Miracle-dz/UniFAR-FTUs huggingface dataset:
When LEP and Tevatron combined with WMAP and XENON100 shed light on the nature of Dark Matter

Recently, several astrophysical data or would-be signals has been observed in different dark-matter oriented experiments. In each case, one could fit the data at the price of specific nature of the coupling between the Standard Model (SM) particles and a light Dark Matter candidate: hadrophobic (INTEGRAL, PAMELA) or leptophobic (WMAP Haze, dijet anomalies of CDF, FERMI Galactic Center observation). In this work, we show that when one takes into account the more recent LEP and Tevatron analysis, a light thermal fermionic Dark Matte (\lesssim 10 GeV) that couples to electrons is mainly ruled out if one combines the analysis with WMAP constraints. We also study the special case of scalar dark matter, using a mono-photon events simulation to constrain the coupling of dark matter to electron.
The diversity and similarity of simulated cold dark matter haloes

We study the mass, velocity dispersion and anisotropy profiles of Lambda cold dark matter (Lambda CDM) haloes using a suite of N-body simulations of unprecedented numerical resolution. The Aquarius Project follows the formation of six different galaxy-sized haloes simulated several times at varying numerical resolution, allowing numerical convergence to be assessed directly. The highest resolution simulation represents a single dark matter halo using 4.4 billion particles, of which 1.1 billion end up within the virial radius. Our analysis confirms a number of results claimed by earlier work, and clarifies a few issues where conflicting claims may be found in the recent literature. The mass profile of Lambda CDM haloes deviates slightly but systematically from the form proposed by Navarro, Frenk & White. The spherically averaged density profile becomes progressively shallower inwards and, at the innermost resolved radius, the logarithmic slope is gamma equivalent to - d ln /d ln r less than or similar to 1. Asymptotic inner slopes as steep as the recently claimed proportional to r-1.2 are clearly ruled out. The radial dependence of gamma is well approximated by a power law, gamma proportional to r alpha (the Einasto profile). The shape parameter, alpha, varies slightly but significantly from halo to halo, implying that the mass profiles of Lambda CDM haloes are not strictly universal: different haloes cannot, in general, be rescaled to look identical. Departures from similarity are also seen in velocity dispersion profiles and correlate with those in density profiles so as to preserve a power-law form for the spherically averaged pseudo-phase-space density, /Sigma 3 proportional to r-1.875. The index here is identical to that of Bertschinger's similarity solution for self-similar infall on to a point mass from an otherwise uniform Einstein-de Sitter universe. The origin of this striking behaviour is unclear, but its robustness suggests that it reflects a fundamental structural property of Lambda CDM haloes. Our conclusions are reliable down to radii below 0.4 per cent of the virial radius, providing well-defined predictions for halo structure when baryonic effects are neglected, and thus an instructive theoretical template against which the modifications induced by the baryonic components of real galaxies can be judged.
Autoimmune disorders and thyroid function in patients with rheumatoid arthritis after biological treatment

Rheumatoid arthritis (RA) and autoimmune diseases of the thyroid gland (AITD) often occur together. As autoimmune diseases, they share common patho-logical pathways, reflecting the fact that the treat ment of the underlying disease can influence the course of thyroid disorders. The pharmacotherapy of RA is based on the supply of disease-modifying anti-inflammatory drugs with an increasing focus on biologics. This article aims to review the available literature describing the effects of biological treatments on thyroid function. The use of biological drugs may have the potential benefit of regulat ing the level of anti-thyroid antibodies. On the other hand, tumour necrosis factor-alpha (TNF- a ) inhibitors are not indifferent to thyroid function and may increase the incidence of subacute thyroiditis. The coexistence of AITD and RA prompts consideration of the need for routine thyroid screening in RA patients and for RA screening in patients with thyroid disease who report joint problems.
In Vitro Propagation of Sweet Cherry Cultivars

In the paper “In Vitro Propagation of Sweet Cherry Cultivars” by Iona Snir [HortScience 17(2): 192-193. 1982] corrections have been made to the experimental method. Page 193, line 8, should read “irradiance intensity of 40 μEm-2s-1” instead of “600 μW/cm2. ”
DUST COOLING IN SUPERNOVA REMNANTS IN THE LARGE MAGELLANIC CLOUD

The infrared-to-X-ray (IRX) flux ratio traces the relative importance of dust cooling to gas cooling in astrophysical plasma such as supernova remnants (SNRs). We derive IRX ratios of SNRs in the LMC using Spitzer and Chandra SNR survey data and compare them with those of Galactic SNRs. IRX ratios of all the SNRs in the sample are found to be moderately greater than unity, indicating that dust grains are a more efficient coolant than gas although gas cooling may not be negligible. The IRX ratios of the LMC SNRs are systematically lower than those of the Galactic SNRs. As both dust cooling and gas cooling pertain to the properties of the interstellar medium, the lower IRX ratios of the LMC SNRs may reflect the characteristics of the LMC, and the lower dust-to-gas ratio (a quarter of the Galactic value) is likely to be the most significant factor. The observed IRX ratios are compared with theoretical predictions that yield IRX ratios an order of magnitude larger. This discrepancy may originate from the dearth of dust in the remnants due to either the local variation of the dust abundance in the preshock medium with respect to the canonical abundance or the dust destruction in the postshock medium. The non-equilibrium ionization cooling of hot gas, in particular for young SNRs, may also cause the discrepancy. Finally, we discuss implications for the dominant cooling mechanism of SNRs in low-metallicity galaxies.
CFD analysis and experimental investigation to determine the flow characteristics around NACA 4412 airfoil blades at different wind speeds and blade angles

An aerodynamically efficient blade is one of the prime necessities to extract the maximum mechanical power from a wind turbine. A number of researches are available in the literature studying blade design and configuration to improve aerodynamic characteristics of horizontal axis wind turbines. Less attention, however, has been devoted to wind turbines in terms of simultaneous optimization of blade and airfoil angles. The present study is important for the aerodynamic design and manufacturing of wind turbine blades. In this regard, various blade angles have been numerically simulated to determine the optimum blade angle. In addition to numerical analysis, experimental tests have been done to investigate NACA 4412 blade angle. As a result of this study, it was observed that blade angle in the range of 5°–10° showed the best performance among the tested various blade angles.
The Canadian Cluster Comparison Project: detailed study of systematics and updated weak lensing masses

Masses of clusters of galaxies from weak gravitational lensing analyses of ever larger samples are increasingly used as the reference to which baryonic scaling relations are compared. In this paper we revisit the analysis of a sample of 50 clusters studied as part of the Canadian Cluster Comparison Project. We examine the key sources of systematic error in cluster masses. We quantify the robustness of our shape measurements and calibrate our algorithm empirically using extensive image simulations. The source redshift distribution is revised using the latest state-of-the-art photometric redshift catalogs that include new deep near-infrared observations. Nonetheless we find that the uncertainty in the determination of photometric redshifts is the largest source of systematic error for our mass estimates. We use our updated masses to determine b, the bias in the hydrostatic mass, for the clusters detected by Planck. Our results suggest 1-b=0.76+-0.05(stat)}+-0.06(syst)}, which does not resolve the tension with the measurements from the primary cosmic microwave background.
The First Billion Years project: the escape fraction of ionizing photons in the epoch of reionization

Proto-galaxies forming in low-mass dark matter haloes are thought to provide the majority of ionizing photons needed to reionize the Universe, due to their high escape fractions of ionizing photons. We study how the escape fraction in high-redshift galaxies relates to the physical properties of the halo in which the galaxies form, by computing escape fractions in more than 75000 haloes between redshifts 27 and 6 that were extracted from the First Billion Years project, high-resolution cosmological hydrodynamics simulations of galaxy formation. We find that the main constraint on the escape fraction is the gas column density in a radius of 10 pc around the stellar populations, causing a strong mass dependence of the escape fraction. The lower potential well in haloes with virial mass below 1e8 solar mass results in low column densities that can be penetrated by radiation from young stars (age < 5 Myr). In haloes with virial mass above 1e8 solar mass supernova feedback is important, but only 30% of the haloes in this mass range have an escape fraction higher than 1%. We find a large range of escape fractions in haloes with similar properties, caused by different distributions of the dense gas in the halo. This makes it very hard to predict the escape fraction on the basis of halo properties and results in a highly anisotropic escape fraction. The strong mass dependence, the large spread and the large anisotropy of the escape fraction may strongly affect the topology of reionization and is something current models of cosmic reionization should strive to take into account.
Space weather conditions and spacecraft anomalies in different orbits

A large database of anomalies, registered by 220 satellites in different orbits over the period 1971–1994, has been compiled. For the first time, data of 49 Russian Kosmos satellites have been included in a statistical analysis. The database also contains a large set of daily and hourly space weather parameters. A series of statistical analyses made it possible to quantify, for different satellite orbits, space weather conditions in the days characterized by anomaly occurrences. In particular, very intense fluxes (>1000 particles cm−2 s−1 sr−1 (pfu) at energy >10 MeV) of solar protons are linked to anomalies registered by satellites in high‐altitude (>15,000 km) near‐polar (inclination >55°) orbits typical for navigation satellites such as those used in the GPS network, NAVSTAR, etc. (the rate of anomalies increases by a factor of ∼20) and to a much smaller extent to anomalies in geostationary orbits (the rate increases by a factor of ∼4). The efficiency in producing anomalies is found to be negligible for proton fluences <100 pfu at energies >10 MeV. Elevated fluxes of energetic (>2 MeV) electrons >108 cm−2 d−1 sr−1 are observed by GOES on days with satellite anomalies occurring at geostationary (GOES, SCATHA, METEOSAT, MARECS A, etc.) and low‐altitude (<1500 km) near‐polar (>55°) orbits (Kosmos, SAMPEX, etc.). These elevated fluxes are not observed on days of anomalies registered in high‐altitude near‐polar orbits. Direct and indirect connections between anomaly occurrence and geomagnetic perturbations are also discussed.
Preheating and locked inflation: an analytic approach towards parametric resonance

We take an analytic approach towards the framework of parametric resonance and apply it on preheating and locked inflation. A two-scalar toy model is analytically solved for the \lambda\phi^2\chi^2 coupling for the homogenous modes. The effects of dynamic universe background and backreaction are taken into account. We show the average effect of parametric resonance to be that \chi's amplitude doubles for each cycle of \phi. Our framework partly solves the preheating scenario, showing two distinct stages of preheating and making the parameters of preheating analytically calculable. It is demonstrated for slowroll inflation models, preheating is terminated, if by backreaction, typically in the 5th e-fold. Under our framework, a possible inhomogeneity amplification effect is also found during preheating, which both may pose strong constraints on some inflationary models and may amplify tiny existing inhomogeneities to the desired scale. For demonstration, we show it rules out the backreaction end of preheating of the quadratic slowroll inflation model with mass m\sim10^{-6}. For locked inflation, parametric resonance is found to be inhibited if \phi{} has more than one real component.
GUIDING THE SWITCH FROM TRIANGLE TESTING TO TETRAD TESTING

ABSTRACT Tetrad testing is theoretically more powerful than Triangle testing, yet the addition of a fourth stimulus raises questions – it is possible that the addition of a fourth stimulus places such an additional demand on subjects that the theoretical advantage of the Tetrad test is lost. In this paper, we provide a guideline to compare results of Tetrad and Triangle. Specifically, it is roughly correct to say that as long as the effect sizes do not drop by more than one third for the same stimuli, then the Tetrad test remains more powerful than the Triangle test. We explain this guideline in terms of perceptual noise, illustrate its use in several examples and discuss the statistical considerations that accompany its use. To assist with statistical evaluation, we provide a table for finding the variance in the Tetrad-based measurement of the effect size. Finally, we show how the Thurstonian framework helps us to improve discrimination testing efficiency even when we do not seek additional power. PRACTICAL APPLICATIONS Discrimination testing programs based on Triangle testing might be made more sensitive or more efficient by the use of Tetrad testing. This paper develops a guideline to assist sensory scientists who are considering a switch from the Triangle test to the Tetrad test. The paper displays the use of this guideline in several examples, discusses the relevant statistical considerations, provides a helpful table and demonstrates how Thurstonian theory can be used to improve efficiency even in an already successful discrimination testing program.
Compactness and finite forcibility of graphons

Graphons are analytic objects associated with convergent sequences of graphs. Problems from extremal combinatorics and theoretical computer science led to a study of graphons determined by finitely many subgraph densities, which are referred to as finitely forcible. Following the intuition that such graphons should have finitary structure, Lovasz and Szegedy conjectured that the topological space of typical vertices of a finitely forcible graphon is always compact. We disprove the conjecture by constructing a finitely forcible graphon such that the associated space is not compact. The construction method gives a general framework for constructing finitely forcible graphons with non-trivial properties.
The Influence Of Environmental Performance And Good Corporate Governance On Company Value

The value of the company is an indicator of the company in terms of fulfilling its obligations to investors, the value of the company also reflects the sustainability of the company in the future. However, there are many cases of environmental pollution in Indonesia, such as the case of PT. Lapindo Brantas Inc. who made negligence in drilling oil and gas in Sidoarjo had a negative impact on society, the environment and resulted in the decline in the share price of PT. Energi Mega Persada, Tbk. (major shareholder of PT. Lapindo Brantas Inc). In addition, there is also a case of PT. Freeport is currently the concern of various parties related to the change in the status of the contract of work owned by PT. Freeport became a Special Mining Business License (IUPK). This study aims to determine the effect of environmental performance and good corporate governance on firm value on IDX LQ45 index companies for the 2017-2021 period. The sampling technique used is purposive sampling technique so as to obtain 45 sample companies. The data analysis technique used in this study is multiple linear regression. This test shows that environmental performance and good corporate governance have a positive and significant effect on firm value on the Indonesia Stock Exchange.
QCD transition temperature: full staggered result

We conclude our investigations on the QCD cross-over transition temperatures with 2+1 staggered flavours and one-link stout improvement. We extend our previous two studies [Phys. Lett. B643 (2006) 46, JHEP 0906:088 (2009)] by choosing even finer lattices (N_t=16) and we work again with physical quark masses. These new results [for details see JHEP 1009:073,2010] support our earlier findings. We compare them with the published results of the hotQCD collaboration. All these results are confronted with the predictions of the Hadron Resonance Gas model and Chiral Perturbation Theory for temperatures below the transition region. Our results can be reproduced by using the physical spectrum. The findings of the hotQCD collaboration can be recovered only by using a distorted spectrum. This analysis provides a simple explanation for the observed discrepancy in the transition T between our and the hotQCD collaborations.
L1506: a prestellar core in the making

Context. Exploring the structure and dynamics of cold starless clouds is necessary to understand the different steps leading to the formation of protostars. Because clouds evolve slowly, many of them must be studied in detail to identify different moments in a cloud's lifetime. Aims: We study a fragment of the long filament L1506 in the Taurus region, which we name L1506C, a core with interesting dust properties observed by the PRONAOS balloon-borne telescope. Methods: To trace the mass content of L1506C and its kinematics, we mapped the dust emission, and the line emission of two key species, C18O and N2H+. We also observed 13CO and C17O. We model the species emission using 1D Monte Carlo models. Results: This cloud is reminiscent of L1498 but also exhibits peculiar features: i) a large envelope emitting solely in 13CO that contains a much smaller core with strong C18O depletion at its centre despite a low maximum opacity (AV ~ 20 mag); ii) extremely narrow C18O lines indicating a low, non-measurable turbulence; iii) contraction traced by C18O itself (plus rotation); iv) unexpectedly, the kinematical signature of the external envelope is opposite to that of the core, the 13CO and C18O velocity gradients having opposite directions and the C18O line profile being blue peaked in contrast to the 13CO one which is red peaked. The core is large (r = 3 × 104 AU) and not very dense (n(H2) ≤ 5 × 104 cm-3, possibly less). This core is therefore not yet prestellar. Conclusions: All these properties imply that the core is kinematically detached from its envelope and in the process of forming a prestellar core. This is the first time that the dynamical formation of a prestellar core has been witnessed. The extremely low turbulence could explain the strong depletion of this core despite its relatively low density and opacity in contrast to undepleted cores such as L1521E, which exhibits a turbulence at least 4 times as high. Based on observations made with the IRAM-30 m. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain).
Quasiclassical cyclotron resonance of Dirac fermions in highly doped graphene

Cyclotron resonance in highly doped graphene has been explored in the infrared magneto-transmission experiment. Contrary to previous works, which only focused on the magneto-optical properties of graphene in its quantum regime, here we study the quasi-classical response of this system. We show that it has a character of classical cyclotron resonance, which is linear in the applied magnetic field, with an effective cyclotron mass defined by the position of the Fermi level m = E_F/v_F^2.
Step-edge magnetoresistance in La0.7Ca0.3MnO3 films

The magnetoresistance of step-edge structures in La0.7Ca0. 3MnO3 films was investigated. Step-edge arrays with 200 steps of height 140–200 nm and step separation 20 μm along [110] were fabricated on LaAlO3 substrates by chemically assisted ion-beam etching. Thin La0.7Ca0. 3MnO3 films were deposited on the structured substrates by pulsed-laser deposition. Measurements of the large low-field magnetoresistance, the dynamic conductance, and the anisotropic magnetoresistance lead to the proposal of a model of spin-polarized tunneling in a ferromagnet/spin-glass/ferromagnet geometry.
Dynamics of stellar black holes in young star clusters with different metallicities – II. Black hole–black hole binaries

In this paper, we study the formation and dynamical evolution of black hole-black hole (BH-BH) binaries in young star clusters (YSCs), by means of N-body simulations. The simulations include metallicity-dependent recipes for stellar evolution and stellar winds, and have been run for three different metallicities (Z = 0.01, 0.1 and 1 Zsun). Following recent theoretical models of wind mass-loss and core-collapse supernovae, we assume that the mass of the stellar remnants depends on the metallicity of the progenitor stars. We find that BH-BH binaries form efficiently because of dynamical exchanges: in our simulations, we find about 10 times more BH-BH binaries than double neutron star binaries. The simulated BH-BH binaries form earlier in metal-poor YSCs, which host more massive black holes (BHs) than in metal-rich YSCs. The simulated BH-BH binaries have very large chirp masses (up to 80 Msun), because the BH mass is assumed to depend on metallicity, and because BHs can grow in mass due to the merger with stars. The simulated BH-BH binaries span a wide range of orbital periods (10^-3-10^7 yr), and only a small fraction of them (0.3 per cent) is expected to merge within a Hubble time. We discuss the estimated merger rate from our simulations and the implications for Advanced VIRGO and LIGO.
CHARACTERIZATION OF THE VERY-LOW-MASS SECONDARY IN THE GJ 660.1AB SYSTEM

We present a spectroscopic analysis of the low-mass binary star system GJ 660.1AB, a pair of nearby M dwarfs for which we have obtained separated near-infrared spectra (0.9–2.5 μm) with the SpeX spectrograph. The spectrum of GJ 660.1B is distinctly peculiar, with a triangular-shaped 1.7 μm peak that initially suggests that it is a low-surface-gravity, young brown dwarf. However, we rule out this hypothesis and determine instead that this companion is a mild subdwarf (d/sdM7) based on the subsolar metallicity of the primary, [Fe/H] = −0.63 ± 0.06. Comparison of the near-infrared spectrum of GJ 660.1B to two sets of spectral models yields conflicting results, with a common effective temperature of Teff = 2550–2650 K, but alternately low surface gravity ( log g ? > = 4.4 − 0.5 + 0.5 ? > ) and very low metallicity ([M/H] = − 0.96 − 0.24 + 0.19 ? > ), or high surface gravity ( log g ? > = 5.0–5.5) and slightly subsolar metallicity ([M/H] = − 0.20 − 0.19 + 0.13 ? > ). We conjecture that insufficient condensate opacity and excessive collision-induced H2 absorption in the models bias them toward low surface gravities and a metallicity that is inconsistent with the primary and points toward improvements needed in the spectral modeling of metal-poor, very-low-mass dwarfs. The peculiar spectral characteristics of GJ 660.1B emphasize that care is needed when interpreting surface gravity features in the spectra of ultracool dwarfs.