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Daily Report #5062



 
 
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Old March 29th 10, 05:09 PM posted to sci.astro.hubble
Cooper, Joe
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Default Daily Report #5062

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5062

PERIOD COVERED: 5am March 26 - 5am March 29, 2010 (DOY 085/09:00z-088/09:00z)

OBSERVATIONS SCHEDULED

ACS/WFC 12016

The Stars and Edge-on Disks of PDS 144: An Intermediate-Mass Analog of
Wide T Tauri Multiple Stars

High-Inclination PMS stars are optimally oriented to measure disk
size, height, to detect jets, and to directly probe disk composition.
Placing these data into evolutionary context requires dates for the
systems and measurements of L bol, and extinction. For such stars,
X-ray data provide L x, but also N(H) and the total extinction. FUV
data measures L UV, and constrains the shape of the extinction curve.
Recent studies have suggested that the frequency of Jovian-mass
planets is higher for systems with intermediate-mass stars, due to
disk mass or composition. While suitable low mass YSOs are
well-represented in the Chandra and HST archives, similar data are
lacking for higher mass systems. We propose joint Chandra and HST
imaging of PDS 144 to fill this gap.

COS/FUV 12011

Magnetic Heating of the Outer Atmospheres of Very Low Mass Dwarfs

The detections of FUV and X-ray emissions from very low mass stars and
brown dwarfs have confirmed that stellar magnetic activity can survive
even at these low stellar masses. The emissions are qualitatively
similar to those from active stars, despite the dramatic differences
between the characteristics of an ultracool (M7) stellar atmosphere
and those of earlier type cool stars. It is currently an open question
how the structures and magnetic heating which exists in these very low
mass stars compare with those seen in higher mass active stars. We
propose to take Chandra and HST/COS spectra of two nearby active very
low mass stars in order to determine the effect that these large-scale
fields have on transition region and coronal structures.

ACS/WFC 11995

CCD Daily Monitor (Part 2)

This program comprises basic tests for measuring the read noise and
dark current of the ACS WFC and for tracking the growth of hot pixels.
The recorded frames are used to create bias and dark reference images
for science data reduction and calibration. This program will be
executed four days per week (Mon, Wed, Fri, Sun) for the duration of
Cycle 17. To facilitate scheduling, this program is split into three
proposals. This proposal covers 320 orbits (20 weeks) from 1 February
2010 to 20 June 2010.

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 11928

WFC3/IR Low-Frequency Flat and Geometric Distortion

Multiple observations of globular cluster Omega Cen at multiple
infrared wavelengths of IR detector will be used to derive filter
dependency of low-frequency sensitivity (L_flat fields) across of IR
detector and its time variation. Additionally, the same data will be
also used to derive filter-dependant geometric distortion of the
detector and its time-dependency.

WFC3/UVIS 11924

WFC3/UVIS External and Internal CTE Monitor

CCD detector Charge Transfer Inefficiency (CTI)-induced losses in
photometry and astrometry will be measured using observations of the
rich open cluster NGC6791 and with the EPER (Extended Pixel Edge
Response) method using tungsten lamp flat field exposures. Although we
do not expect to see CTE effects at the outset of Cycle 17, this CTE
monitoring program is the first of a multi-cycle program to monitor
and establish CTE-induced losses with time. We expect to measure CTE
effects with a precision comparable to the ACS measurements.

WFC3/UVIS 11908

Cycle 17: UVIS Bowtie Monitor

Ground testing revealed an intermittent hysteresis type effect in the
UVIS detector (both CCDs) at the level of ~1%, lasting hours to days.
Initially found via an unexpected bowtie-shaped feature in flatfield
ratios, subsequent lab tests on similar e2v devices have since shown
that it is also present as simply an overall offset across the entire
CCD, i.e., a QE offset without any discernable pattern. These lab
tests have further revealed that overexposing the detector to count
levels several times full well fills the traps and effectively
neutralizes the bowtie. Each visit in this proposal acquires a set of
three 3x3 binned internal flatfields: the first unsaturated image will
be used to detect any bowtie, the second, highly exposed image will
neutralize the bowtie if it is present, and the final image will allow
for verification that the bowtie is gone.

WFC3/UVIS 11907

UVIS Cycle 17 Contamination Monitor

The UV throughput of WFC3 during Cycle 17 is monitored via weekly
standard star observations in a subset of key filters covering
200-600nm and F606W, F814W as controls on the red end. The data will
provide a measure of throughput levels as a function of time and
wavelength, allowing for detection of the presence of possible
contaminants.

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).

COS/NUV 11900

NUV Internal/External Wavelength Scale Monitor

This program monitors the offsets between the wavelength scale set by
the internal wavecal versus that defined by absorption lines in
external targets. This is accomplished by observing two external
radial velocity standard targets: HD187691 with G225M and G285M and
HD6655 with G285M and G230L. The two standard targets have little flux
in the wavelength range covered by G185M and so Feige 48 (sdO) is
observed with this grating. Both Feige 48 and HD6655 are also observed
in SMOV. The cenwaves observed in this program are a subset of the
ones used during Cycle 17. Observing all cenwaves would require a
considerably larger number of orbits. Constraints on scheduling of
each target are placed so that each target is observed once every ~2-3
months. Observing the three targets every month would also require a
considerably larger number of orbits.

STIS/CC 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.

STIS/CC 11845

CCD Dark Monitor Part 2

Monitor the darks for the STIS CCD.

WFC3/IR 11738

SPIDERWEBS AND FLIES: OBSERVING MASSIVE GALAXY FORMATION IN ACTION

Distant luminous radio galaxies are among the brightest known galaxies
in the early Universe, pinpoint likely progenitors of dominant cluster
galaxies and are unique laboratories for studying massive galaxy
formation. Spectacular images with the ACS and NICMOS of one such
object, the "Spiderweb Galaxy" at z = 2.2, show in exquisite detail,
hierarchical merging occurring 11 Gyr ago. By imaging 3 additional
Spiderweb-like galaxies we wish to study this potentially crucial
phase of massive galaxy evolution, when hierarchical merging, galaxy
downsizing and AGN feedback are all likely to be occurring. Properties
of the complete sample of Spiderweb galaxies will be used to (i)
constrain models for the formation and evolution of the most massive
galaxies that dominate rich clusters and (ii) investigate the nature
of chain and tadpole galaxies, a fundamental but poorly understood
constituent of the early Universe.

We shall image rest-frame UV and optical continuum emission from 3
radio galaxies with 2.4 z 3.8 that appear clumpy and large in
shallow WFPC/PC observations. The new observations will typically
reach ~2 magnitudes fainter over 20-40 times larger area than
previously. Photometric and morphological parameters will be measured
for satellite galaxies ("flies") in the clumpy massive hosts and for
galaxies in ~ 1.5 Mpc x 1.5 Mpc regions of surrounding protoclusters.
Locations, sizes, elongations, clumpiness, masses, and star formation
rates of the merging satellite and protocluster galaxies will be
compared with new state of the art simulations. Combination of ACS and
WFC3 images will help disentangle the properties of the young and old
populations.

Specific goals include: (i) investigating star formation histories of
the satellite galaxies and the extended emission, (ii) studying
"downsizing" and merging scenarios and (iii) measuring the statistics
of linear galaxies and relating them to models for the formation of
massive galaxies and to the properties of the important but enigmatic
class of chain/tadpole galaxies in the HUDF.

ACS/WFC 11715

The Luminous Galactic Cepheid RS Puppis: A Geometric Distance from its
Nested Light Echoes

RS Puppis is one of the most luminous Cepheids in the Milky Way (P =
41.4 days) and an analog of the bright Cepheids used to measure
extragalactic distances. An accurate distance would help anchor the
zero-point of the bright end of the period-luminosity relation, but at
a distance of about 2 kpc it is too far away for a trigonometric
parallax with existing instrumentation.

RS Pup is unique in being surrounded by a reflection nebula, whose
brightness varies as pulses of light from the Cepheid propagate
outwards. Members of our team have used ground-based imaging of the
nebula to derive phase lags in the light variations of individual
features in the nebula, and have inferred a seemingly very precise
geometric distance to the star. However, there is an unavoidable
ambiguity involving the cycle counts, which was resolved by assuming
that the features lie in the plane of the sky. If this assumption is
incorrect, a large systematic error would be introduced into the
distance measurement.

We show that polarimetric imaging using the high spatial resolution of
ACS/WFC and its ability to image close to the star can resolve this
ambiguity and yield a reliable geometric distance to RS Pup. We will
also obtain a wide-field multicolor image of the nebula, in order to
study its morphology and the mass-loss history of the Cepheid.

COS/FUV 11687

SNAPing Coronal Iron

This is a Snapshot Survey to explore two forbidden lines of highly
ionized iron in late-type coronal sources. Fe XII 1349 (T~ 2 MK) and
Fe XXI 1354 (T~ 10 MK) -- well known to Solar Physics -- have been
detected in about a dozen cool stars, mainly with HST/STIS. The UV
coronal forbidden lines are important because they can be observed
with velocity resolution of better than 15 km/s, whereas even the
state-of-the-art X-ray spectrometers on Chandra can manage only 300
km/s in the kilovolt band where lines of highly ionized iron more
commonly are found. The kinematic properties of hot coronal plasmas,
which are of great interest to theorists and modelers, thus only are
accessible in the UV at present. The bad news is that the UV coronal
forbidden lines are faint, and were captured only in very deep
observations with STIS. The good news is that 3rd-generation Cosmic
Origins Spectrograph, slated for installation in HST by SM4, in a mere
25 minute exposure with its G130M mode can duplicate the sensitivity
of a landmark 25-orbit STIS E140M observation of AD Leo, easily the
deepest such exposure of a late-type star so far. Our goal is to build
up understanding of the properties of Fe XII and Fe XXI in additional
objects beyond the current limited sample: how the lineshapes depend
on activity, whether large scale velocity shifts can be detected, and
whether the dynamical content of the lines can be inverted to map the
spatial morphology of the stellar corona (as in "Doppler Imaging'').
In other words, we want to bring to bear in the coronal venue all the
powerful tricks of spectroscopic remote sensing, well in advance of
the time that this will be possible exploiting the corona's native
X-ray radiation. The 1290-1430 band captured by side A of G130M also
contains a wide range of key plasma diagnostics that form at
temperatures from below 10, 000 K (neutral lines of CNO), to above
200, 000 K (semi-permitted O V 1371), including the important bright
multiplets of C II at 1335 and Si IV at 1400; yielding a diagnostic
gold mine for the subcoronal atmosphere. Because of the broad value of
the SNAP spectra, beyond the coronal iron project, we waive the normal
proprietary rights.

STIS/CC 11654

UV Studies of a Core Collapse Supernova

Observations of the UV spectrum of core collapse SNe hold unique
information about nucleosynthesis, the mass loss history, shock
physics and dust formation in the explosion on massive stars. This
proposal aims at a detailed study of a bright core collapse SN,
discovered by any of the many ongoing surveys, either a Type IIP, IIn
or Ibc supernova. We will address the role of circumstellar
interaction and mass loss through CNO lines in the UV, the nature of
dust formation from UV line profiles and use the UV continuum as a
diagnostic of non-thermal emission from the shock. The overall goal of
our team is to achieve a better understanding of these objects by
combining HST data with complementary ground-based observations. We
have used HST to obtain UV spectra from the explosion to the nebular
phase. Over the past decade, we have conducted studies of nearby SNe
with HST, and we have published an extensive series of papers. When
Nature provides a bright candidate, HST should be ready to respond.

COS/NUV 11651

Is the Atmosphere of the Hottest Known Transiting Exoplanet
Evaporating?

WASP-12 is the hottest and the largest currently known transiting
exoplanet. It has the shortest orbital period and is the closest to
its host star. Previous spectacular HST observations revealed that the
atmosphere of HD 209458b appears to be evaporating away, though this
interpretation has recently been questioned. We propose ultraviolet
observations of WASP-12 to learn whether it is in a state of
hydrodynamic 'blow-off' as the work on HD 209458b would suggest. We
will obtain a precise radius for the planet, free from systematic
errors caused by the earth's atmosphere. We will use our data to hone
models of exoplanet atmospheres.

ACS/WFC3 11604

The Nuclear Structure of OH Megamaser Galaxies

We propose a snapshot survey of a complete sample of 80 OH megamaser
galaxies. Each galaxy will be imaged with the ACS/WFC through F814W
and a linear ramp filter (FR656N or FR716N or FR782N or FR853N)
allowing us to study both the spheroid and the gas morphology in
Halpha + [N II]. We will use the 9% ramps FR647M (5370-7570 angstroms)
centered at 7000 angstroms and FR914M (7570-10, 719 angstroms) 8000
angstroms for continuum subtraction for the high and low z objects
respectively. OH megamaser galaxies (OHMG) form an important class of
ultraluminous IR-galaxies (ULIRGs) whose maser lines emit QSO-like
luminosities. ULIRGs in general are associated with recent mergers but
it is often unclear whether their power output is dominated by
starbursts or a hidden QSO because of the high absorbing columns which
hide their nuclei even at X-ray wavelengths. In contrast, OHMG exhibit
strong evidence for the presence of an energetically important and
recently triggered active nucleus. In particular it is clear that much
of the gas must have already collapsed to form a nuclear disk which
may be the progenitor of a circum-nuclear torus, a key element of the
unified scheme of AGN. A great advantage of studying OHMG systems over
the general ULIRG population, is that the circum-nuclear disks are
effectively "fixed" at an inner, edge on, orientation, eliminating
varying inclination as a nuisance parameter. We will use the HST
observations in conjunction with existing maser and spectroscopic data
to construct a detailed picture of the circum-nuclear regions of a
hitherto relatively neglected class of galaxy that may hold the key to
understanding the relationship between galaxy mergers, nuclear
star-formation, and the growth of massive black holes and the
triggering of nuclear activity.

STIS/CCD/MA2 11568

A SNAPSHOT Survey of the Local Interstellar Medium: New NUV
Observations of Stars with Archived FUV Observations

We propose to obtain high-resolution STIS E230H SNAP observations of
MgII and FeII interstellar absorption lines toward stars within 100
parsecs that already have moderate or high-resolution far-UV (FUV),
900-1700 A, observations available in the MAST Archive. Fundamental
properties, such as temperature, turbulence, ionization, abundances,
and depletions of gas in the local interstellar medium (LISM) can be
measured by coupling such observations. Due to the wide spectral range
of STIS, observations to study nearby stars also contain important
data about the LISM embedded within their spectra. However, unlocking
this information from the intrinsically broad and often saturated FUV
absorption lines of low-mass ions, (DI, CII, NI, OI), requires first
understanding the kinematic structure of the gas along the line of
sight. This can be achieved with high resolution spectra of high-mass
ions, (FeII, MgII), which have narrow absorption lines, and can
resolve each individual velocity component (interstellar cloud). By
obtaining short (~10 minute) E230H observations of FeII and MgII, for
stars that already have moderate or high- resolution FUV spectra, we
can increase the sample of LISM measurements, and thereby expand our
knowledge of the physical properties of the gas in our galactic
neighborhood. STIS is the only instrument capable of obtaining the
required high resolution data now or in the foreseeable future.

STIS/CCD 11567

Boron Abundances in Rapidly Rotating Early-B Stars

Models of rotation in early-B stars predict that rotationally driven
mixing should deplete surface boron abundances during the
main-sequence lifetime of many stars. However, recent work has shown
that many boron depleted stars are intrinsically slow rotators for
which models predict no depletion should have occurred, while
observations of nitrogen in some more rapidly rotating stars show less
mixing than the models predict. Boron can provide unique information
on the earliest stages of mixing in B stars, but previous surveys have
been biased towards narrow- lined stars because of the difficulty in
measuring boron abundances in rapidly rotating stars. The two targets
observed as part of our Cycle 13 SNAP program 10175, just before STIS
failed, demonstrate that it is possible to make useful boron abundance
measurements for early-B stars with Vsin(i) above 100 km/s. We propose
to extend that survey to a large enough sample of stars to allow
statistically significant tests of models of rotational mixing in
early-B stars.

COS/NUV/FUV 11555

Transition Region and Chromospheric Activity on Low Metallicity
Arcturus Moving Group `Alien' Dwarfs

How does low metallicity affect the heating and resultant temperature
structure of the chromospheres, transition regions, and coronae of old
solar-like dwarf stars?

The Arcturus Moving Group is very likely a remnant of the merger of a
dwarf galaxy with the Milky Way Galaxy in the distant (~ 7- 8 Gyr)
past. This kinematically distinct group has members that are located
very close to the Sun, allowing study of stellar activity on very old,
low metallicity stars that typically would not be possible. We propose
to obtain COS G140L spectra of four dwarf star members of the Arcturus
Moving Group to measure the fluxes of their transition region and
upper chromospheric emission lines and to investigate the effects of
low metallicity on the outer atmospheric radiative losses and
temperature structure. Our targets have metallicities of ~ 20% solar
or less, spectral types F9 - M4, and are at distances less than 25 pc
from the Sun. COS is the only UV spectrograph that is capable of
registering the FUV spectra of these stars in a reasonable number of
HST orbits.

COS/FUV 11524

COS-GTO: Warm and Hot ISM In and Near the Milky Way

COS G130M and G160M 20, 000 resolution observations will be obtained
for 10 AGNs situated beyond Milky Way high velocity clouds. For all
objects good O VI line profile observations exist from FUSE and high
velocity O VI is detected. The COS observations will be used to obtain
high quality absorption line profiles (S/N ~ 30 to 40) for C IV, Si IV
and N V in the low and high velocity gas toward each AGN. The high
ionization profiles of O VI (from FUSE), N V, C IV, and Si IV will be
compared to low ionization profiles (O I, S II, Si II, Fe II, etc.) in
order to evaluate the physical conditions and origins of the highly
ionized gas in and near the Milky Way at low and high velocity. The
HVCs include Complex C (four lines of sight), Complex A, WD, WB, and
several negative velocity O VI HVCs. Other studies to be undertaken
with this data set include studies of the physical conditions and
abundances in the cool and warm HVC gas and studies of the physical
conditions in low redshift IGM systems detected along the 10 lines of
sight.

COS/NUV/FUV/WFC3/UVI 11520

S/IR COS-GTO: QSO Absorbers, Galaxies and Large-Scale Structures in
the Local Universe

This is a program to probe the large scale structure of baryons in the
universe, including addressing questions of baryon fraction, physical
conditions and relationships between absorbers and large-scale
structures of galaxies. Besides these specific goals, this proposed
GTO program also probes a large enough total path length in Ly alpha
and OVI to add significantly to what STIS/FUSE has already observed.
Several Galactic High Velocity Cloud Complexes also are probed by
these sightlines, particularly the M Complex. The total path length of
this proposed program for Ly alpha large-scale structure surveys is
delta_z~5.5.

We have selected a variety of targets to address these questions,
under the following subcategories:

1. Target 8 bright BL Lac objects to search for low contrast Ly alpha
absorbers from the warm- hot interstellar medium (WHIM).

2. Ly alpha cloud sizes: The targets are a bright AGN pair which yield
tangential distance separations of 100--500 kpc at z=0.01--0.05, where
galaxy surveys are excellent. This pair has two filaments and two
voids in this distance range.

3. Probes of starburst outflows: The targets are bright AGN, = 100
kpc in projection out of the minor axis of nearby starburst galaxies.

4. A large galaxy's gaseous halo: Three probes of the kinematics and
metallicity of a single L* galaxy halo. These observations includes
G130M, G160M exposures at SNR~20 and G285M at 2850A and SNR~10 for
MgII. The 2L* galaxy, ESO 157-G049 (cz=1678 km/s), being probed by
these sightlines has an available H I 21cm map from ATCA, H alpha
imaging from CTIO and long- slit spectra from MSSSO.

5. Dwarf galaxy winds: These targets probe the kinematics and
metallicities of outflows from active and inactive (in terms of star
formation) dwarfs.

STIS/CC/MA 11516

COS-GTO: Cold ISM

With the COS, we will be able to observe interstellar spectra in a new
regime, translucent clouds, for atomic, ionic, and molecular lines and
bands, and extinction curves. The COS will allow us to observe stars
with total visual extinctions up to 10 magnitudes, and the grain size
indicator Rv up to 4.5. In translucent clouds we expect to see the
transition from neutral and ionized carbon to mostly C I, and then
from there, we should expect to see carbon increasingly locked up in
molecular form, as CO. Other species are expected to make similar
transitions, so we should find detectable abundances of molecules such
as H2O, OH, CS, CH2, SiO, and others; also, lower ionization fractions
of the metallic elements - and higher depletions of those elements as
well. Given that we expect to find higher depletions, we should see an
altered grain size distribution, which may show up in the extinction
curves, probably as lower far-UV extinction than in diffuse clouds.
Finally, we will search for neutral PAHs in absorption, as diffuse
bands in the UV, paralleling the optical DIBs (which are thought by
some scientists to be formed by singly-ionized PAHs). In translucent
clouds, models show that the PAHs will be neutral, not in cationic
form.

NIC3/WFC3/IR 11149

Characterizing the Stellar Populations in Lyman-Alpha Emitters and
Lyman Break Galaxies at 5.7z7 in the Subaru Deep Field

The epoch of reionization marks a major phase transition of the
Universe, during which the intergalactic space became transparent to
UV photons. Determining when this occurred and the physical processes
involved represents the latest frontier in observational cosmology.
Over the last few years, searches have intensified to identify the
population of high-redshift (z6) galaxies that might be responsible
for this process, but the progress is hampered partly by the
difficulty of obtaining physical information (stellar mass, age, star
formation rate/history) for individual sources. This is because the
number of z6 galaxies that have both secure spectroscopic redshifts
and high-quality infrared photometry (especially with Spitzer/IRAC) is
still fairly small. Considering that only several photometric points
are available per source, and that many model SEDs are highly
degenerate, it is crucial to obtain as many observational constraints
as possible for each source to ensure the validity of SED modeling. To
better understand the physical properties of high-redshift galaxies,
we propose here to conduct HST/NICMOS (72 orbits) and Spitzer/IRAC
(102 hours) imaging of spectroscopically confirmed, bright (z26 mag
(AB)) Ly-alpha emitters (LAEs) and Lyman-break galaxies (LBGs) at
5.7z7 selected from the Subaru Deep Field. Spectroscopic redshifts
remove one critical free parameter from SED modeling while bright
source magnitudes ensure high-quality photometric data. By making
accurate determinations of stellar masses, ages, and star-formation
histories, we will specifically address the following major questions:
(1) Do LAEs and LBGs represent physically different galaxy populations
at z6 as suggested recently? (2) Is Ly-alpha emission systematically
suppressed at z6 with respect to continuum emission? (i.e., are we
reaching the epoch of incomplete reionization?), and (3) Do we see any
sign of abnormally young stellar population in any of the z6
galaxies?

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 17 17
FGS REAcq 23 23
OBAD with Maneuver 14 14

SIGNIFICANT EVENTS: (None)


 




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