pinecone/core-2020-05-10-deduplication huggingface dataset:
Multiplicity dependence of the average transverse momentum in pp, p-Pb,
  and Pb-Pb collisions at the LHC

The average transverse momentum $\langle p_{\rm T}\rangle$ versus the
charged-particle multiplicity $N_{\rm ch}$ was measured in p-Pb collisions at a
collision energy per nucleon-nucleon pair $\sqrt{s_{\rm NN}}=5.02$ TeV and in
pp collisions at collision energies of $\sqrt{s}=0.9$, 2.76, and 7 TeV in the
kinematic range $0.15<p_{\rm T}<10.0$ GeV/$c$ and $|\eta|<0.3$ with the ALICE
apparatus at the LHC. These data are compared to results in Pb-Pb collisions at
$\sqrt{s_{\rm NN}}=2.76$ TeV at similar charged-particle multiplicities. In pp
and p-Pb collisions, a strong increase of $\langle p_{\rm T}\rangle$ with
$N_{\rm ch}$ is observed, which is much stronger than that measured in Pb-Pb
collisions. For pp collisions, this could be attributed, within a model of
hadronizing strings, to multiple-parton interactions and to a final-state color
reconnection mechanism. The data in p-Pb and Pb-Pb collisions cannot be
described by an incoherent superposition of nucleon-nucleon collisions and pose
a challenge to most of the event generators.Comment: 18 pages, 4 captioned figures, 2 tables, authors from page 12,
  published version, figures at http://aliceinfo.cern.ch/ArtSubmission/node/59
X-ray nuclear activity in S4G barred galaxies: No link between bar
  strength and co-occurrent supermassive black hole fueling

Stellar bars can lead to gas inflow toward the center of a galaxy and
stimulate nuclear star formation. However, there is no compelling evidence on
whether they also feed a central supermassive black hole: by measuring the
fractions of barred active and inactive galaxies, previous studies have yielded
conflicting results. In this paper, we aim to understand the lack of
observational evidence for bar-driven active galactic nucleus (AGN) activity by
studying a sample of 41 nearby (d < 35 Mpc) barred galaxies from the Spitzer
Survey for Stellar Structure in Galaxies. We use Chandra observations to
measure nuclear 2--10 keV X-ray luminosities and estimate Eddington ratios,
together with Spitzer 3.6um imaging to quantify the strength of the stellar bar
in two independent ways: (1) from its structure, as traced by its ellipticity
and boxiness, and (2) from its gravitational torque Q_b, taken as the maximum
ratio of the tangential force to the mean background radial force. In this way,
rather than discretizing the presence of both stellar bars and nuclear
activity, we are able to account for the continuum of bar strengths and degrees
of AGN activity. We find nuclear X-ray sources in 31 out of 41 galaxies with
median X-ray luminosity and Eddington ratio of L_X=4.3x10^{38} erg/s and
L_bol/L_Edd=6.9x10^{-6} respectively, consistent with low-luminosity AGN
activity. Including upper limits for those galaxies without nuclear detections,
we find no significant correlation between any of the bar strength indicators
and the degree of nuclear activity, irrespective of galaxy luminosity, stellar
mass, Hubble type, or bulge size. Strong bars do not favor brighter or more
efficient nuclear activity, implying that at least for the low-luminosity
regime, supermassive black hole fueling is not closely connected to large scale
features.Comment: 16 pages, 6 figures, accepted for publication in Ap
Reconstructing the density and temperature structure of prestellar cores
  from $Herschel$ data: A case study for B68 and L1689B

Utilizing multi-wavelength dust emission maps acquired with $Herschel$, we
reconstruct local volume density and dust temperature profiles for the
prestellar cores B68 and L1689B using inverse-Abel transform based technique.
We present intrinsic radial dust temperature profiles of starless cores
directly from dust continuum emission maps disentangling the effect of
temperature variations along the line of sight which was previously limited to
the radiative transfer calculations. The reconstructed dust temperature
profiles show a significant drop in core center, a flat inner part, and a
rising outward trend until the background cloud temperature is reached. The
central beam-averaged dust temperatures obtained for B68 and L1689B are 9.3
$\pm$ 0.5 K and 9.8 $\pm$0.5 K, respectively, which are lower than the
temperatures of 11.3 K and 11.6 K obtained from direct SED fitting. The best
mass estimates derived by integrating the volume density profiles of B68 and
L1689B are 1.6 M_sol and 11 M_sol, respectively. Comparing our results for B68
with the near-infrared extinction studies, we find that the dust opacity law
adopted by the HGBS project, $\kappa_{\lambda} =0.1(\lambda/300 \mu m)^{-2}$,
agrees to within 50% with the dust extinction constraintsComment: 10 pages, 7 figures, Accepted for publication to A&
Study Majorana Neutrino Contribution to B-meson Semi-leptonic Rare
  Decays

B meson semi-leptonic rare decays are sensitive to new physics beyond
standard model. We study the $B^{-}\to \pi^{-}\mu^{+}\mu^{-}$ process and
investigate the Majorana neutrino contribution to its decay width. The
constraints on the Majorana neutrino mass and mixing parameter are obtained
from this decay channel with the latest LHCb data. Utilizing the best fit for
the parameters, we study the lepton number violating decay $B^{-}\to
\pi^{+}\mu^{-}\mu^{-}$, and find its branching ratio is about
$6.4\times10^{-10}$, which is consistent with the LHCb data reported recently.Comment: 10 pages, 3 figure
The $16$th Hilbert problem on algebraic limit cycles

For real planar polynomial differential systems there appeared a simple
version of the $16$th Hilbert problem on algebraic limit cycles: {\it Is there
an upper bound on the number of algebraic limit cycles of all polynomial vector
fields of degree $m$?} In [J. Differential Equations, 248(2010), 1401--1409]
Llibre, Ram\'irez and Sadovskia solved the problem, providing an exact upper
bound, in the case of invariant algebraic curves generic for the vector fields,
and they posed the following conjecture: {\it Is $1+(m-1)(m-2)/2$ the maximal
number of algebraic limit cycles that a polynomial vector field of degree $m$
can have?}
  In this paper we will prove this conjecture for planar polynomial vector
fields having only nodal invariant algebraic curves. This result includes the
Llibre {\it et al}\,'s as a special one. For the polynomial vector fields
having only non--dicritical invariant algebraic curves we answer the simple
version of the 16th Hilbert problem.Comment: 16. Journal Differential Equations, 201
Planck intermediate results. XXX. The angular power spectrum of
  polarized dust emission at intermediate and high Galactic latitudes

The polarized thermal emission from Galactic dust is the main foreground
present in measurements of the polarization of the cosmic microwave background
(CMB) at frequencies above 100GHz. We exploit the Planck HFI polarization data
from 100 to 353GHz to measure the dust angular power spectra $C_\ell^{EE,BB}$
over the range $40<\ell<600$ well away from the Galactic plane. These will
bring new insights into interstellar dust physics and a precise determination
of the level of contamination for CMB polarization experiments. We show that
statistical properties of the emission can be characterized over large
fractions of the sky using $C_\ell$. For the dust, they are well described by
power laws in $\ell$ with exponents $\alpha^{EE,BB}=-2.42\pm0.02$. The
amplitudes of the polarization $C_\ell$ vary with the average brightness in a
way similar to the intensity ones. The dust polarization frequency dependence
is consistent with modified blackbody emission with $\beta_d=1.59$ and
$T_d=19.6$K. We find a systematic ratio between the amplitudes of the Galactic
$B$- and $E$-modes of 0.5. We show that even in the faintest dust-emitting
regions there are no "clean" windows where primordial CMB $B$-mode polarization
could be measured without subtraction of dust emission. Finally, we investigate
the level of dust polarization in the BICEP2 experiment field. Extrapolation of
the Planck 353GHz data to 150GHz gives a dust power
$\ell(\ell+1)C_\ell^{BB}/(2\pi)$ of $1.32\times10^{-2}\mu$K$_{CMB}^2$ over the
$40<\ell<120$ range; the statistical uncertainty is $\pm0.29$ and there is an
additional uncertainty (+0.28,-0.24) from the extrapolation, both in the same
units. This is the same magnitude as reported by BICEP2 over this $\ell$ range,
which highlights the need for assessment of the polarized dust signal even in
the cleanest windows of the sky.Comment: 25 pages, 25 figures, accepted in A&
The production and decay of the top partner $T$ in the left-right twin
  higgs model at the ILC and CLIC

The left-right twin Higgs model (LRTHM) predicts the existence of the top
partner $T$. In this work, we make a systematic investigation for the single
and pair production of this top partner $T$ through the processes:
$e^{+}e^{-}\to t\ov{T} + T\bar{t}$ and $ T\ov{T}$, the neutral scalar (the
SM-like Higgs boson $h$ or neutral pseudoscalar boson $\phi^{0}$) associate
productions $e^{+}e^{-}\to t\ov{T}h +T\bar{t}h$, $T\ov{T}h$,
$t\ov{T}\phi^{0}+T\bar{t}\phi^{0}$ and $ T\ov{T}\phi^{0}$. From the numerical
evaluations for the production cross sections and relevant phenomenological
analysis we find that (a) the production rates of these processes, in the
reasonable parameter space, can reach the level of several or tens of fb; (b)
for some cases, the peak value of the resonance production cross section can be
enhanced significantly and reaches to the level of pb; (c) the subsequent decay
of $T\to \phi^{+}b \to t\bar{b}b$ may generate typical phenomenological
features rather different from the signals from other new physics models beyond
the standard model(SM); and (d) since the relevant SM background is generally
not large, some signals of the top partner $T$ predicted by the LRTHM may be
detectable in the future ILC and CLIC experiments.Comment: 20pages, 15 figures and 6 Tables. Minor corrections on text. new
  references adde
N=8 Nonlinear Supersymmetric Mechanics

We construct a new two-dimensional N=8 supersymmetric mechanics with
nonlinear chiral supermultiplet. Being intrinsically nonlinear this multiplet
describes 2 physical bosonic and 8 fermionic degrees of freedom. We construct
the most general superfield action of the sigma-model type and propose its
simplest extension by a Fayet-Iliopoulos term. The most interesting property of
the constructed system is a new type of geometry in the bosonic subsector,
which is different from the special Kahler one characterizing the case of the
linear chiral N=8 supermultiplet.Comment: 9 pages, no figures, minor correction
Spin-field Interaction Effects and Loop Dynamics in AdS/CFT Duality

The spin-field interaction is considered, in the context of the gauge
fields/string correspondence, in the large 't Hooft coupling limit. The latter
can be viewed as a WKB-type approximation to the AdS/CFT duality conjecture.
Basic theoretical objects entering the present study are (a) the Wilson loop
functional, on the gauge field side and (b) the sigma model action for the
string propagating in AdS$_5$. Spin effects are introduced in a worldline
setting, via the spin factor for a particle entity propagating on a Wilson loop
contour. The computational tools employed for conducting the relevant analysis,
follow the methodological guidelines introduced in two papers by Polyakov and
Rychkov. The main result is expressed in terms of the modification of the spin
factor brought about by dynamical effects, both perturbative and
non-perturbative, according to AdS/CFT in the considered limit.Comment: 21 page
Higher-level Appell functions, modular transformations, and characters.

We study modular transformation properties of a class of indefinite theta series involved in characters of infinite-dimensional Lie superalgebras. The level- Appell functions  satisfy open quasiperiodicity relations with additive theta-function terms emerging in translating by the period. Generalizing the well-known interpretation of theta functions as sections of line bundles, the  function enters the construction of a section of a rank-(+1) bundle . We evaluate modular transformations of the  functions and construct the action of an SL(2,) subgroup that leaves the section of  constructed from  invariant.\ud
Modular transformation properties of  are applied to the affine Lie superalgebra  at a rational level k>–1 and to the N=2 super-Virasoro algebra, to derive modular transformations of admissible characters, which are not periodic under the spectral flow and cannot therefore be rationally expressed through theta functions. This gives an example where constructing a modular group action involves extensions among representations in a nonrational conformal model
Quantifying three dimensional reconnection in fragmented current layers

There is growing evidence that when magnetic reconnection occurs in high
Lundquist number plasmas such as in the Solar Corona or the Earth's
Magnetosphere it does so within a fragmented, rather than a smooth current
layer. Within the extent of these fragmented current regions the associated
magnetic flux transfer and energy release occurs simultaneously in many
different places. This investigation focusses on how best to quantify the rate
at which reconnection occurs in such layers. An analytical theory is developed
which describes the manner in which new connections form within fragmented
current layers in the absence of magnetic nulls. It is shown that the
collective rate at which new connections form can be characterized by two
measures; a total rate which measures the true rate at which new connections
are formed and a net rate which measures the net change of connection
associated with the largest value of the integral of $E_{\|}$ through all of
the non-ideal regions. Two simple analytical models are presented which
demonstrate how each should be applied and what they quantify.Comment: 14 pages, 15 figures. Published in Physics of Plasma
Planck 2015 results. XIII. Cosmological parameters

We present results based on full-mission Planck observations of temperature
and polarization anisotropies of the CMB. These data are consistent with the
six-parameter inflationary LCDM cosmology. From the Planck temperature and
lensing data, for this cosmology we find a Hubble constant, H0= (67.8 +/- 0.9)
km/s/Mpc, a matter density parameter Omega_m = 0.308 +/- 0.012 and a scalar
spectral index with n_s = 0.968 +/- 0.006. (We quote 68% errors on measured
parameters and 95% limits on other parameters.) Combined with Planck
temperature and lensing data, Planck LFI polarization measurements lead to a
reionization optical depth of tau = 0.066 +/- 0.016. Combining Planck with
other astrophysical data we find N_ eff = 3.15 +/- 0.23 for the effective
number of relativistic degrees of freedom and the sum of neutrino masses is
constrained to < 0.23 eV. Spatial curvature is found to be |Omega_K| < 0.005.
For LCDM we find a limit on the tensor-to-scalar ratio of r <0.11 consistent
with the B-mode constraints from an analysis of BICEP2, Keck Array, and Planck
(BKP) data. Adding the BKP data leads to a tighter constraint of r < 0.09. We
find no evidence for isocurvature perturbations or cosmic defects. The equation
of state of dark energy is constrained to w = -1.006 +/- 0.045. Standard big
bang nucleosynthesis predictions for the Planck LCDM cosmology are in excellent
agreement with observations. We investigate annihilating dark matter and
deviations from standard recombination, finding no evidence for new physics.
The Planck results for base LCDM are in agreement with BAO data and with the
JLA SNe sample. However the amplitude of the fluctuations is found to be higher
than inferred from rich cluster counts and weak gravitational lensing. Apart
from these tensions, the base LCDM cosmology provides an excellent description
of the Planck CMB observations and many other astrophysical data sets.Comment: Abstract severely abridged. Revised to match version accepted by
  Astronomy & Astrophysics. Many minor changes, but basic results remain
  unchange
Evidence for non-exponential elastic proton-proton differential
  cross-section at low |t| and sqrt(s) = 8 TeV by TOTEM

The TOTEM experiment has made a precise measurement of the elastic
proton-proton differential cross-section at the centre-of-mass energy sqrt(s) =
8 TeV based on a high-statistics data sample obtained with the beta* = 90
optics. Both the statistical and systematic uncertainties remain below 1%,
except for the t-independent contribution from the overall normalisation. This
unprecedented precision allows to exclude a purely exponential differential
cross-section in the range of four-momentum transfer squared 0.027 < |t| < 0.2
GeV^2 with a significance greater than 7 sigma. Two extended parametrisations,
with quadratic and cubic polynomials in the exponent, are shown to be well
compatible with the data. Using them for the differential cross-section
extrapolation to t = 0, and further applying the optical theorem, yields total
cross-section estimates of (101.5 +- 2.1) mb and (101.9 +- 2.1) mb,
respectively, in agreement with previous TOTEM measurements.Comment: Final version published in Nuclear Physics
Uniform Atmospheric Retrieval Analysis of Ultracool Dwarfs I:
  Characterizing Benchmarks, Gl570D and HD3651B

Interpreting the spectra of brown dwarfs is key to determining the
fundamental physical and chemical processes occurring in their atmospheres.
Powerful Bayesian atmospheric retrieval tools have recently been applied to
both exoplanet and brown dwarf spectra to tease out the thermal structures and
molecular abundances to understand those processes. In this manuscript we
develop a significantly upgraded retrieval method and apply it to the SpeX
spectral library data of two benchmark late T-dwarfs, Gl570D and HD3651B, to
establish the validity of our upgraded forward model parameterization and
Bayesian estimator. Our retrieved metallicities, gravities, and effective
temperature are consistent with the metallicity and presumed ages of the
systems. We add the carbon-to-oxygen ratio as a new dimension to benchmark
systems and find good agreement between carbon-to-oxygens ratio derived in the
brown dwarfs and the host stars. Furthermore, we have for the first time
unambiguously determined the presence of ammonia in the low-resolution spectra
of these two late T-dwarfs. We also show that the retrieved results are not
significantly impacted by the possible presence of clouds, though some
quantities are significantly impacted by uncertainties in photometry. This
investigation represents a watershed study in establishing the utility of
atmospheric retrieval approaches on brown dwarf spectra.Comment: submitted to Apj, addressed first round of minor revision
Contributions to the width difference in the neutral $D$ system from
  hadronic decays

Recent studies of several multi-body $D^0$ meson decays have revealed that
the final states are dominantly $CP$-even. However, the small value of the
width difference between the two physical eigenstates of the
$D^0$-$\overline{D}{}^0$ system indicates that the total widths of decays to
$CP$-even and $CP$-odd final states should be the same to within about a
percent. The known contributions to the width difference from hadronic $D^0$
decays are discussed, and it is shown that an apparent excess of
quasi-$CP$-even modes is balanced, within current uncertainty, by interference
effects in quasi-flavour-specific decays. Decay modes which may significantly
affect the picture with improved measurements are considered.Comment: 17 pages including 3 tables. v2: Updated with published version
  including new comments in summar
A possible link between the power spectrum of interstellar filaments and
  the origin of the prestellar core mass function

Two major features of the prestellar CMF are: 1) a broad peak below 1 Msun,
presumably corresponding to a mean gravitational fragmentation scale, and 2) a
characteristic power-law slope, very similar to the Salpeter slope of the
stellar initial mass function (IMF) at the high-mass end. While recent Herschel
observations have shown that the peak of the prestellar CMF is close to the
thermal Jeans mass in marginally supercritical filaments, the origin of the
power-law tail of the CMF/IMF at the high-mass end is less clear. Inutsuka
(2001) proposed a theoretical scenario in which the origin of the power-law
tail can be understood as resulting from the growth of an initial spectrum of
density perturbations seeded along the long axis of filaments by interstellar
turbulence. Here, we report the statistical properties of the line-mass
fluctuations of filaments in nearby molecular clouds observed with Herschel
using a 1-D power spectrum analysis. The observed filament power spectra were
fitted by a power-law function $(P_{true}(s) \propto s^{\alpha})$ after
removing the effect of beam convolution at small scales. A Gaussian-like
distribution of power-spectrum slopes was found centered at -1.6, close to that
of the one-dimensional velocity power spectrum generated by subsonic
Kolomogorov turbulence (-1.67). An empirical correlation, $P^{0.5}(s_0) \propto
<N_{\rm H_2}>^{1.4 \pm 0.1} $, was also found between the amplitude of each
filament power spectrum $P(s_0)$ and the mean column density along the filament
$<N_{\rm H_2}>$. Finally, the dispersion of line-mass fluctuations along each
filament $\sigma_{\rm M_{line}}$ was found to scale with the physical length
$L$ of the filament, roughly as $\sigma_{M_{line}} \propto L^{0.7}$. Overall,
our results are consistent with the suggestion that the bulk of the CMF/IMF
results from the gravitational fragmentation of filaments.Comment: 10 pages, 12 figures, Accepted for publication in Astronomy and
  Astrophysics journa
Luminescence dating of glacial advances at Lago Buenos Aires (?46 ?S), Patagonia

Understanding the timing of past glacial advances in Patagonia is of global climatic importance because of the insight this can provide into the influence on glacier behaviour of changes in temperature and precipitation related to the Southern Westerlies. In this paper we present new luminescence ages determined using single grains of K-feldspar from proglacial outwash sediments that were deposited by the Patagonian Ice Sheet around Lago Buenos Aires (?46 ?S), east of the contemporary Northern Patagonian Icefield. The new luminescence ages indicate that major outwash accumulations formed around ?110 ? 20 ka to 140 ? 20 ka and that these correspond to the Moreno I and II moraine ridges, which were previously dated using cosmogenic isotope dating to 150 ? 30 ka. Luminescence dating at Lago Buenos Aires has also identified outwash sediments that were deposited during glacial advances ?30.8 ? 5.7 ka and ?34.0 ? 6.1 ka (MIS 3) that are not recorded in the moraine record. Younger outwash accumulations were then deposited between ?14.7 ? 2.1 and 26.2 ? 1.6 ka which correspond to the Fenix I ? V moraine ridges. The combined chronology suggests that glacial advances occurred ?110 ? 20 ka to 150 ? 30 ka (MIS 6), ?30.8 ? 5.7 ka to ?34.0 ? 6.1 ka (MIS 3), and ?14.7 ? 2.1 to 26.2 ? 1.6 ka (MIS 2) at Lago Buenos Aires. Overall luminescence dating using single grains of K-feldspar has excellent potential to contribute towards the ever-increasing geochronological dataset constraining the timings of glacial advances in Patagonia.publishersversionPeer reviewe