Miracle-dz/UniFAR-FTUs huggingface dataset:
Correlation of Single Nucleotide Polymorphisms of PRM1, PRM2, PYGO2, and DAZL Genes with Male Infertility in North West of Iran

Objective: Almost half of infertility is related to male factors. Although the effect of genetic factors on male infertility is identified, about 30%-50% still has no proven cause and is classified as idiopathic infertility. This study was performed to investigate the correlation of some single nucleotide polymorphisms of PYGO2, DAZL, PRM1, and PRM2 genes with male infertility in idiopathic cases among the Iranian population. Material and methods: In this case-control study, 120 idiopathic azoospermia or severe oligospermia patients in the range of 25-45 years and 120 fertile men in the same age range were recruited as case and control groups, respectively. Eight different single nucleotide polymorphisms including PRM1 rs737008, PRM1 rs423668, PRM2 rs1646022, PRM2 rs11645592, PYGO2 rs141722381, PYGO2rs61758741, DAZL rs75931701, and DAZL rs188506466 were genotyped by using amplification-refractory mutation system polymerase chain reaction methods. Hardy-Weinberg was calculated by using online website. Statistical Package for Social Sciences software was applied for statistical analysis. P value <. 05 was considered significant. Thirty percent of the samples were regenotyped to confirm the obtained results. Results: The obtained results showed a significant correlation between PYGO2 rs141722381 in the heterozygote form (odds ratio: 2.803, 95% CI: 1.397-5.626). Heterozygote over-dominance was also observed in this variant (odds ratio: 2.637, 95%CI: 1.321-5.264). There was no significant association between other studied single nucleotide polymorphisms and male infertility. Conclusion: This study proposed a novel single nucleotide polymorphism as a predisposition of male infertility among the Iranian population, but more studies in larger populations are needed to confirm the results.
DYNAMICAL EVOLUTION OF YOUNG EMBEDDED CLUSTERS: A PARAMETER SPACE SURVEY

This paper investigates the dynamical evolution of embedded stellar clusters from the protocluster stage, through the embedded star-forming phase, and out to ages of 10 Myr—after the gas has been removed from the cluster. The relevant dynamical properties of young stellar clusters are explored over a wide range of possible star formation environments using N-body simulations. Many realizations of equivalent initial conditions are used to produce robust statistical descriptions of cluster evolution including the cluster bound fraction, radial probability distributions, as well as the distributions of close encounter distances and velocities. These cluster properties are presented as a function of parameters describing the initial configuration of the cluster, including the initial cluster membership N, initial stellar velocities, cluster radii, star formation efficiency, embedding gas dispersal time, and the degree of primordial mass segregation. The results of this parameter space survey, which includes ∼25,000 simulations, provide a statistical description of cluster evolution as a function of the initial conditions. We also present a compilation of the FUV radiation fields provided by these same cluster environments. The output distributions from this study can be combined with other calculations, such as disk photoevaporation models and planetary scattering cross sections, to ascertain the effects of the cluster environment on the processes involved in planet formation.
Mechanical and Thermal Properties of Shale Ceramsite Concrete: Experimental Study on the Influence Law due to Microencapsulated Phase-Change Material Content and Phase-Change Cycle Numbers

The addition of microencapsulated phase-change materials (MPCM) to concrete will inevitably cause changes in the mechanical and thermal properties of concrete, and this is vitally important for the safety and energy saving of concrete building components. In this research, shale ceramsite and shale ceramics sand were used as the main raw materials to produce lightweight aggregate concrete (LWAC) mixed with MPCM. In order to investigate the effect of MPCM content and phase-change cycle numbers on the mechanical and thermal properties of MPCM-LWAC, two groups of MPCM-LWAC specimens were prepared. One group consists of specimens containing 2.5%, 5.0%, 7.5%, and 10% MPCM, respectively, and they are used to reveal the change law of tensile strength, compressive strength, enthalpy, and specific heat capacity of LWAC integrated into MPCM. The other group includes specimens with the same MPCM content, but the specimens are subjected to different phase-change cycle numbers of 50, 100, 150, and 200 at the environment temperature of −10–60°C to study the thermal properties of MPCM-LWAC. Findings from the experimental results include the following: (1)The tensile and compressive strengths of MPCM-LWAC concrete are negatively correlated with the MPCM content, while the enthalpy and specific heat capacity are positively correlated with the MPCM content. When the MPCM content reaches 10%, the compressive and tensile strengths of MPCM-LWAC decreased, respectively, by 45.49% and 52.63% than the LWAC without MPCM. (2) Under heating and curing condition, the corresponding maximum specific heat capacity of LWAC with 10% MPCM is 328.35% and 249.50% higher than the LWAC without MPCM, respectively, and the average specific heat capacities increase 71.21% and 44.94%, respectively. (3) The melting enthalpy of MPCM-LWAC is slightly larger than the curing enthalpy, and the difference is more noticeable with the increase of MPCM content. In addition, when the number of phase-change cycle is below 200, the compressive strength and splitting tensile strength of MPCM-LWAC decrease by less than 5%, and the specific heat capacity decreases by less than 1.33%. Hence, it concludes that shale ceramsite concrete with MPCM has promising application prospects.
Using XMM–Newton to study the energy-dependent variability of H 1743-322 during its 2014 outburst

Black hole transients during bright outbursts show distinct changes of their spectral and variability properties as they evolve during an outburst, that are interpreted as evidence for changes in the accretion flow and X-ray emitting regions. We obtained an anticipated XMM-Newton ToO observation of H 1743-322 during its outburst in September 2014. Based on data of eight outbursts observed in the last 10 years we expected to catch the start of the hard-to-soft state transition. The fact that neither the general shape of the observed power density spectrum nor the characteristic frequency show an energy dependence implies that the source still stays in the low-hard state at the time of our observation near outburst peak. The spectral properties agree with the source being in the low-hard state and a Swift/XRT monitoring of the outburst reveals that H 1743-322 stays in the low-hard state during the entire outburst (a. k. a. 'failed outburst'). We derive the averaged QPO waveform and obtain phase-resolved spectra. Comparing the phase-resolved spectra to the phase averaged energy spectrum reveals spectral pivoting. We compare variability on long and short time scales using covariance spectra and find that the covariance ratio does not show an increase towards lower energies as has been found in other black hole X-ray binaries. There are two possible explanations: either the absence of additional disc variability on longer time scales is related to the rather high inclination of H 1743-322 compared to other black hole X-ray binaries or it is the reason why we observe H 1743-322 during a failed outburst. More data on failed outbursts and on high-inclination sources will be needed to investigate these two possibilities further.
Suppression of phase mixing in drift-kinetic plasma turbulence

Transfer of free energy from large to small velocity-space scales by phase mixing leads to Landau damping in a linear plasma. In a turbulent drift-kinetic plasma, this transfer is statistically nearly canceled by an inverse transfer from small to large velocity-space scales due to “anti-phase-mixing” modes excited by a stochastic form of plasma echo. Fluid moments (density, velocity, and temperature) are thus approximately energetically isolated from the higher moments of the distribution function, so phase mixing is ineffective as a dissipation mechanism when the plasma collisionality is small.
NEAR-INFRARED DIFFUSE INTERSTELLAR BANDS IN 0.91–1.32 μm

We present a comprehensive survey of diffuse interstellar bands (DIBs) in 0.91–1.32 μm with the newly developed near-infrared (NIR) spectrograph WINERED mounted on the Araki 1.3 m telescope in Japan. We obtained high-resolution (R = 28, 300) spectra of 25 early-type stars with color excesses of 0.07 < E(B − V) < 3.4. In addition to the 4 DIBs previously detected in this wavelength range, we identified 15 new DIBs, 7 of which were reported as DIB “candidates” by Cox. We analyze the correlations among NIR DIBs, strong optical DIBs, and the reddening of the stars. Consequently, we found that all NIR DIBs show weaker correlations with the reddening rather than the optical DIBs, suggesting that the equivalent widths of NIR DIBs depend on some physical conditions of the interstellar clouds, such as UV flux. Three NIR DIBs, λλ10780, 10792, and 11797, are found to be classifiable as a “family,” in which the DIBs are well correlated with each other, suggesting that the carriers of these DIBs are connected with some chemical reactions and/or have similar physical properties such as ionization potential. We also found that the three strongest NIR DIBs, λλ10780, 11797, and 13175 are well correlated with the optical DIB λ5780. 5, whose carrier is proposed to be a cation molecule with high ionization potential, indicating that the carriers of the NIR DIBs could be cation molecules.
Hexagonal phase stabilization and magnetic orders of multiferroic Lu1-xScxFeO3

Hexagonal $\mathrm{LuFe}{\mathrm{O}}_{3}$ has drawn a lot of research attention due to its contentious room-temperature multiferroicity. Due to the instability of hexagonal phase in the bulk form, most experimental studies focused on $\mathrm{LuFe}{\mathrm{O}}_{3}$ thin films which can be stabilized by strain using proper substrates. Here we report on the hexagonal phase stabilization, magnetism, and magnetoelectric coupling of bulk $\mathrm{LuFe}{\mathrm{O}}_{3}$ by partial Sc substitution of Lu. First, our first-principles calculations show that the hexagonal structure can be stabilized by partial Sc substitution, while the multiferroic properties, including the noncollinear magnetic order and geometric ferroelectricity, remain robustly unaffected. Therefore, $\mathrm{L}{\mathrm{u}}_{1\ensuremath{-}x}\mathrm{S}{\mathrm{c}}_{x}\mathrm{Fe}{\mathrm{O}}_{3}$ can act as a platform to check the multiferroicity of $\mathrm{LuFe}{\mathrm{O}}_{3}$ and related materials in the bulk form. Second, the magnetic characterizations on bulk $\mathrm{L}{\mathrm{u}}_{1\ensuremath{-}x}\mathrm{S}{\mathrm{c}}_{x}\mathrm{Fe}{\mathrm{O}}_{3}$ demonstrate a magnetic anomaly (probable antiferromagnetic ordering) above room temperature, \ensuremath{\sim}425--445 K, followed by magnetic transitions in low temperatures (\ensuremath{\sim}167--172 K). In addition, a magnetoelectric response is observed in the low-temperature region. Our study provides useful information on the multiferroic physics of hexagonal $R\mathrm{Fe}{\mathrm{O}}_{3}$ and related systems.
How Halal Labelled Products Influence on Repurchase Intention

Innovation is a source of competitive advantage. Halal labeled as an output of innovation is still very rare in research and publication. This study examines the influence of innovation attributes on repurchase intention of halal-labelled products of PT Indofood Sukses Makmur Tbk. The respondents are people who have purchased Indofood products and live in Jabodetabek area, amounting to 188 respondents. Data analysis applied simple linear regression test using SPSS software. Quantitative method conducted in this research and data collected through digital form questionnaire derived from each variable. The research results indicated that four dimensions of innovation attributes, namely relative advantage, trialability, observability, and compatibility, have a positive effect on repurchase intention, while one dimension, namely complexity, has a negative effect. It indicates that innovation attributes will be able to increase repurchase intention.
Gamete donation: anti-anonymity does not equate to anti-donation

Abstract What is the relationship between the position that anonymous gamete donation is wrong (i.e. the anti-anonymity position) and the position that all gamete donation is wrong (i.e. the anti-donation position)? Some argue that people who accept the anti-anonymity position should also accept the anti-donation position on the grounds that the two positions share the same main arguments. But that’s not true. One argument in favor of anti-anonymity does not generate genuine dialectical pressure to accept the anti-donation position. The other anti-anonymity arguments do generate dialectical pressure, but not in a way that pushes toward the anti-donation position. Instead, they push toward what we might call the ‘pro-known-donation’ position. So, either there is no dialectical pressure or, where there is, it doesn’t flow toward the anti-donation position.
Neptune's atmospheric composition from AKARI infrared spectroscopy

Aims. Disk-averaged infrared spectra of Neptune between 1.8 and 13 μm, obtained by the AKARI infrared camera (IRC) in May 2007, have been analysed to (a) determine the globally-averaged stratospheric temperature structure; (b) derive the abundances of stratospheric hydrocarbons; and (c) detect fluorescent emission from CO at 4.7 μm. Methods. Mid-infrared spectra (SG1 and SG2 channels of AKARI/IRC), with spectral resolutions of 47 and 34 respectively, were modelled using a line-by-line radiative transfer code to determine the temperature structure between 1‐1000 μbar and the abundances of CH4 ,C H3D and higher-order hydrocarbons. A full non-LTE radiative model was then used to determine the best fitting CO profile to reproduce the fluorescent emission observed at 4.7 μm in the NG channel (with a spectral resolution of 135). Results. The globally-averaged stratospheric temperature structure is quasi-isothermal between 1‐1000 μbar, which suggests little variation in global stratospheric conditions since studies by the Infrared Space Observatory a decade earlier. The derived CH4 mole fraction of (9.0 ± 3.0) × 10 −4 at 50 mbar, decreasing to (0.9 ± 0.3) × 10 −4 at 1 μbar, is larger than that expected if the tropopause at 56 K acts as an efficient cold trap, but consistent with the hypothesis that CH4 leaking through the warm south polar tropopause (62‐66 K) is globally redistributed by stratospheric motion. The ratio of D/ Hi n CH4 of 3.0 ± 1.0 × 10 −4 supports the conclusion that Neptune is enriched in deuterium relative to the other giant planets. We determine a mole fraction of ethane of (8.5 ± 2.1) × 10 −7 at 0.3 mbar, consistent with previous studies, and a mole fraction of ethylene of 5.0 +1.8
Does Democracy Die in Darkness? An Examination of the Relationship between Local Newspaper Health and Turnout in Municipal Politics

Abstract This study is, to our knowledge, the first quantitative analyses of the relationship between local print newspaper health and voter turnout in Canadian municipal elections. Municipal turnout is understudied in Canada, and the few studies on the topic overlook the role of local media. This cross-sectional study fills a gap in the literature by determining the relationship between local print newspaper health and municipal election turnout in a unique dataset of 233 populous Canadian municipalities. Results reveal a significant positive correlation between turnout and two measures of newspaper health: (1) the total number of newspapers per population and (2) the publication frequency of the largest newspaper in a municipality.
A ~6 Mpc overdensity at z = 2.7 detected along a pair of quasar sight lines: filament or protocluster?

Simulations predict that gas in the intergalactic medium (IGM) is distributed in filamentary structures that connect dense galaxy clusters and form the cosmic web. These structures of predominantly ionized hydrogen are difficult to observe directly due to their lack of emitting regions. We serendipitously detected an overdensity of log N(HI) > 18.0 absorbers at z = 2.69 along the lines of sight toward a pair of background quasars. Three main absorption regions spanning ~2000 km/s (corresponding to 6.4 (h_70)^(-1) Mpc proper) are coincident in the two lines of sight, which are separated by ~90 (h_70)^(-1) kpc transverse proper distance. Two regions have [Fe/H] < -1.9 and correspond to mild overdensities in the IGM gas. The third region is a sub-DLA with [Fe/H] = -1.1 that is probably associated with a galaxy. We discuss the possibility that the lines of sight probe along the length of a filament or intercept a galaxy protocluster.
Milky Way simulations: The Galaxy, its stellar halo and its satellites – insights from a hybrid cosmological approach

Our home galaxy – the Milky Way – is a fairly large spiral galaxy, prototype of the most common morphological class in the local Universe. Although being only a galaxy, it is the only one that can be studied in unique detail: for the Milky Way and for a number of members of the Local Group, a wealth of observational data is available about the ages and chemical abundances of their stars. Much more information is expected to come in the next few years, from ongoing and planned spectroscopic and astrometric surveys, providing a unique benchmark for modern theories of galaxy formation. In this review, I will summarize recent results on the formation of our Milky Way, its stellar halo, and its satellite galaxies. I will focus, in particular, on results obtained in the framework of hybrid models of galaxy formation, and refer to other reviews in this issue for studies based on hydrodynamical simulations (© 2012 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)
RADIO MONITORING OF THE TIDAL DISRUPTION EVENT SWIFT J164449.3+573451. I. JET ENERGETICS AND THE PRISTINE PARSEC-SCALE ENVIRONMENT OF A SUPERMASSIVE BLACK HOLE

We present continued radio observations of the tidal disruption event Swift J164449.3+573451 extending to δt ≈ 216 days after discovery. The data were obtained with the EVLA, AMI Large Array, CARMA, the SMA, and the VLBA+Effelsberg as part of a long-term program to monitor the expansion and energy scale of the relativistic outflow, and to trace the parsec-scale environment around a previously dormant supermassive black hole (SMBH). The new observations reveal a significant change in the radio evolution starting at δt ≈ 1 month, with a brightening at all frequencies that requires an increase in the energy by about an order of magnitude, and an overall density profile around the SMBH of ρ∝r−3/2 (0.1–1.2 pc) with a significant flattening at r ≈ 0.4–0.6 pc. The increase in energy cannot be explained with continuous injection from an L∝t−5/3 tail, which is observed in the X-rays. Instead, we conclude that the relativistic jet was launched with a wide range of Lorentz factors, obeying E(> Γj)∝Γ−2.5j. The similar ratios of duration to dynamical timescale for Sw 1644+57 and gamma-ray bursts (GRBs) suggest that this result may be applicable to GRB jets as well. The radial density profile may be indicative of Bondi accretion, with the inferred flattening at r ∼ 0.5 pc in good agreement with the Bondi radius for a ∼few × 106 M☉ black hole. The density at ∼0.5 pc is about a factor of 30 times lower than inferred for the Milky Way Galactic Center, potentially due to a smaller number of mass-shedding massive stars. From our latest observations (δt ≈ 216 days) we find that the jet energy is Ej, iso ≈ 5 × 1053 erg (Ej ≈ 2.4 × 1051 erg for θj = 0.1), the radius is r ≈ 1.2 pc, the Lorentz factor is Γj ≈ 2.2, the ambient density is n ≈ 0.2 cm−3, and the projected angular size is rproj ≈ 25 μas, below the resolution of the VLBA+Effelsberg. Assuming no future changes in the observed evolution and a final integrated total energy of Ej ≈ 1052 erg, we predict that the radio emission from Sw 1644+57 should be detectable with the EVLA for several decades and will be resolvable with very long baseline interferometry in a few years.
REVISITING ULYSSES OBSERVATIONS OF INTERSTELLAR HELIUM

We report the results of a comprehensive reanalysis of Ulysses observations of interstellar He atoms flowing through the solar system, the goal being to reassess the interstellar He flow vector and to search for evidence of variability in this vector. We find no evidence that the He beam seen by Ulysses changes at all from 1994–2007. The direction of flow changes by no more than ∼0. °3 and the speed by no more than ∼0.3 km s−1. A global fit to all acceptable He beam maps from 1994–2007 yields the following He flow parameters: VISM = 26.08 ± 0.21 km s−1, λ = 75.54 ± 0. °19, β = −5.44 ± 0. °24, and T = 7260 ± 270 K; where λ and β are the ecliptic longitude and latitude direction in J2000 coordinates. The flow vector is consistent with the original analysis of the Ulysses team, but our temperature is significantly higher. The higher temperature somewhat mitigates a discrepancy that exists in the He flow parameters measured by Ulysses and the Interstellar Boundary Explorer, but does not resolve it entirely. Using a novel technique to infer photoionization loss rates directly from Ulysses data, we estimate a density of nHe = 0.0196 ± 0.0033 cm−3 in the interstellar medium.
Multiple Regression: A Primer

What Is Multiple Regression? How Do I Interpret Multiple Regression Results? What Can Go Wrong with Multiple Regression? How Do I Run a Multiple Regression? How Does Bivariate Regression Work? What Are the Assumptions of Multiple Regression? What Can Be Done about Multicollinearity? How Can Multiple Regression Handle Nonlinear Relationships? How Is Multiple Regression Related to Other Statistical Techniques?
Properties of the first-order Fermi acceleration in fast magnetic reconnection driven by turbulence in collisional magnetohydrodynamical flows

Fast magnetic reconnection may occur in different astrophysical sources, producing flare-like emission and particle acceleration. Currently, this process is being studied as an efficient mechanism to accelerate particles via a first-order Fermi process. In this work we analyse the acceleration rate and the energy distribution of test particles injected in three-dimensional magnetohydrodynamical (MHD) domains with large-scale current sheets where reconnection is made fast by the presence of turbulence. We study the dependence of the particle acceleration time with the relevant parameters of the embedded turbulence, i.e., the Alfv\'en speed $V_{\rm A}$, the injection power $P_{\rm inj}$ and scale $k_{\rm inj}$ ($k_{\rm inj} = 1/l_{\rm inj}$). We find that the acceleration time follows a power-law dependence with the particle kinetic energy: $t_{acc} \propto E^{\alpha}$, with $0.2 < \alpha < 0.6$ for a vast range of values of $c / V_{\rm A} \sim 20 - 1000$. The acceleration time decreases with the Alfv\'en speed (and therefore with the reconnection velocity) as expected, having an approximate dependence $t_{acc} \propto (V_{\rm A} / c)^{-\kappa}$, with $\kappa \sim 2.1- 2.4$ for particles reaching kinetic energies between $1 - 100 \, m_p c^2$, respectively. Furthermore, we find that the acceleration time is only weakly dependent on the $P_{\rm inj}$ and $l_{\rm inj}$ parameters of the turbulence. The particle spectrum develops a high-energy tail which can be fitted by a hard power-law already in the early times of the acceleration, in consistency with the results of kinetic studies of particle acceleration by magnetic reconnection in collisionless plasmas.