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- Daily Report #5198 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/b330c02b49b4138a?hl=en
- HST Status Oct 08, 2010 - 2 messages, 1 author http://groups google com/group/sci astro hubble/t/147a66aa6e045954?hl=en
============================================================================== TOPIC: Daily Report #5198
http://groups google com/group/sci astro hubble/t/b330c02b49b4138a?hl=en
== 1 of 1 == Date: Fri, Oct 8 2010 9:47 am From: "Cooper, Joe"
HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science
DAILY REPORT #5198
PERIOD COVERED: 8pm October 6 - 7:59pm October 7, 2010 (DOY 280/00:00z-280/23:59z)
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated )
HSTARS: (None)
COMPLETED OPS REQUEST: (None)
COMPLETED OPS NOTES: (None)
Scheduled Successful
FGS GSAcq 11 11 FGS REAcq 07 07 OBAD with Maneuver 08 08
SIGNIFICANT EVENTS: (None)
OBSERVATIONS SCHEDULED:
ACS/WFC 12209
A Strong Lensing Measurement of the Evolution of Mass Structure in Giant Elliptical Galaxies
The structure and evolution of giant elliptical galaxies provide key quantitative tests for the theory of hierarchical galaxy formation in a cold dark matter dominated universe Strong gravitational lensing provides the only direct means for the measurement of individual elliptical galaxy masses beyond the local universe, but there are currently no large and homogeneous samples of strong lens galaxies at significant cosmological look-back time Hence, an accurate and unambiguous measurement of the evolution of the mass-density structure of elliptical galaxies has until now been impossible Using spectroscopic data from the recently initiated Baryon Oscillation Spectroscopic Survey (BOSS) of luminous elliptical galaxies at redshifts from approximately 0 4 to 0 7, we have identified a large sample of high-probability strong gravitational lens candidates at significant cosmological look-back time, based on the detection of emission-line features from more distant galaxies along the same lines of sight as the target ellipticals We propose to observe 45 of these systems with the ACS-WFC in order to confirm the incidence of lensing and to measure the masses of the lens galaxies We will complement these lensing mass measurements with stellar velocity dispersions from ground-based follow-up spectroscopy In combination with similar data from the Sloan Lens ACS (SLACS) Survey at lower redshifts, we will directly measure the cosmic evolution of the ratio between lensing mass and dynamical mass, to reveal the structural explanation for the observed size evolution of elliptical galaxies (at high mass) We will also measure the evolution of the logarithmic mass-density profile of massive ellipticals, which is sensitive to the details of the merging histories through which they are assembled Finally, we will use our lensing mass-to-light measurements to translate the BOSS galaxy luminosity function into a mass function, and determine its evolution in combination with data from the original Sloan Digital Sky Survey
ACS/WFC 12210
SLACS for the Masses: Extending Strong Lensing to Lower Masses and Smaller Radii
Strong gravitational lensing provides the most accurate possible measurement of mass in the central regions of early-type galaxies (ETGs) We propose to continue the highly productive Sloan Lens ACS (SLACS) Survey for strong gravitational lens galaxies by observing a substantial fraction of 135 new ETG gravitational-lens candidates with HST-ACS WFC F814W Snapshot imaging The proposed target sample has been selected from the seventh and final data release of the Sloan Digital Sky Survey, and is designed to complement the distribution of previously confirmed SLACS lenses in lens-galaxy mass and in the ratio of Einstein radius to optical half-light radius The observations we propose will lead to a combined SLACS sample covering nearly two decades in mass, with dense mapping of enclosed mass as a function of radius out to the half-light radius and beyond With this longer mass baseline, we will extend our lensing and dynamical analysis of the mass structure and scaling relations of ETGs to galaxies of significantly lower mass, and directly test for a transition in structural and dark-matter content trends at intermediate galaxy mass The broader mass coverage will also enable us to make a direct connection to the structure of well-studied nearby ETGs as deduced from dynamical modeling of their line-of-sight velocity distribution fields Finally, the combined sample will allow a more conclusive test of the current SLACS result that the intrinsic scatter in ETG mass-density structure is not significantly correlated with any other galaxy observables The final SLACS sample at the conclusion of this program will comprise approximately 130 lenses with known foreground and background redshifts, and is likely to be the largest confirmed sample of strong-lens galaxies for many years to come
COS/NUV/FUV 12178
Spanning the Reionization History of IGM Helium: a Highly Efficient Spectral Survey of the Far-UV-Brightest Quasars
The reionization of IGM helium likely occurred at redshifts of z=3 to
4
Detailed studies of HeII Ly-alpha absorption toward a handful of
quasars at 2
7 COS/NUV/FUV 12299 Spectroscopic Signatures of Binary and Recoiling Black Holes We propose to obtain UV the spectra of the Ly-alpha and Mg II lines of
13 SDSS quasars whose H-beta lines are offset by 1000-4000 km/s from
their systemic redshifts
Such lines have been suggested to originate
in recoiling or close binary black holes
However these
interpretations are not unique and UV spectroscopy, possible only with
the HST, can discriminate between competing possibilities
Identifying
such systems is extremely important in the context of scenarios for
galaxy formation and evolution and in view of recent predictions from
numerical relativity
Close binary black holes represent an apparently
inevitable stage in the merger of two massive galaxies
The subsequent
merger of the members of the binary is expected to produce a recoiling
black hole in some fraction of cases
Thus, the census of such
systems, their environments, and hosts can constrain some of the more
uncertain parameters in evolutionary models
But before we can find
them in any numbers, we need to evaluate the candidates known so far
This is the goal of our proposal
COS/NUV/FUV/WFC3/UV 12248 How Dwarf Galaxies Got That Way: Mapping Multiphase Gaseous Halos and
Galactic Winds Below L* One of the most vexing problems in galaxy formation concerns how gas
accretion and feedback influence the evolution of galaxies
In high
mass galaxies, numerical simulations predict the initial fuel is
accreted through 'cold' streams, after which AGN suppress star
formation to leave galaxies red and gas-poor
In the shallow potential
wells that host dwarf galaxies, gas accretion can be very efficient,
and "superwinds" driven either by hot gas expelled by SNe or momentum
imparted by SNe and hot-star radiation are regarded as the likely
source(s) of feedback
However, major doubts persist about the physics
of gas accretion, and particularly about SN-driven feedback, including
their scalings with halo mass and their influence on the evolution of
the galaxies
While "superwinds" are visible in X-rays near the point
of their departure, they generally drop below detectable
surface-brightness limits at ~ 10 kpc
Cold clumps in winds can be
detected as blue-shifted absorption against the galaxy's own
starlight, but the radial extent of these winds are difficult to
constrain, leaving their energy, momentum, and ultimate fate
uncertain
Wind prescriptions in hydrodynamical simulations are
uncertain and at present are constrained only by indirect
observations, e
g
by their influence on the stellar masses of
galaxies and IGM metallicity
All these doubts lead to one conclusion:
we do not understand gas accretion and feedback because we generally
do not observe the infall and winds directly, in the extended gaseous
halos of galaxies, when it is happening
To do this effectively, we
must harness the power of absorption-line spectroscopy to measure the
density, temperature, metallicity, and kinematics of small quantities
of diffuse gas in galaxy halos
The most important physical
diagnostics lie in the FUV, so this is uniquely a problem for HST and
COS
We propose new COS G130M and G160M observations of 41 QSOs that
probe the gaseous halos of 44 SDSS dwarf galaxies well inside their
virial radii
Using sensitive absorption-line measurements of the
multiphase gas diagnostics Lya, CII/IV, Si II/III/IV, and other
species, supplemented by optical data from SDSS and Keck, we will map
the halos of galaxies with L = 0
02 - 0
3 L*, stellar masses M* =
10^(8-10) Msun, over impact parameter from 15 - 150 kpc
These
observations will directly constrain the content and kinematics of
accreting and outflowing material, provide a concrete target for
simulations to hit, and statistically test proposed galactic superwind
models
These observations will also inform the study of galaxies at
high z, where the shallow halo potentials that host dwarf galaxies
today were the norm
These observations are low-risk and routine for
COS, easily schedulable, and promise a major advance in our
understanding of how dwarf galaxies came to be
STIS/CCD 11845 CCD Dark Monitor Part 2 Monitor the darks for the STIS CCD
STIS/CCD 11847 CCD Bias Monitor-Part 2 Monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1,
and 1x1 at gain = 4, to build up high-S/N superbiases and track the
evolution of hot columns
WFC3/IR 12283 WFC3 Infrared Spectroscopic Parallel Survey (WISP): A Survey of Star
Formation Across Cosmic Time We will use the unique power of WFC3 slitless spectroscopy to measure
cosmic star formation across its peak epoch
The broad, continuous,
spectral coverage of the G102 and G141 grisms provides the best
currently feasible measurement of the star formation rate continuously
from 0
5 Our primary science goals are: (1) Measure ratios of bright emission
lines ([OII], [OIII], Ha, and Hb) in a substantial fraction of these
galaxies, thereby estimating dust and metallicity evolution in a
sample of galaxies that is not biased by photometric selection
(2)
Derive an extinction-corrected Ha luminosity function, with a 20 times
larger sample than our previous NICMOS results
(3) Measure the
mass-metallicity relation at crucial intermediate redshifts, with the
support of our ongoing ground-based, follow-up, observing program (4)
Determine the spectroscopic close pair fraction in this sample, in
order to constrain hierarchal merging models (5) Uncover a new sample
of obscured AGN at these redshifts and, (6) Use the Balmer break
diagnostic to constrain the ages of continuum detected sources down to
H = 25
As a bonus, these observations will be sensitive to Lya emission at
z>5
5, taking advantage of continuous spectral coverage to observe
large volumes for luminous galaxies at the highest redshifts
Over
Cycles 17 and 18, we expect to detect 5-20 LAEs over redshifts
spanning 5
5 < z < 7
5
These observations will likely place the most
stringent constraint on the numbers of z>6
5 Lya emitters until JWST
We are waiving all proprietary rights to our data and will make
high-level data products available through the ST/ECF
WFC3/IR/S/C 11929 IR Dark Current Monitor Analyses of ground test data showed that dark current signals are more
reliably removed from science data using darks taken with the same
exposure sequences as the science data, than with a single dark
current image scaled by desired exposure time
Therefore, dark current
images must be collected using all sample sequences that will be used
in science observations
These observations will be used to monitor
changes in the dark current of the WFC3-IR channel on a day-to-day
basis, and to build calibration dark current ramps for each of the
sample sequences to be used by Gos in Cycle 17
For each sample
sequence/array size combination, a median ramp will be created and
delivered to the calibration database system (CDBS)
WFC3/IR/UV 12163 Structure and Stellar Content of the Nearest Nuclear Clusters in
Late-Type Spiral Galaxies HST surveys have shown that nuclear star clusters are nearly
ubiquitous in late-type, bulgeless disk galaxies
In early-type
galaxies, the central black hole mass correlates with the bulge mass
and velocity dispersion, but the relationship between black hole mass
and host galaxy properties in bulgeless galaxies is not yet
understood
Some nuclear clusters (such as the one in M33) do not
contain a central massive black hole at all, while other late-type
galaxies (such as NGC 4395) are known to contain accretion-powered
active nuclei within their nuclear clusters, indicating that a central
black hole is present
But, the overall "occupation fraction" of black
holes within nuclear clusters is largely unconstrained
Measurement of
the structure, dynamics, and stellar content of nuclear star clusters
is an important pathway toward understanding the demographics of
low-mass black holes in late-type galaxies
We propose to obtain multi-filter WFC3 UV, optical, and near-IR images
of 10 of the nearest and brightest nuclear clusters in late-type
spiral galaxies
We will use the new WFC3 data to measure the cluster
radial profiles, to search for color gradients, and in combination
with ground-based spectroscopy and stellar population modeling, to
determine the stellar masses of the clusters
Since nuclear clusters
are known to contain stellar populations with a wide range of ages,
the broad wavelength coverage of our data will provide new leverage to
constrain the star formation history of the clusters
We will carry
out dynamical modeling for the clusters, using the cluster structural
parameters and stellar M/L ratios measured from the WFC3 data and
kinematics measured from ground-based, adaptive-optics assisted
integral-field spectroscopy (already obtained or approved for 8 of the
10 targets)
This will yield tight new constraints on the masses of
intermediate-mass black holes (IMBH) within the clusters, and may
result in the first dynamical detections of IMBHs in the nuclei of
late-type spirals
WFC3/UV 12215 Searching for the Missing Low-Mass Companions of Massive Stars Recent results on binary companions of massive O stars appear to
indicate that the distribution of secondary masses is truncated at low
masses
It thus mimics the distribution of companions of G dwarfs and
also the Initial Mass Function (IMF), except that it is shifted upward
by a factor of 20 in mass
These results, if correct, provide a
distribution of mass ratios that hints at a strong constraint on the
star-formation process
However, this intriguing result is derived
from a complex simulation of data which suffer from observational
incompleteness at the low-mass end
We propose a snapshot survey to test this result in a very direct way
HST WFC3 images of a sample of the nearest Cepheids (which were
formerly B stars of ~5 Msun) will search for low-mass companions down
to M dwarfs
We will confirm any companions as young stars, and thus
true physical companions, through follow-up Chandra X-ray images
Our
survey will show clearly whether the companion mass distribution is
truncated at low masses, but at a mass much higher than that of the
IMF or G dwarfs
WFC3/UV 12245 Orbital Evolution and Stability of the Inner Uranian Moons Nine densely-packed inner moons of Uranus show signs of chaos and
orbital instability over a variety of time scales
Many moons show
measureable orbital changes within a decade or less
Long-term
integrations predict that some moons could collide in less than one
million years
One faint ring embedded in the system may, in fact, be
the debris left behind from an earlier such collision
Meanwhile, the
nearby moon Mab falls well outside the influence of the others but
nevertheless shows rapid, as yet unexplained, changes in its orbit
It
is embedded within a dust ring that also shows surprising variability
A highly optimized series of observations with WFC3 over the next
three cycles will address some of the fundamental open questions about
this dynamically active system: Do the orbits truly show evidence of
chaos? If so, over what time scales? What can we say about the masses
of the moons involved? What is the nature of the variations in Mab's
orbit? Is Mab's motion predictable or random? Astrometry will enable
us to derive the orbital elements of these moons with 10-km precision
This will be sufficient to study the year-by-year changes and,
combined with other data from 2003-2007, the decadal evolution of the
orbits
The pairing of precise astrometry with numerical integrations
will enable us to derive new dynamical constraints on the masses of
these moons
Mass is the fundamental unknown quantity currently
limiting our ability to reproduce the interactions within this system
This program will also capitalize upon our best opportunity for nearly
40 years to study the unexplained variations in Uranus's faint outer
rings
WFC3/UV 12324 The Temperature Profiles of Quasar Accretion Disks We can now routinely measure the size of quasar accretion disks using
gravitational microlensing of lensed quasars
At optical wavelengths
we observe a size and scaling with black hole mass roughly consistent
with thin disk theory but the sizes are larger than expected from the
observed optical fluxes
One solution would be to use a flatter
temperature profile, which we can study by measuring the wavelength
dependence of the disk size over the largest possible wavelength
baseline
Thus, to understand the size discrepancy and to probe closer
to the inner edge of the disk we need to extend our measurements to UV
wavelengths, and this can only be done with HST
For example, in the
UV we should see significant changes in the optical/UV size ratio with
black hole mass
We propose monitoring 5 lenses spanning a broad range
of black hole masses with well-sampled ground based light curves,
optical disk size measurements and known GALEX UV fluxes during Cycles
17 and 18 to expand from our current sample of two lenses
We would
obtain 5 observations of each target in each Cycle, similar to our
successful strategy for the first two targets
WFC3/UV 12345 UVIS Long Darks Test Darks during SMOV showed a systematically lower global dark rate as
well as lower scatter when compared to the Cycle 17 darks
Those two
sets of exposures differ in exposure time - 1800 sec during SMOV and
900 sec during Cycle 17
Hypothetically, the effect could be caused by
short-duration stray light, say ~500-sec in duration
During the
latter part of Cycle 17, operation of WFC3 was changed to additionally
block the light path to the detector with the CSM
This program
acquires a small number of darks at the longer SMOV exposure times
(1800 sec) in order to check whether the effect repeats in the new
operating mode
WFC3/UVIS 11905 WFC3 UVIS CCD Daily Monitor The behavior of the WFC3 UVIS CCD will be monitored daily with a set
of full-frame, four-amp bias and dark frames
A smaller set of 2Kx4K
subarray biases are acquired at less frequent intervals throughout the
cycle to support subarray science observations
The internals from
this proposal, along with those from the anneal procedure (Proposal
11909), will be used to generate the necessary superbias and superdark
reference files for the calibration pipeline (CDBS)
==============================================================================
TOPIC: HST Status Oct 08, 2010 == 1 of 2 ==
Date: Sat, Oct 9 2010 4:33 pm
From: Paul Scowen The Hubble Space Telescope
Unlocking the Secrets of the Universe Daily Report #5199 Period Covered:
08:00 pm October 7, 2010 - 07:59 pm October 8, 2010
(DOY 281/0000z - 281/2359z) Flight Operations Summary Significant Spacecraft Anomalies: (The following are preliminary reports
of potential non-nominal performance that will be investigated
) HSTARs:
none COMPLETED OPS REQUEST:
none COMPLETED OPS NOTES:
none FGS ACQ STATUS:
SCHEDULED SUCCESSFUL
FGS GSAcq 12 0
FGS REAcq 4 0
OBAD with Maneuver 9 0 SIGNIFICANT EVENTS:
none Program Principal Investigator Program Title
Science Observations Scheduled
11694http://www
stsci
edu/observing/phase2-public/11694
pro David Law, =
University of California - Los Angeles Mapping the Interaction betwee=
n High-Redshift Galaxies and the Intergalactic Environment
12041http://www
stsci
edu/observing/phase2-public/12041
pro James Green=
, University of Colorado at Boulder COS-GTO: Io Atmosphere/STIS
12061http://www
stsci
edu/observing/phase2-public/12061
pro Sandra Fabe=
r, University of California - Santa Cruz Cosmic Assembly Near-IR Deep E=
xtragalactic Legacy Survey -- GOODS-South Field, Early Visits of SNe Search
12178http://www
stsci
edu/observing/phase2-public/12178
pro Scott Ander=
son, University of Washington Spanning the Reionization History of I=
GM Helium: a Highly Efficient Spectral Survey of the Far-UV-Brightest Quasa=
rs
12210http://www
stsci
edu/observing/phase2-public/12210
pro Adam Bolton=
, University of Utah SLACS for the Masses: Extending Strong Lensing to Lowe=
r Masses and Smaller Radii
12234http://www
stsci
edu/observing/phase2-public/12234
pro Wesley Fras=
er, California Institute of Technology Differentiation in the Kuiper =
belt: a search for silicates on icy bodies
12248http://www
stsci
edu/observing/phase2-public/12248
pro Jason Tumli=
nson, Space Telescope Science Institute How Dwarf Galaxies Got That Wa=
y: Mapping Multiphase Gaseous Halos and Galactic Winds Below L*
12251http://www
stsci
edu/observing/phase2-public/12251
pro Zachory Ber=
ta, Harvard University The First Characterization of a Super-Earth At=
mosphere
12283http://www
stsci
edu/observing/phase2-public/12283
pro Matthew Mal=
kan, University of California - Los Angeles WFC3 Infrared Spectroscopic Pa=
rallel Survey {WISP}: A Survey of Star Formation Across Cosmic Time
12307http://www
stsci
edu/observing/phase2-public/12307
pro Andrew Leva=
n, The University of Warwick A public SNAPSHOT survey of gamma-ray burst ho=
st galaxies
Calibration Observations Scheduled
11845http://www
stsci
edu/observing/phase2-public/11845
pro Michael Wol=
fe, Space Telescope Science Institute CCD Dark Monitor Part 2
11847http://www
stsci
edu/observing/phase2-public/11847
pro Michael Wol=
fe, Space Telescope Science Institute CCD Bias Monitor-Part 2
11905http://www
stsci
edu/observing/phase2-public/11905
pro Tiffany Bor=
ders, Space Telescope Science Institute WFC3 UVIS CCD Daily Monitor
11929http://www
stsci
edu/observing/phase2-public/11929
pro Bryan Hilbe=
rt, Space Telescope Science Institute IR Dark Current Monitor
11996http://www
stsci
edu/observing/phase2-public/11996
pro David Golim=
owski, Space Telescope Science Institute CCD Daily Monitor {Part 3}
12380http://www
stsci
edu/observing/phase2-public/12380
pro Bryan Hilbe=
rt, Space Telescope Science Institute Guard Darks == 2 of 2 ==
Date: Sat, Oct 9 2010 4:43 pm
From: Paul Scowen Earlier reportshttp://www
stsci
edu/hst/scheduling/daily_status Convert Day of Yearhttp://disc
gsfc
nasa
gov/julian_calendar
shtml
The Hubble Space Telescope
Unlocking the Secrets of the Universe Daily Report #5199 Period Covered:
08:00 pm October 7, 2010 - 07:59 pm October 8, 2010
(DOY 281/0000z - 281/2359z) Flight Operations Summary Significant Spacecraft Anomalies: (The following are preliminary reports
of potential non-nominal performance that will be investigated
) HSTARs:
none COMPLETED OPS REQUEST:
none COMPLETED OPS NOTES:
none FGS ACQ STATUS:
SCHEDULED SUCCESSFUL
FGS GSAcq 12 0
FGS REAcq 4 0
OBAD with Maneuver 9 0 SIGNIFICANT EVENTS:
none Program Principal Investigator Program Title
Science Observations Scheduled
11694http://www
stsci
edu/observing/phase2-public/11694
pro David Law, University of California - Los Angeles Mapping the Interaction between High-Redshift Galaxies and the Intergalactic Environment
12041http://www
stsci
edu/observing/phase2-public/12041
pro James Green, University of Colorado at Boulder COS-GTO: Io Atmosphere/STIS
12061http://www
stsci
edu/observing/phase2-public/12061
pro Sandra Faber, University of California - Santa Cruz Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey -- GOODS-South Field, Early Visits of SNe Search
12178http://www
stsci
edu/observing/phase2-public/12178
pro Scott Anderson, University of Washington Spanning the Reionization History of IGM Helium: a Highly Efficient Spectral Survey of the Far-UV-Brightest Quasars
12210http://www
stsci
edu/observing/phase2-public/12210
pro Adam Bolton, University of Utah SLACS for the Masses: Extending Strong Lensing to Lower Masses and Smaller Radii
12234http://www
stsci
edu/observing/phase2-public/12234
pro Wesley Fraser, California Institute of Technology Differentiation in the Kuiper belt: a search for silicates on icy bodies
12248http://www
stsci
edu/observing/phase2-public/12248
pro Jason Tumlinson, Space Telescope Science Institute How Dwarf Galaxies Got That Way: Mapping Multiphase Gaseous Halos and Galactic Winds Below L*
12251http://www
stsci
edu/observing/phase2-public/12251
pro Zachory Berta, Harvard University The First Characterization of a Super-Earth Atmosphere
12283http://www
stsci
edu/observing/phase2-public/12283
pro Matthew Malkan, University of California - Los Angeles WFC3 Infrared Spectroscopic Parallel Survey {WISP}: A Survey of Star Formation Across Cosmic Time
12307http://www
stsci
edu/observing/phase2-public/12307
pro Andrew Levan, The University of Warwick A public SNAPSHOT survey of gamma-ray burst host galaxies
Calibration Observations Scheduled
11845http://www
stsci
edu/observing/phase2-public/11845
pro Michael Wolfe, Space Telescope Science Institute CCD Dark Monitor Part 2
11847http://www
stsci
edu/observing/phase2-public/11847
pro Michael Wolfe, Space Telescope Science Institute CCD Bias Monitor-Part 2
11905http://www
stsci
edu/observing/phase2-public/11905
pro Tiffany Borders, Space Telescope Science Institute WFC3 UVIS CCD Daily Monitor
11929http://www
stsci
edu/observing/phase2-public/11929
pro Bryan Hilbert, Space Telescope Science Institute IR Dark Current Monitor
11996http://www
stsci
edu/observing/phase2-public/11996
pro David Golimowski, Space Telescope Science Institute CCD Daily Monitor {Part 3}
12380http://www
stsci
edu/observing/phase2-public/12380
pro Bryan Hilbert, Space Telescope Science Institute Guard Darks ============================================================================== You received this message because you are subscribed to the Google Groups "sci
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