
NASA 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