pinecone/core-2020-05-10-deduplication huggingface dataset:
Topological expansion of the β-ensemble model and quantum algebraic geometry in the sectorwise approach

International audienceWe construct the solution of the loop equations of the β-ensemble model in a form analogous to the solution in the case of the Hermitian matrices β = 1. The solution for β = 1 is expressed in terms of the algebraic spectral curve given by y2 = U(x). The spectral curve for arbitrary β converts into the Schrödinger equation (ħ∂)2 − U(x) ψ(x) = 0, where ħ ∝ (β√−1/β√)/N . The basic ingredients of the method based on the algebraic solution retain their meaning, but we use an alternative approach to construct a solution of the loop equations in which the resolvents are given separately in each sector. Although this approach turns out to be more involved technically, it allows consistently defining the B-cycle structure for constructing the quantum algebraic curve (a D-module of the form y2 − U(x), where [y, x] = ħ) and explicitly writing the correlation functions and the corresponding symplectic invariants Fh or the terms of the free energy in an 1/N2-expansion at arbitrary ħ. The set of "flat" coordinates includes the potential times tk and the occupation numbers ε˜α . We define and investigate the properties of the A- and B-cycles, forms of the first, second, and third kinds, and the Riemann bilinear identities. These identities allow finding the singular part of F0 , which depends only on ε˜α
Women, Weather, and Woes: The Triangular Dynamics of Female-Headed Households, Economic Vulnerability, and Climate Variability in South Africa

Existing gender inequality is believed to be heightened as a result of weather events and climate-related disasters that are likely to become more common in the future. We show that an already marginalized group—female-headed households in South Africa—is differentially affected by relatively modest levels of variation in rainfall, which households experience on a year-to-year basis. Data from three waves of the National Income Dynamics Survey in South Africa allow us to follow incomes of 4,162 households from 2006 to 2012. By observing how household income is affected by variation in rainfall relative to what is normally experienced during the rainy season in each district, our study employs a series of naturally occurring experiments that allow us to identify causal effects. We find that households where a single head can be identified based on residency or work status are more vulnerable to climate variability than households headed by two adults. Single male-headed households are more vulnerable because of lower initial earnings and, to a lesser extent, other household characteristics that contribute to economic disadvantages. However, this can only explain some of the differential vulnerability of female-headed households. This suggests that there are traits specific to female-headed households, such as limited access to protective social networks or other coping strategies, which makes this an important dimension of marginalization to consider for further research and policy in South Africa and other national contexts. Households headed by widows, never-married women, and women with a non-resident spouse (e.g., “left-behind” migrant households) are particularly vulnerable. We find vulnerable households only in districts where rainfall has a large effect on agricultural yields, and female-headed households remain vulnerable when accounting for dynamic impacts of rainfall on income
Identifying genetic risk variants for coronary heart disease in familial hypercholesterolemia: an extreme genetics approach

Mutations in the low-density lipoprotein receptor (LDLR) gene cause familial hypercholesterolemia (FH), a disorder characterized by coronary heart disease (CHD) at young age. We aimed to apply an extreme sampling method to enhance the statistical power to identify novel genetic risk variants for CHD in individuals with FH. We selected cases and controls with an extreme contrast in CHD risk from 17 000 FH patients from the Netherlands, whose functional LDLR mutation was unequivocally established. The genome-wide association (GWA) study was performed on 249 very young FH cases with CHD and 217 old FH controls without CHD (above 65 years for males and 70 years of age for females) using the Illumina HumanHap550K chip. In the next stage, two independent samples (one from the Netherlands and one from Italy, Norway, Spain, and the United Kingdom) of FH patients were used as replication samples. In the initial GWA analysis, we identified 29 independent single nucleotide polymorphisms (SNPs) with suggestive associations with premature CHD (P<1 × 10-4). We examined the association of these SNPs with CHD risk in the replication samples. After Bonferroni correction, none of the SNPs either replicated or reached genome-wide significance after combining the discovery and replication samples. Therefore, we conclude that the genetics of CHD risk in FH is complex and even applying an 'extreme genetics' approach we did not identify new genetic risk variants. Most likely, this method is not as effective in leveraging effect size as anticipated, and may, therefore, not lead to significant gains in statistical power
The Herschel Virgo Cluster survey, XIX : physical properties of low luminosity FIR sources at z < 0.5

Context. The star formation rate is a crucial parameter for the investigation galaxy evolution. At low redshift the cosmic star formation rate density declines smoothly, and massive active galaxies become passive, reducing their star formation activity. This implies that the bulk of the star formation rate density at low redshift is mainly driven by low mass objects. 
Aims. We investigate the properties of a sample of low luminosity far-infrared sources selected at 250 mu m. We have collected data from ultraviolet to far-infrared in order to perform a multiwavelengths analysis. The main goal is to investigate the correlation between star formation rate, stellar mass, and dust mass for a galaxy population with a wide range in dust content and stellar mass, including the low mass regime that most probably dominates the star formation rate density at low redshift. 
Methods. We define a main sample of similar to 800 sources with full spectral energy distribution coverage between 0 : 15 < lambda < 500 mu m and an extended sample with similar to 5000 sources in which we remove the constraints on the ultraviolet and near-infrared bands. We analyze both samples with two different spectral energy distribution fitting methods: MAGPHYS and CIGALE, which interpret a galaxy spectral energy distribution as a combination of different simple stellar population libraries and dust emission templates. 
Results. In the star formation rate versus stellar mass plane our samples occupy a region included between local spirals and higher redshift star forming galaxies. These galaxies represent the population that at z < 0.5 quenches their star formation activity and reduces their contribution to the cosmic star formation rate density. The subsample of galaxies with the higher masses (M-* > 3 x 10(10) M-circle dot) do not lie on the main sequence, but show a small off set as a consequence of the decreased star formation. Low mass galaxies (M-* < 1 x 10(10) M-circle dot) settle in the main sequence with star formation rate and stellar mass consistent with local spirals. 
Conclusions. Deep Herschel data allow the identification of a mixed galaxy population with galaxies still in an assembly phase or galaxies at the beginning of their passive evolution. We find that the dust luminosity is the parameter that allow us to discriminate between these two galaxy populations. The median spectral energy distribution shows that even at low star formation rate our galaxy sample has a higher mid-infrared emission than previously predicted
Measurement of the tt production cross section in the all-jet  final state in pp collisions at √s = 7 TeV

Journal of High Energy Physics 2013.5 (2013): 065 reproduced by permission of Scuola Internazionale Superiore di Studi Avanzati (SISSA)Artículo escrito por un elevado número de autores, solo se referencian el que aparece en primer lugar, el nombre del grupo de colaboración, si le hubiere, y los autores pertenecientes a la UAMA measurement is presented of the tt production cross section (σtt) in protonproton
collisions at a centre-of-mass energy of 7TeV, in the all-jet final state that contains
at least six jets, two of which are tagged as originating from b quarks. The data correspond to an integrated luminosity of 3.54 fb-1, collected with the CMS detector at the LHC. The cross section is determined through an unbinned maximum likelihood fit of background and tt signal to the reconstructed mass spectrum of tt candidates in the data, in which events are subjected to a kinematic fit assuming a tt → W+bW-b → 6 jets hypothesis. The measurement yields σtt = 139±10 (stat.)±26 (syst.)±3 (lum.) pb, a result consistent with those obtained in other tt decay channels, as well as with predictions of the standard mode
Structural, EPR, optical and Raman studies of Nd 2O 3:Cu 2+ nanophosphors

Nanocrystalline Nd2O3:Cu2+ (2 mol %) phosphors have been prepared by a low temperature solution combustion technique. Powder X-ray diffraction (PXRD) results confirm that hexagonal A-type Nd2O3 (900 °C, 3 h) and the lattice parameters have been evaluated by Rietveld refinement. Surface morphology of as-formed and Cu2+ doped Nd2O3 phosphors show that the particles are irregular in shape and porous in nature. TEM results also confirm the nature and size of the particles. The EPR spectrum exhibits two resonance signals with effective g values at gǀǀ ≈ 2.12 and g⊥ ≈ 2.04. The g values indicate that the site symmetry of Cu2+ ions is octahedral symmetry with elongated tetragonal distortion. Raman studies show major peaks, which are assigned, to Fg and combination of Ag + Eg modes. It is observed that the Raman peaks and intensity have been reduced in Cu2+ doped samples. UV–Visible absorption spectra exhibit a strong and broad absorption band at ∼240 nm. Further, the absorption peak shifts to ∼14 nm in Cu2+ doped samples. The optical band gap is estimated to be 5.28 eV for Cu doped Nd2O3 nanoparticles which are higher than the bulk Nd2O3 (4.7 eV). This can be attributed to the quantum confinement effect of the nanoparticles
Effect of Coriolis force on thermomagnetic convection in a ferrofluid saturating porous medium: A weakly nonlinear stability analysis

We investigate the influence of Coriolis force on the onset of thermomagnetic convection in ferrofluid saturating a porous layer in the presence of a uniform vertical magnetic field using both linear and weakly non-linear analyses. The modified Brinkman-Forchheimer-extended Darcy equation with Coriolis term has been used to describe the fluid flow. The linear theory based on normal mode method is considered to find the criteria for the onset of stationary thermomagnetic Convection and weakly non-linear analysis based on minimal representation of truncated Fourier series analysis containing only two terms has been used to find the Nusselt number Nu as functions of time. The range of thermal Rayleigh number R beyond which the bifurcation becomes subcritical increases with increasing A, Da(-1) and Ta. The global quantity of the heat transfer rate decreases by increasing the Taylor number Ta. The results obtained, during the above analyses, have been presented graphically and the effects of various parameters on heat and mass transfer have been discussed. Finally, we have drawn the steady streamlines for various parameters. (C) 2014 Elsevier B.V. All rights reserve
Floquet theory of radical pairs in radiofrequency magnetic fields

We present a new method for calculating the product yield of a radical pair
recombination reaction in the presence of a weak time-dependent magnetic field.
This method successfully circumvents the computational difficulties presented
by a direct solution of the Liouville-von Neumann equation for a long-lived
radical pair containing many hyperfine-coupled nuclear spins. Using a modified
formulation of Floquet theory, treating the time-dependent magnetic field as a
perturbation, and exploiting the slow radical pair recombination, we show that
one can obtain a good approximation to the product yield by considering only
nearly-degenerate sub-spaces of the Floquet space. Within a significant
parameter range, the resulting method is found to give product yields in good
agreement with exact quantum mechanical results for a variety of simple model
radical pairs. Moreover it is considerably more efficient than the exact
calculation, and it can be applied to radical pairs containing significantly
more nuclear spins. This promises to open the door to realistic theoretical
investigations of the effect of radiofrequency electromagnetic radiation on the
photochemically induced radical pair recombination reactions in the avian
retina which are believed to be responsible for the magnetic compass sense of
migratory birds.Comment: 11 pages, 7 figure
Characterizing the gamma-ray long-term variability of PKS 2155-304 with
  H.E.S.S. and Fermi-LAT

Studying the temporal variability of BL Lac objects at the highest energies
provides unique insights into the extreme physical processes occurring in
relativistic jets and in the vicinity of super-massive black holes. To this
end, the long-term variability of the BL Lac object PKS 2155-304 is analyzed in
the high (HE, 100 MeV < E < 300 GeV) and very high energy (VHE, E > 200 GeV)
gamma-ray domain. Over the course of ~9 yr of H.E.S.S observations the VHE
light curve in the quiescent state is consistent with a log-normal behavior.
The VHE variability in this state is well described by flicker noise
(power-spectral-density index {\ss}_VHE = 1.10 +0.10 -0.13) on time scales
larger than one day. An analysis of 5.5 yr of HE Fermi LAT data gives
consistent results ({\ss}_HE = 1.20 +0.21 -0.23, on time scales larger than 10
days) compatible with the VHE findings. The HE and VHE power spectral densities
show a scale invariance across the probed time ranges. A direct linear
correlation between the VHE and HE fluxes could neither be excluded nor firmly
established. These long-term-variability properties are discussed and compared
to the red noise behavior ({\ss} ~ 2) seen on shorter time scales during
VHE-flaring states. The difference in power spectral noise behavior at VHE
energies during quiescent and flaring states provides evidence that these
states are influenced by different physical processes, while the compatibility
of the HE and VHE long-term results is suggestive of a common physical link as
it might be introduced by an underlying jet-disk connection.Comment: 11 pages, 16 figure
First measurement of jet mass in Pb-Pb and p-Pb collisions at the LHC

This letter presents the first measurement of jet mass in Pb-Pb and p-Pb
collisions at $\sqrt{s_{\rm NN}}$ = 2.76 TeV and 5.02 TeV, respectively. Both
the jet energy and the jet mass are expected to be sensitive to jet quenching
in the hot Quantum Chromodynamics (QCD) matter created in nuclear collisions at
collider energies. Jets are reconstructed from charged particles using the
anti-$k_{\rm T}$ jet algorithm and resolution parameter $R = 0.4$. The jets are
measured in the pseudorapidity range $|\eta_{\rm{jet}}|<0.5$ and in three
intervals of transverse momentum between 60 GeV/$c$ and 120 GeV/$c$. The
measurement of the jet mass in central Pb-Pb collisions is compared to the jet
mass as measured in p-Pb reference collisions, to vacuum event generators, and
to models including jet quenching. It is observed that the jet mass in central
Pb-Pb collisions is consistent within uncertainties with p-Pb reference
measurements. Furthermore, the measured jet mass in Pb-Pb collisions is not
reproduced by the quenching models considered in this letter and is found to be
consistent with PYTHIA expectations within systematic uncertainties.Comment: 26 pages, 11 captioned figures, 1 table, authors from page 21,
  published version, figures at
  http://aliceinfo.cern.ch/ArtSubmission/node/336
The effect of autonomous and controlled motives on eating dysregulation: Implications for individuals classified as underweight, overweight or obese

Introduction Controlled and autonomous motivational factors from self-determination theory have previously been highlighted as key factors in eating regulation. The present study examined controlled motives as an overarching motivational factor in eating dysregulation and examined its effects on dieting behaviour for those who are underweight, overweight or obese.\ud
\ud
Objective To examine whether the influence of controlled motives on dieting behaviour would be moderated by body mass index (BMI). Specifically, it was hypothesised that controlled motives would be associated with high levels of dieting behaviour in underweight individuals and low levels of dieting behaviour in individuals classified as overweight or obese.\ud
\ud
Method One hundred and thirty-seven participants completed the measures of height, weight, and motivation and intentions towards watching their diet and subsequently completed a measure of dieting behaviour two weeks later.\ud
\ud
Results Moderated regression and simple slopes analyses provided support for the hypothesised effects at underweight, overweight, and obese range BMIs.\ud
\ud
Conclusion The effect of controlled motives on dieting behaviour is dependent upon BMI and therefore varies across underweight, overweight, and obese individuals. The implications of controlled motives and external pressures to watch one's diet are discussed
How affordances associated with a distractor object affect compatibility effects: a study with the computational model TRoPICALS.

Seeing an object activates both visual and action codes in the brain. Crucial evidence supporting this view is the observation of object to response compatibility effects: perception of an object can facilitate or interfere with the execution of an action (e.g., grasping) even when the viewer has no intention of interacting with the object. TRoPICALS is a computational model that proposes some general principles about the brain mechanisms underlying compatibility effects, in particular the idea that top-down bias from prefrontal cortex, and whether it conflicts or not with the actions afforded by an object, plays a key role in such phenomena. Experiments on compatibility effects using a target and a distractor object show the usual positive compatibility effect of the target, but also an interesting negative compatibility effect of the distractor: responding with a grip compatible with the distractor size produces slower reaction times than the incompatible case. Here, we present an enhanced version of TRoPICALS that reproduces and explains these new results. This explanation is based on the idea that the prefrontal cortex plays a double role in its top-down guidance of action selection producing: (a) a positive bias in favour of the action requested by the experimental task; (b) a negative bias directed to inhibiting the action evoked by the distractor. The model also provides testable predictions on the possible consequences of damage to volitional circuits such as in Parkinsonian patients
The Herschel Virgo Cluster Survey, XX : dust and gas in the foreground Galactic cirrus

We study the correlation between far-infrared/submm dust emission and atomic gas column density in order to derive the properties of the high Galactic latitude, low density, Milky Way cirrus in the foreground of the Virgo cluster of galaxies. Dust emission maps from 60 to 850 mu m are obtained from observations with the Spectral and Photometric Imaging Receiver (SPIRE) and carried out within the Herschel Virgo Cluster Survey (HeViCS); these are complemented by IRAS and Planck maps. Data from the Arecibo legacy Fast ALFA Survey is used to derive atomic gas column densities for two broad velocity components: low and intermediate velocity clouds. Dust emissivities are derived for each gas component and each far-infrared/submm band. For the low velocity clouds, we measure an average emissivity epsilon(LVC)(nu) = (0 . 79 +/- 0.08) x 10(-20) MJy sr(-1) cm(2) at 250 mu m. After fitting a modified blackbody to the available bands, we estimated a dust absorption cross section of tau(LVC)(nu)/ N-HI = (0.49 +/- 0.13) x 10(-25) cm(2) H-1 at 250 mu m (with dust temperature T = 20.4 +/- 1.5 K and spectral index beta = 1.53 +/- 0.17). The results are in excellent agreement with those obtained by Planck over a much larger coverage of the high Galactic latitude cirrus (50% of the sky versus 0.2% in our work). For dust associated with intermediate velocity gas, we confirm earlier Planck results and find a higher temperature and lower emissivity and cross section. After subtracting the modeled components, we find regions at scales smaller than 20 0 in which the residuals deviate significantly from the average scatter, which is dominated by cosmic infrared background. These large residuals are most likely due to local variations in the cirrus dust properties or to high-latitude molecular clouds with average N-H2 less than or similar to 10(20)cm(-2). We find no conclusive evidence for intracluster dust emission in Virgo
VLTI-AMBER velocity-resolved aperture-synthesis imaging of η Carinae with a spectral resolution of 12 000. Studies of the primary star wind and innermost wind-wind collision zone

This is the final version of the article. Available from the publisher via the DOI in this record.Context. The mass loss from massive stars is not understood well. η Carinae is a unique object for studying the massive stellar wind during the luminous blue variable phase. It is also an eccentric binary with a period of 5.54 yr. The nature of both stars is uncertain, although we know from X-ray studies that there is a wind-wind collision whose properties change with orbital phase.
Aims. We want to investigate the structure and kinematics of η Car’s primary star wind and wind-wind collision zone with a high spatial resolution of ~6 mas (~14 au) and high spectral resolution of R = 12 000.
Methods. Observations of η Car were carried out with the ESO Very Large Telescope Interferometer (VLTI) and the AMBER instrument between approximately five and seven months before the August 2014 periastron passage. Velocity-resolved aperture-synthesis images were reconstructed from the spectrally dispersed interferograms. Interferometric studies can provide information on the binary orbit, the primary wind, and the wind collision.
Results. We present velocity-resolved aperture-synthesis images reconstructed in more than 100 different spectral channels distributed across the Brγ 2.166 μm emission line. The intensity distribution of the images strongly depends on wavelength. At wavelengths corresponding to radial velocities of approximately −140 to − 376 km s-1 measured relative to line center, the intensity distribution has a fan-shaped structure. At the velocity of − 277 km s-1, the position angle of the symmetry axis of the fan is ~126°. The fan-shaped structure extends approximately 8.0 mas (~18.8 au) to the southeast and 5.8 mas (~13.6 au) to the northwest, measured along the symmetry axis at the 16% intensity contour. The shape of the intensity distributions suggests that the obtained images are the first direct images of the innermost wind-wind collision zone. Therefore, the observations provide velocity-dependent image structures that can be used to test three-dimensional hydrodynamical, radiative transfer models of the massive interacting winds of η Car.n. The telluric spectra used in this work for spectral calibration of the AMBER
data were created from data that was kindly made available by the NSO/Kitt Peak
Observatory. This publication makes use of the SIMBAD database operated at
CDS, Strasbourg, France. We thank the referee for helpful suggestions. A.F.J.M.
is grateful for financial aid from NSERC (Canada) and FQRNT (Quebec). S.K.
acknowledges support from an STFC Rutherford Fellowship (ST/J004030/1)
and ERC Starting Grant (Grant Agreement No. 639889)