2,933 research outputs found
Fusing Continuous-valued Medical Labels using a Bayesian Model
With the rapid increase in volume of time series medical data available
through wearable devices, there is a need to employ automated algorithms to
label data. Examples of labels include interventions, changes in activity (e.g.
sleep) and changes in physiology (e.g. arrhythmias). However, automated
algorithms tend to be unreliable resulting in lower quality care. Expert
annotations are scarce, expensive, and prone to significant inter- and
intra-observer variance. To address these problems, a Bayesian
Continuous-valued Label Aggregator(BCLA) is proposed to provide a reliable
estimation of label aggregation while accurately infer the precision and bias
of each algorithm. The BCLA was applied to QT interval (pro-arrhythmic
indicator) estimation from the electrocardiogram using labels from the 2006
PhysioNet/Computing in Cardiology Challenge database. It was compared to the
mean, median, and a previously proposed Expectation Maximization (EM) label
aggregation approaches. While accurately predicting each labelling algorithm's
bias and precision, the root-mean-square error of the BCLA was
11.780.63ms, significantly outperforming the best Challenge entry
(15.372.13ms) as well as the EM, mean, and median voting strategies
(14.760.52ms, 17.610.55ms, and 14.430.57ms respectively with
)
Hard - X-rays selected Active Galactic Nuclei. I. A radio view at high-frequencies
A thorough study of radio emission in Active Galactic Nuclei (AGN) is of
fundamental importance to understand the physical mechanisms responsible for
the emission and the interplay between accretion and ejection processes. High
frequency radio observations can target the nuclear contribution of smaller
emitting regions and are less affected by absorption. We present JVLA 22 and 45
GHz observations of 16 nearby (0.003z0.3) hard - X-rays selected AGN
at the (sub)-kpc scale with tens uJy beam sensitivity. We detected 15/16
sources, with flux densities ranging from hundreds uJy beam to tens Jy
(specific luminosities from 10 to 10 at
22 GHz). All detected sources host a compact core, with 8 being core-dominated
at either frequencies, the others exhibiting also extended structures. Spectral
indices range from steep to flat/inverted. We interpret this evidence as either
due to a core+jet system (6/15), a core accompanied by surrounding star
formation (1/15), to a jet oriented close to the line of sight (3/15), to
emission from a corona or the base of a jet (1/15), although there might be
degeneracies between different processes. Four sources require more data to
shed light on their nature. We conclude that, at these frequencies, extended,
optically-thin components are present together with the flat-spectrum core. The
relation is roughly followed, indicating a possible
contribution to radio emission from a hot corona. A weakly significant
correlation between radio core (22 and 45 GHz) and X-rays luminosities is
discussed in the light of an accretion-ejection framework.Comment: Accepted for publication on MNRA
Absorption spectra of Fe L-lines in Seyfert 1 galaxies
Absorption L-lines of iron ions are observed, in absorption, in spectra of
Seyfert 1 galaxies by the new generation of X-ray satellites: Chandra (NASA)
and XMM-Newton (ESA). Lines associated to Fe23+ to Fe17+ are well resolved.
Whereas, those corresponding to Fe16+ to Fe6+ are unresolved. Forbidden
transitions of the Fe16+ to Fe6+ ions were previously observed, for the same
objects, in the visible and infra-red regions, showing that the plasma had a
low density. To interpret X-ray, visible and infra-red data, astrophysical
models assume an extended absorbing medium of very low density surrounding an
intense X-ray source. We have calculated atomic data (wavelengths, radiative
and autoionization rates) for n=2 to n'=3-4 transitions and used them to
construct refined synthetic spectra of the unresolved part of the L-line
spectra.Comment: 17 pages, 5 figures, Journal of Quantitative Spectroscopy and
Radiative Transfer, in pres
Dielectronic Recombination (via N=2 --> N'=2 Core Excitations) and Radiative Recombination of Fe XX: Laboratory Measurements and Theoretical Calculations
We have measured the resonance strengths and energies for dielectronic
recombination (DR) of Fe XX forming Fe XIX via N=2 --> N'=2 (Delta_N=0) core
excitations. We have also calculated the DR resonance strengths and energies
using AUTOSTRUCTURE, HULLAC, MCDF, and R-matrix methods, four different
state-of-the-art theoretical techniques. On average the theoretical resonance
strengths agree to within <~10% with experiment. However, the 1 sigma standard
deviation for the ratios of the theoretical-to-experimental resonance strengths
is >~30% which is significantly larger than the estimated relative experimental
uncertainty of <~10%. This suggests that similar errors exist in the calculated
level populations and line emission spectrum of the recombined ion. We confirm
that theoretical methods based on inverse-photoionization calculations (e.g.,
undamped R-matrix methods) will severely overestimate the strength of the DR
process unless they include the effects of radiation damping. We also find that
the coupling between the DR and radiative recombination (RR) channels is small.
We have used our experimental and theoretical results to produce
Maxwellian-averaged rate coefficients for Delta_N=0 DR of Fe XX. For kT>~1 eV,
which includes the predicted formation temperatures for Fe XX in an optically
thin, low-density photoionized plasma with cosmic abundances, our experimental
and theoretical results are in good agreement. We have also used our R-matrix
results, topped off using AUTOSTRUCTURE for RR into J>=25 levels, to calculate
the rate coefficient for RR of Fe XX. Our RR results are in good agreement with
previously published calculations.Comment: To be published in ApJS. 65 pages with 4 tables and lots of figure
The radio emission in radio-quiet quasars: the VLBA perspective
The origin of the radio emission in radio-quiet quasars (RQQ) is not
established yet. We present new VLBA observations at 1.6 and 4.9 GHz of ten RQQ
(nine detected), which together with published earlier observations of eight
RQQ (five detected), forms a representative sample of 18 RQQ drawn from the
Palomar-Green sample of low z (< 0.5) AGN. The spectral slope of the integrated
emission extends from very steep (alpha < -1.98) to strongly inverted (alpha =
+2.18), and the slopes of nine of the 14 objects are flat (alpha > -0.5). Most
objects have an unresolved flat-spectrum core, which coincides with the optical
Gaia position. The extended emission is generally steep-spectrum, has a low
brightness temperature (< 10^7 K), and is displaced from the optical core (the
Gaia position) by ~ 5-100 pc. The VLBA core flux is tightly correlated with the
X-ray flux, and follows a radio to X-ray luminosity relation of log L_R/L_X =
-6, for all objects with a black hole mass log M_BH/M_Sun < 8.5. The flatness
of the core emission implies a compact source size (< 0.1 pc), which likely
originates from the accretion disk corona. The mas-scale extended emission is
optically thin and of clumpy structure, and is likely produced by an outflow
from the center. Radio observations at higher frequencies can further test the
accretion disk coronal emission interpretation for the core emission in RQQ.Comment: Accepted for publication in MNRA
Estudio de las transiciones beta primeras prohibidas en el Au 198, Ce 141 y Pr 144
Fil: Behar, D. Moni. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina
A genetic contribution from the Far East into Ashkenazi Jews via the ancient Silk Road
Contemporary Jews retain a genetic imprint from their Near Eastern ancestry, but obtained substantial genetic components from their neighboring populations during their history. Whether they received any genetic contribution from the Far East remains unknown, but frequent communication with the Chinese has been observed since the Silk Road period. To address this issue, mitochondrial DNA (mtDNA) variation from 55,595 Eurasians are analyzed. The existence of some eastern Eurasian haplotypes in eastern Ashkenazi Jews supports an East Asian genetic contribution, likely from Chinese. Further evidence indicates that this connection can be attributed to a gene flow event that occurred less than 1.4 kilo-years ago (kya), which falls within the time frame of the Silk Road scenario and fits well with historical records and archaeological discoveries. This observed genetic contribution from Chinese to Ashkenazi Jews demonstrates that the historical exchange between Ashkenazim and the Far East was not confined to the cultural sphere but also extended to an exchange of genes
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