pinecone/core-2020-05-10-deduplication huggingface dataset:
Universal Bethe ansatz solution for the Temperley-Lieb spin chain

We consider the Temperley-Lieb (TL) open quantum spin chain with "free"
boundary conditions associated with the spin-$s$ representation of
quantum-deformed $sl(2)$. We construct the transfer matrix, and determine its
eigenvalues and the corresponding Bethe equations using analytical Bethe
ansatz. We show that the transfer matrix has quantum group symmetry, and we
propose explicit formulas for the number of solutions of the Bethe equations
and the degeneracies of the transfer-matrix eigenvalues. We propose an
algebraic Bethe ansatz construction of the off-shell Bethe states, and we
conjecture that the on-shell Bethe states are highest-weight states of the
quantum group. We also propose a determinant formula for the scalar product
between an off-shell Bethe state and its on-shell dual, as well as for the
square of the norm. We find that all of these results, except for the
degeneracies and a constant factor in the scalar product, are universal in the
sense that they do not depend on the value of the spin. In an appendix, we
briefly consider the closed TL spin chain with periodic boundary conditions,
and show how a previously-proposed solution can be improved so as to obtain the
complete (albeit non-universal) spectrum.Comment: v2: 21 pages; minor revisions, references added, publishe
Deep observation of the NGC 1275 region with MAGIC: search of diffuse
  gamma-ray emission from cosmic rays in the Perseus cluster

Clusters of galaxies are expected to be reservoirs of cosmic rays (CRs) that
should produce diffuse gamma-ray emission due to their hadronic interactions
with the intra-cluster medium. The nearby Perseus cool-core cluster, identified
as the most promising target to search for such an emission, has been observed
with the MAGIC telescopes at very-high energies (VHE, E>100 GeV) for a total of
253 hr from 2009 to 2014. The active nuclei of NGC 1275, the central dominant
galaxy of the cluster, and IC 310, lying at about 0.6$^\circ$ from the centre,
have been detected as point-like VHE gamma-ray emitters during the first phase
of this campaign. We report an updated measurement of the NGC 1275 spectrum,
which is well described by a power law with a photon index of
$3.6\pm0.2_{stat}\pm0.2_{syst}$ between 90 GeV and 1.2 TeV. We do not detect
any diffuse gamma-ray emission from the cluster and set stringent constraints
on its CR population. In order to bracket the uncertainties over the CR spatial
and spectral distributions, we adopt different spatial templates and power-law
spectral indexes $\alpha$. For $\alpha=2.2$, the CR-to-thermal pressure within
the cluster virial radius is constrained to be below 1-2%, except if CRs can
propagate out of the cluster core, generating a flatter radial distribution and
releasing the CR-to-thermal pressure constraint to <20%. Assuming that the
observed radio mini-halo of Perseus is generated by secondary electrons from CR
hadronic interactions, we can derive lower limits on the central magnetic
field, $B_0$, that depend on the CR distribution. For $\alpha=2.2$,
$B_0\gtrsim5-8 \mu$G, which is below the 25 $\mu$G inferred from Faraday
rotation measurements, whereas, for $\alpha\lesssim2.1$, the hadronic
interpretation of the diffuse radio emission is in contrast with our gamma-ray
flux upper limits independently of the magnetic field strength.Comment: 13 pages, 8 figures, accepted for publication in Section 3. Cosmology
  (including clusters of galaxies) of Astronomy and Astrophysics. Corresponding
  authors: P. Colin (colin@mppmu.mpg.de) and F. Zandanel (f.zandanel@uva.nl
A $\gamma\gamma$ Collider for the 750 GeV Resonant State

Recent data collected by ATLAS and CMS at 13 TeV collision energy of the LHC
indicate the existence of a new resonant state $\phi$ with a mass of 750 GeV
decaying into two photons $\gamma\gamma$. The properties of $\phi$ should be
studied further at the LHC and also future colliders. Since only $\phi \to
\gamma\gamma$ decay channel has been measured, one of the best ways to extract
more information about $\phi$ is to use a $\gamma\gamma$ collider to produce
$\phi$ at the resonant energy. In this work we show how a $\gamma\gamma$
collider helps to verify the existence of $\phi$ and to provide some of the
most important information about the properties of $\phi$, such as branching
fractions of $\phi\to V_1V_2$. Here $V_i$ can be $\gamma$, $Z$, or $W^\pm$. We
also show that by studying angular distributions of the final $\gamma$'s in
$\gamma\gamma \to \phi \to \gamma\gamma$, one can obtain crucial information
about whether this state is a spin-0 or a spin-2 state.Comment: ReTex, 12 page with 6 figures. Expanded discussion on distinguishing
  spin-0 and spin-2 cases. Several figures adde
Erupting filaments with large enclosing flux tubes as sources of
  high-mass 3-part CMEs, and erupting filaments in the absence of enclosing
  flux tubes as sources of low-mass unstructured CMEs

The 3-part appearance of many CMEs arising from erupting filaments emerges
from a large magnetic flux tube structure, consistent with the form of the
erupting filament system. Other CMEs arising from erupting filaments lack a
clear 3-part structure and reasons for this have not been researched in detail.
This paper aims to further establish the link between CME structure and the
structure of the erupting filament system and to investigate whether CMEs which
lack a 3-part structure have different eruption characteristics. A survey is
made of 221 near-limb filament eruptions observed from 2013/05/03-2014/06/30 by
EUV imagers and coronagraphs. 92 filament eruptions are associated with 3-part
structured CMEs, 41 eruptions are associated with unstructured CMEs. The
remaining 88 are categorized as failed eruptions. For 34% of the 3-part CMEs,
processing applied to EUV images reveals the erupting front edge is a
pre-existing loop structure surrounding the filament, which subsequently erupts
with the filament to form the leading bright front edge of the CME. This
connection is confirmed by a flux-rope density model. Furthermore, the
unstructured CMEs have a narrower distribution of mass compared to structured
CMEs, with total mass comparable to the mass of 3-part CME cores. This study
supports the interpretation of 3-part CME leading fronts as the outer
boundaries of a large pre-existing flux tube. Unstructured (non 3-part) CMEs
are a different family to structured CMEs, arising from the eruption of
filaments which are compact flux tubes in the absence of a large system of
enclosing closed field
Computing solutions for matching games

A  matching  game  is  a  cooperative  game  (\ud
N; v\ud
)  de�ned  on\ud
a graph\ud
G\ud
= (\ud
N; E\ud
) with an edge weighting\ud
w\ud
:\ud
E\ud
!\ud
R\ud
+\ud
. The player\ud
set is\ud
N\ud
and the value of a coalition\ud
S\ud
�\ud
N\ud
is de�ned as the maximum\ud
weight of a matching in the subgraph induced by\ud
S\ud
. First we present an\ud
O\ud
(\ud
nm\ud
+\ud
n\ud
2\ud
log\ud
n\ud
) algorithm that tests if the core of a matching game de-\ud
�ned on a weighted graph with\ud
n\ud
vertices and\ud
m\ud
edges is nonempty and\ud
that computes a core member if the core is nonempty. This algorithm im-\ud
proves previous work based on the ellipsoid method and can also be used\ud
to compute stable solutions for instances of the stable roommates prob-\ud
lem with payments. Second we show that the nucleolus of an\ud
n\ud
-player\ud
matching game with a nonempty core can be computed in\ud
O\ud
(\ud
n\ud
4\ud
) time.\ud
This generalizes the corresponding result of Solymosi and Raghavan for\ud
assignment games. Third we prove that is\ud
NP\ud
-hard to determine an impu-\ud
tation with minimum number of blocking pairs, even for matching games\ud
with unit edge weights, whereas the problem of determining an imputa-\ud
tion with minimum total blocking value is shown to be polynomial-time\ud
solvable for general matching games
Dynamics of isolated-photon plus jet production in pp collisions at root s=7 TeV with the ATLAS detector

The dynamics of isolated-photon plus jet production in pp collisions at a centre-of-mass energy of 7 TeV has been studied with the ATLAS detector at the LHC using an integrated luminosity of 37 pb(-1). Measurements of isolated-photon plus jet bin-averaged cross sections are presented as functions of photon transverse energy, jet transverse momentum and jet rapidity. In addition, the bin-averaged cross sections as functions of the difference between the azimuthal angles of the photon and the jet, the photon jet invariant mass and the scattering angle in the photon jet centre-of-mass frame have been measured. Next-to-leading-order QCD calculations are compared to the measurements and provide a good description of the data, except for the case of the azimuthal opening angle
Search for squarks and gluinos using final states with jets and missing transverse momentum with the ATLAS detector in root s=7 TeV proton-proton collisions

A search for squarks and gluinos in events containing jets, missing transverse momentum and no electrons or muons is presented. The data were recorded in 2011 by the ATLAS experiment in root s = 7 TeV proton-proton collisions at the Large Hadron Collider. No excess above the Standard Model background expectation is observed in 1.04 fb(-1) of data. Gluino and squark masses below 700 GeV and 875 GeV respectively are excluded at the 95% confidence level in simplified models containing only squarks of the first two generations, a gluino octet and a massless neutralino. The exclusion limit increases to 1075 GeV for squarks and gluinos of equal mass. In MSUGRA/CMSSM models with tan beta = 10, A(0) = 0 and mu > 0, squarks and gluinos of equal mass are excluded for masses below 950 GeV. These limits extend the region of supersymmetric parameter space excluded by previous measurements
Spiral-driven accretion in protoplanetary discs
 : 
I. 2D models

The  computations  presented  here  were  performed  using  the  Froggy  platform  of  the  CIMENT  infrastructure  (https://ciment.ujf-grenoble.fr)International audienceWe numerically investigate the dynamics of a 2D non-magnetised protoplanetary disc surrounded by an inflow coming from an external envelope. We find that the accretion shock between the disc and the inflow is unstable, leading to the generation of large-amplitude spiral density waves. These spiral waves propagate over long distances, down to radii at least ten times smaller than the accretion shock radius. We measure spiral-driven outward angular momentum transport with 10-4 ≲ α < 10-2 for an inflow accretion rate Ṁinf ≳ 10-8 M⊙ yr-1. We conclude that the interaction of the disc with its envelope leads to long-lived spiral density waves and radial angular momentum transport with rates that cannot be neglected in young non-magnetised protostellar discs
The remarkable solar twin HIP 56948: a prime target in the quest for
  other Earths

We study HIP 56948, the best solar twin known to date, to determine with an
unparalleled precision how similar is to the Sun in its physical properties,
chemical composition and planet architecture. We explore whether the abundances
anomalies may be due to pollution from stellar ejecta or to terrestrial planet
formation.
  We perform a differential abundance analysis (both in LTE and NLTE) using
high resolution (R = 100,000) high S/N (600) Keck HIRES spectra of the Sun and
HIP 56948. We use precise radial velocity data from the McDonald and Keck
observatories to search for planets around this star.
  We achieve a precision of sigma = 0.003 dex for several elements. Including
errors in stellar parameters the total uncertainty is as low as sigma = 0.005
dex (1 %), which is unprecedented in elemental abundance studies.
  The similarities between HIP 56948 and the Sun are astonishing. HIP 56948 is
only 17+/-7 K hotter than the Sun, and log g, [Fe/H] and microturbulence are
only +0.02+/-0.02 dex, +0.02+/-0.01 dex and +0.01+/-0.01 km/s higher than
solar, respectively. HIP 56948 has a mass of 1.02+/-0.02M_Sun and is 1 Gyr
younger than the Sun. Both stars show a chemical abundance pattern that differs
from most solar twins. The trend with T_cond in differential abundances (twins
- HIP56948) can be reproduced very well by adding 3 M_Earth of a mix of Earth
and meteoritic material, to the convection zone of HIP 56948. From our radial
velocity monitoring we find no indications of giant planets interior to or
within the habitable zone of HIP 56948.
  We conclude that HIP 56948 is an excellent candidate to host a planetary
system like our own, including the possible presence of inner terrestrial
planets. Its striking similarity to the Sun and its mature age makes HIP 56948
a prime target in the quest for other Earths and SETI endeavors.Comment: A & A, in pres
A Lattice Boltzmann - Immersed Boundary method to simulate the fluid interaction with moving and slender flexible objects

International audienceA numerical approach based on the Lattice Boltzmann and Immersed Boundary methods is pro- posed to tackle the problem of the interaction of moving and/or deformable slender solids with an incompressible fluid flow. The method makes use of a Cartesian uniform lattice that encom- passes both the fluid and the solid domains. The deforming/moving elements are tracked through a series of Lagrangian markers that are embedded in the computational domain. Differently from classical projection methods applied to advance in time the incompressible Navier-Stokes equa- tions, the baseline Lattice Boltzmann fluid solver is free from pressure corrector step, which is known to affect the accuracy of the boundary conditions. Also, in contrast to other immersed boundary methods proposed in the literature, the proposed algorithm does not require the in- troduction of any empirical parameter. In the case of rigid bodies, the position of the markers delimiting the surface of an object is updated by tracking both the position of the center of mass of the object and its rotation using Newton's Laws and the conservation of angular momentum. The dynamics of a flexible slender structure is determined as a function of the forces exerted by the fluid, its flexural rigidity and the tension necessary to enforce the filament inextensibility. For both rigid and deformable bodies, the instantaneous no-slip and impermeability conditions on the solid boundary are imposed via external and localized body forces which are consistently introduced into the Lattice Boltzmann equation. The validation test-cases for rigid bodies in- clude the case of an impulsively started plate and the sedimentation of particles under gravity in a fluid initially at rest. For the case of deformable slender structures we consider the beating of both a single filament and a pair filaments induced by the interaction with an incoming uniformly streaming flow
Rotation and magnetism of Kepler pulsating solar-like stars
 : 
Towards asteroseismically calibrated age-rotation relations

International audienceKepler ultra-high precision photometry of long and continuous observations provides a unique dataset in which surface rotation and variability can be studied for thousands of stars. Because many of these old field stars also have independently measured asteroseismic ages, measurements of rotation and activity are particularly interesting in the context of age-rotation-activity relations. In particular, age-rotation relations generally lack good calibrators at old ages, a problem that this Kepler sample of old-field stars is uniquely suited to address. We study the surface rotation and photometric magnetic activity of a subset of 540 solar-like stars on the main-sequence and the subgiant branch for which stellar pulsations have been measured. The rotation period was determined by comparing the results from two different analysis methods: i) the projection onto the frequency domain of the time-period analysis, and ii) the autocorrelation function of the light curves. Reliable surface rotation rates were then extracted by comparing the results from two different sets of calibrated data and from the two complementary analyses. General photometric levels of magnetic activity in this sample of stars were also extracted by using a photometric activity index, which takes into account the rotation period of the stars. We report rotation periods for 310 out of 540 targets (excluding known binaries and candidate planet-host stars); our measurements span a range of 1 to 100 days. The photometric magnetic activity levels of these stars were computed, and for 61.5% of the dwarfs, this level is similar to the range, from minimum to maximum, of the solar magnetic activity. We demonstrate that hot dwarfs, cool dwarfs, and subgiants have very different rotation-age relationships, highlighting the importance of separating out distinct populations when interpreting stellar rotation periods. Our sample of cool dwarf stars with age and metallicity data of the highest quality is consistent with gyrochronology relations reported in the literature
Fractal dimension computation from equal mass partitions.

International audienceNumerical methods which utilize partitions of equal-size, including the box-counting method, remain the most popular choice for computing the generalized dimension of multifractal sets. However, it is known that mass-oriented methods generate relatively good results for computing generalized dimensions for important cases where the box-counting method is known to fail. Here, we revisit two mass-oriented methods and discuss their strengths and limitations. V C 2014 AIP Publishing LLC. [http://dx.doi.org/10.1063/1.4885778] Fractal sets are characterized by self-similarity, and power laws can be associated with them. Examples of fractals in nature are ubiquitous. Their discovery led to the extension of the notion of dimension. For monofrac-tals, the scaling pattern is homogeneous and the set can be characterized by a single dimension. In contrast, mul-tifractals are inhomogeneous and require a spectrum of dimensions D q to capture their geometry. In finding the generalized dimensions, the box-counting method has been by far the most popular choice among researchers across various fields. However, it is known that the class of methods which deal with partitions into cells of equal size, including the box-counting method, is ill-suited for computing the generalized dimensions on some domain of q. In this paper, two alternative methods which utilize mass-oriented partitions, rather than partitions of equal-size, are investigated
On isometric full embeddings of symplectic dual polar spaces into Hermitian dual polar spaces.

Let  \geq 2$, let ,K'$ be fields such that '$ is a quadratic Galois-extension of $ and let $\theta$ denote the unique nontrivial element in (K'/K)$. Suppose the symplectic dual polar space (2n-1,K)$ is fully and isometrically embedded into the Hermitian dual polar space (2n-1,K',\theta)$. We prove that the projective embedding
of (2n-1,K)$ induced by the Grassmann-embedding of (2n-1,K',\theta)$ is isomorphic to the Grassmann-embedding of (2n-1,K)$. We also prove that if $ is even, then the set of points of (2n-1,K',\theta)$ at distance at most $\frac{n}{2}-1$ from (2n-1,K)$ is a hyperplane of (2n-1,K',\theta)$ which arises from the Grassmann-embedding of (2n-1,K',\theta)$
Measurement of the relative width difference of the B0-B¯¯¯¯0 system with the ATLAS detector

This paper presents the measurement of the relative width difference ΔΓd/Γd of the B0-B¯¯¯¯0 system using the data collected by the ATLAS experiment at the LHC in pp collisions at s√=7 TeV and s√=8 TeV and corresponding to an integrated luminosity of 25.2 fb−1. The value of ΔΓd/Γd is obtained by comparing the decay-time distributions of B0 → J/ψKS and B0 → J/ψK*0(892) decays. The result is ΔΓd/Γd = (−0.1±1.1 (stat.)± 0.9 (syst.)) × 10−2. Currently, this is the most precise single measurement of ΔΓd/Γd. It agrees with the Standard Model prediction and the measurements by other experiments
Combined search for the Standard Model Higgs boson using up to 4.9 fb-1 of pp collision data at √s =7TeV with the ATLAS detector at the LHC

Artículo escrito por muchos autores, sólo se referencian el que aparece en primer lugar, el nombre del grupo de colaboración y los autores que firman como pertenecientes a la UAMA combined search for the Standard Model Higgs boson with the ATLAS experiment at the LHC using datasets corresponding to integrated luminosities from 1.04 fb−1 to 4.9 fb−1 of pp collisions collected at √s=7 TeV is presented. The Higgs boson mass ranges 112.9–115.5 GeV, 131–238 GeV and 251–466 GeV are excluded at the 95% confidence level (CL), while the range 124–519 GeV is expected to be excluded in the absence of a signal. An excess of events is observed around mH∼126 with a local significance of 3.5 standard deviations (σ ). The local significances of H→γγ, H→ZZ(*)→ℓ+ℓ−ℓ′+ℓ′− and H→WW(*)→ℓ+νℓ′−ν¯, the three most sensitive channels in this mass range, are 2.8σ, 2.1σ and 1.4σ , respectively. The global probability for the background to produce such a fluctuation anywhere in the explored Higgs boson mass range 110–600 GeV is estimated to be ∼1.4% or, equivalently, 2.2σWe acknowledge the support of ANPCyT, Argentina; YerPhI, Armenia; ARC, Australia; BMWF, Austria; ANAS, Azerbaijan; SSTC, Belarus; CNPq and FAPESP, Brazil; NSERC, NRC and CFI, Canada; CERN; CONICYT, Chile; CAS, MOST and NSFC, China; COLCIENCIAS, Colombia; MSMT CR, MPO CR and VSC CR, Czech Republic; DNRF, DNSRC and Lundbeck Foundation, Denmark; ARTEMIS and ERC, European Union; IN2P3–CNRS, CEA-DSM/IRFU, France; GNAS, Georgia; BMBF, DFG, HGF, MPG and AvH Foundation, Germany; GSRT, Greece; ISF, MINERVA, GIF, DIP and Benoziyo Center, Israel; INFN, Italy; MEXT and JSPS, Japan; CNRST, Morocco; FOM and NWO, Netherlands; RCN, Norway; MNiSW, Poland; GRICES and FCT, Portugal; MERYS (MECTS), Romania; MES of Russia and ROSATOM, Russian Federation; JINR; MSTD, Serbia; MSSR, Slovakia; ARRS and MVZT, Slovenia; DST/NRF, South Africa; MICINN, Spain; SRC and Wallenberg Foundation, Sweden; SER, SNSF and Cantons of Bern and Geneva, Switzerland; NSC, Taiwan; TAEK, Turkey; STFC, the Royal Society and Leverhulme Trust, United Kingdom; DOE and NSF, United States of America. The crucial computing support from all WLCG partners is acknowledged gratefully, in particular from CERN and the ATLAS Tier-1 facilities at TRIUMF (Canada), NDGF (Denmark, Norway,
Sweden), CC-IN2P3 (France), KIT/GridKA (Germany), INFN-CNAF (Italy), NL-T1 (Netherlands), PIC (Spain), ASGC (Taiwan), RAL (UK) and BNL (USA) and in the Tier-2 facilities worldwid
Designed folding of pseudopeptides: the transformation of a configurationally driven preorganization into a stereoselective multicomponent macrocyclization

The efficient synthesis of large-ring pseudopeptidic macrocycles through a multicomponent [2+2] reductive amination reaction is described. The reaction was entirely governed by the structural information contained in the corresponding open-chain pseudopeptidic bis(amidoamine) precursors, which have a rigid (R,R)-cyclohexane-1,2-diamine moiety. A remarkable match/mismatch relationship between the configurations of the chiral centers of the cyclic diamine and those of the peptidic frame was observed. The macrocyclic tetraimine intermediates have been studied in detail by NMR spectroscopy, circular dichroism (CD), and molecular modeling, and the results support the appropriate preorganization induced by the match combination of the chiral centers. We have also synthesized the corresponding open-chain bis(imine) model compounds. The structural studies (NMR spectroscopy, CD, modeling) of these systems showed an intrinsically lower reactivity of the mismatch combination, even when the product of the reaction was acyclic. In addition, a synergistic effect between the two chiral substructures for the correct folding of the molecules was observed. Finally, X-ray analysis of the HCl salt of one of the macrocycles showed an interesting pattern; the macrocyclic rings stack in columnar aggregates leaving large interstitial channels filled with water-solvated chloride anion