Miracle-dz/UniFAR-FTUs huggingface dataset:
Relational Leadership Within Business Partnerships In India: A Process Framework

Inter-organizational partnerships are an essential mechanism for corporations to access resources, particularly in emerging markets. This study is concerned with the steps relating to how multinational corporations in India create, develop, and evaluate their partnerships based on relationships. In the context of business-to-business partnerships, the researchers aim to (i) create a relational leadership process framework for how these relationships are built, and (ii) analyze if relational governance through relational leadership is complementary or rather a substitute to formal contracts in the context of such business-to-business partnerships. A case study-based research design is employed to explore relational leadership in business partnerships in India, thereby incorporating case studies based on interviews from nine internationally operating corporations. A process framework for relational leadership with six distinct steps on how to develop business partnerships in India was developed. Furthermore, the researchers found that the framework complements the relational governance processes supported by relational leadership and formal contracts when engaging in business partnerships in India. The study’s main aim was to contribute to the current theory in the emergent field of relational leadership. Practitioners responsible for partnership building among corporations can gain insights from the framework into the application of relational leadership. The results indicate that corporations can maintain long-term partnerships if specific relational governance mechanisms mainly supported by the application of relational leadership are in place.
Kochen-Specker Sets with a Mixture of 16 Rank-1 and 14 Rank-2 Projectors for a Three-Qubit System

Kochen—Specker (KS) theorem denies the possibility for the noncontextual hidden variable theories to reproduce the predictions of quantum mechanics. A set of projection operators (projectors) and bases used to show the impossibility of noncontextual definite values assignment is named as the KS set. Since one KS set with a mixture of 16 rank-1 projectors and 14 rank-2 projectors was proposed in 1995 [Kernaghan M and Peres A Phys. Lett. A 198 (1995) 1] for a three-qubit system, there have been plenty of the same type KS sets and we propose a systematic way to produce them. We also propose a probabilistic state-dependent proof of the KS theorem that mainly focuses on the values assignment for all the rank-2 projectors.
THE QUANTITY OF INTRACLUSTER LIGHT: COMPARING THEORETICAL AND OBSERVATIONAL MEASUREMENT TECHNIQUES USING SIMULATED CLUSTERS

Using a suite of N-body simulations of galaxy clusters specifically tailored to studying the intracluster light (ICL) component, we measure the quantity of ICL using a number of different methods previously employed in the literature for both observational and simulation data sets. By measuring the ICL of the clusters using multiple techniques, we are able to identify systematic differences in how each detection method identifies the ICL. We find that techniques which define the ICL solely based on the current position of the cluster luminosity, such as a surface brightness or local density threshold, tend to find less ICL than methods utilizing time or velocity information, including stellar particles’ density history or binding energy. The range of ICL fractions (the fraction of the clusters’ total luminosity found in the ICL component) we measure at z = 0 across all our clusters using any definition spans the range 9%–36%, and even within a single cluster different methods can change the measured ICL fraction by up to a factor of two. Separating the cluster's central galaxy from the surrounding ICL component is a challenge for all ICL techniques, and because the ICL is centrally concentrated within the cluster, the differences in the measured ICL quantity between techniques are largely a consequence of this central galaxy/ICL separation. We thoroughly explore the free parameters involved with each measurement method, and find that adjusting these parameters can change the measured ICL fraction by up to a factor of two. The choice of ICL definition does not strongly affect the ICL's ability to trace the major features of the cluster's dynamical evolution. While for all definitions the quantity of ICL tends to increase with time, the ICL fraction does not grow at a uniform rate, nor even monotonically under some definitions. Thus, the ICL can be used as a rough indicator of dynamical age, where more dynamically advanced clusters will on average have higher ICL fractions.
A REDSHIFT FOR THE INTERMEDIATE-MASS BLACK HOLE CANDIDATE HLX-1: CONFIRMATION OF ITS ASSOCIATION WITH THE GALAXY ESO 243-49

In this Letter, we report a spectroscopic confirmation of the association of HLX-1, the brightest ultra-luminous X-ray (ULX) source, with the galaxy ESO 243-49. At the host galaxy distance of 95 Mpc, the maximum observed 0.2–10 keV luminosity is 1.2 × 1042 erg s−1. This luminosity is ∼400 times above the Eddington limit for a 20 M☉ black hole and has been interpreted as implying an accreting intermediate-mass black hole with a mass in excess of 500 M☉ (assuming that the luminosity is a factor of 10 above the Eddington value). However, a number of other ULX sources have been later identified as background active galaxies or foreground sources. It has recently been claimed that HLX-1 could be a quiescent neutron star X-ray binary at a Galactic distance of only 2.5 kpc, so a definitive association with the host galaxy is crucial in order to confirm the nature of the object. Here, we report the detection of the Hα emission line for the recently identified optical counterpart at a redshift consistent with that of ESO 243-49. This finding definitively places HLX-1 inside ESO 243-49, confirming the extreme maximum luminosity and strengthening the case for it containing an accreting intermediate-mass black hole of more than 500 M☉.
FORMATION AND EVOLUTION OF THE DISK SYSTEM OF THE MILKY WAY: [α/Fe] RATIOS AND KINEMATICS OF THE SEGUE G-DWARF SAMPLE

We employ measurements of the [α/Fe] ratio derived from low-resolution (R ∼ 2000) spectra of 17,277 G-type dwarfs from the SEGUE survey to separate them into likely thin- and thick-disk subsamples. Both subsamples exhibit strong gradients of orbital rotational velocity with metallicity, of opposite signs, −20 to −30 km s−1 dex−1 for the thin-disk and +40 to +50 km s−1 dex−1 for the thick-disk population. The rotational velocity is uncorrelated with Galactocentric distance for the thin-disk subsample and exhibits a small trend for the thick-disk subsample. The rotational velocity decreases with distance from the plane for both disk components, with similar slopes (−9.0 ± 1.0 km s−1 kpc−1). Thick-disk stars exhibit a strong trend of orbital eccentricity with metallicity (about −0.2 dex−1), while the eccentricity does not change with metallicity for the thin-disk subsample. The eccentricity is almost independent of Galactocentric radius for the thin-disk population, while a marginal gradient of the eccentricity with radius exists for the thick-disk population. Both subsamples possess similar positive gradients of eccentricity with distance from the Galactic plane. The shapes of the eccentricity distributions for the thin- and thick-disk populations are independent of distance from the plane, and include no significant numbers of stars with eccentricity above 0.6. Among several contemporary models of disk evolution that we consider, radial migration appears to have played an important role in the evolution of the thin-disk population, but possibly less so for the thick disk, relative to the gas-rich merger or disk heating scenarios. We emphasize that more physically realistic models and simulations need to be constructed in order to carry out the detailed quantitative comparisons that our new data enable.
Revista Mexicana de Biodiversidad

Cambarellus chapalanus is an endemic species of the area around Lake Chapala in Mexico and knowledge about its biology and ecology is scarce. Its population dynamics were evaluated based on individual growth, mortality, production, and productivity. For this, individuals were collected between November 2011 and October 2012
From cosmic ray source to the Galactic pool

The Galactic cosmic ray spectrum is a remarkably straight power law. Our current understanding is that the dominant sources that accelerate cosmic rays up to the knee ($3 \times 10^{15}$ eV) or perhaps even the ankle ($3 \times 10^{18}$ eV), are young Galactic supernova remnants. In theory, however, there are various reasons why the spectrum may be different for different sources, and may not even be a power law if nonlinear shock acceleration applies during the most efficient stages of acceleration. We show how the spectrum at the accelerator translates to the spectrum that make up the escaping cosmic rays that replenish the Galactic pool of cosmic rays. We assume that cosmic ray confinement, and thus escape, is linked to the level of magnetic field amplification, and that the magnetic field is amplified by streaming cosmic rays according to the non-resonant hybrid or resonant instability. When a fixed fraction of the energy is transferred to cosmic rays, it turns out that a source spectrum that is flatter than $E^{-2}$ will result in a $E^{-2}$ escape spectrum, whereas a steeper source spectrum will result in an escape spectrum with equal steepening. This alleviates some of the concern that may arise from expected flat or concave cosmic ray spectra associated with nonlinear shock modification.
Caustic formation in expanding condensates of cold atoms

We study the evolution of density in an expanding Bose-Einstein condensate that initially has a spatially varying phase, concentrating on behavior when these phase variations are large. In this regime large density fluctuations develop during expansion. Maxima have a characteristic density that diverges with the amplitude of phase variations and their formation is analogous to that of caustics in geometrical optics. We analyze in detail caustic formation in a quasi-one-dimensional condensate, which before expansion is subject to a periodic or random optical potential, and we discuss the equivalent problem for a quasi-two-dimensional system. We also examine the influence of many-body correlations in the initial state on caustic formation for a Bose gas expanding from a strictly one-dimensional trap. In addition, we study a similar arrangement for noninteracting fermions, showing that Fermi surface discontinuities in the momentum distribution give rise in that case to sharp peaks in the spatial derivative of the density. We discuss recent experiments and argue that fringes reported in time of flight images [Chen et al., Phys. Rev. A 77, 033632 (2008)] are an example of caustic formation.
PROBING THE PROTOSTELLAR ENVELOPE AROUND L1157: THE DUST AND GAS CONNECTION

We present observations of the Class 0 protostar L1157-mm using the Combined Array for Research in Millimeter-wave Astronomy (CARMA) in 3 mm dust continuum and N2H+ line emission. In the N2H+ line, we detect a large-scale envelope extended over a linear size of ∼20,000 AU flattened in the direction perpendicular to the outflow. This N2H+ feature coincides with the outer envelope seen in the 8 μm extinction by Looney et al. Meanwhile, the dust continuum traces the compact, nearly spherical structure of the inner envelope, where N2H+ becomes depleted. This highly flattened N2H+ envelope also shows dynamical signatures consistent with gravitational infall in the inner region, but a slow, solid-body rotation at large scales. This flattened structure is not a rotationally supported circumstellar disk; instead, it resembles a prestellar core both morphologically and kinematically, representing the early phase of a Class 0 system. In this paper, we construct a simple model to interpret both the dust continuum and N2H+ emission and suggest a possible dynamical scenario for the overall properties of the envelope.
A low-luminosity type-1 QSO sample: II. Tracing circumnuclear star formation in HE 1029-1831 with SINFONI

Circumnuclear star formation and AGN feedback is believed to play a critical role in the context of galaxy evolution. The low-luminosity QSO (LLQSO) sample that contains 99 of the closest AGN with redshift z<=0.06 fills the gap between the local AGN population and high-redshift QSOs that is essential to understand the AGN evolution with redshift. In this paper, we present the results of near-infrared H+K-integral field spectroscopy of the inner kiloparsecs of the LLQSO HE 1029-1831 with SINFONI. Line maps show that ionized hydrogen gas is located in spiral arms within the stellar bar and in a circumnuclear ring. Line fluxes and diagnostic line ratios indicate recent or ongoing star formation in the circumnuclear region and the presence of young and intermediate-age stellar populations in the bulge. In particular, we find traces of an intense starburst in the circumnuclear region that has begun around 100 Myr ago but has declined to a fraction of the maximum intensity now. We estimate the dynamical bulge mass and find that the galaxy follows published M_BH-M_bulge relations. However, bulge-disk decomposition of the K-band image with BUDDA reveals that HE 1029-1831 does not follow the M_BH-L_bulge relations of inactive galaxies. We conclude that the deviation from M_BH-L_bulge relations of inactive galaxies in this source is rather caused by young stellar populations and not by an undermassive black hole.
The Moderating Effect of Firm Characteristics on the Relationship between Accounting Conservatism and Treasury Stocks: Evidence from Firms Listed on the Saudi Stock Exchange

: This research aims to investigate the relationship between accounting conservatism and treasury stocks. The current research examines the potential influence of firm-specific characteristics as moderating variables on this relationship. Ordinary least squares regression and multiple regressions are used to test the research hypotheses. The study sample consists of 13 non-financial firms listed on the Saudi Stock Exchange during 2018–2020, resulting in a final sample of 39 firm-year observations. The researcher concludes that accounting conservatism has a significant and negative effect on treasury stocks. In addition, the negative effect of accounting conservatism on treasury stocks is strengthened in the presence of firm size, leverage ratio and return on assets as moderating variables. These findings are robust, as the results of the sensitivity analysis support those of the fundamental analysis. To the best of the researcher’s knowledge, there is relatively limited evidence, in previous studies relating to accounting conservatism and its association with treasury stocks in the presence of firm characteristics as moderating variables. Furthermore, the findings of this research have implications for researchers and regulatory bodies that seek to enhance the quality of financial statements in emerging economies.
Quantifying galactic morphological transformations in the cluster environment

We study the effects of the cluster environment on galactic morphology by defining a dimensionless angular momentum parameter, λd, to obtain a quantitative and objective measure of galaxy type. The use of this physical parameter allows us to take the study of morphological transformations in clusters beyond the measurements of merely qualitative parameters, e.g. spiral/elliptical (S/E) ratios, to a more physical footing. To this end, we employ an extensive Sloan Digital Sky Survey sample (Data Release 7) with galaxies associated with Abell galaxy clusters. The sample contains 121 relaxed Abell clusters and over 51 000 individual galaxies, which guarantees a thorough statistical coverage over a wide range of physical parameters. We find that the median λd value tends to decrease as we approach the cluster centre, with different dependences according to the mass of the galaxies and the hosting cluster; low- and intermediate-mass galaxies show a strong dependence, while massive galaxies seem to show, at all radii, low λd values. By analysing trends in λd as functions of the nearest neighbour environment, clustercentric radius and velocity dispersion of clusters, we can identify clearly the leading physical processes at work. We find that in massive clusters ( σ> 700 km s −1 ), the interaction with the cluster central region dominates, whilst in smaller clusters galaxy–galaxy interactions are chiefly responsible for driving galactic morphological transformations.
X-RAY MONITORING OF GRAVITATIONAL LENSES WITH CHANDRA

We present Chandra monitoring data for six gravitationally lensed quasars: QJ 0158−4325, HE 0435−1223, SDSS 0924+0219, SDSS 1004+4112, HE 1104−1805, and Q 2237+0305. X-ray microlensing variability is detected in all six lenses with high confidence. We furthermore detect energy-dependent microlensing in HE 0435−1223, SDSS 0924+0219, SDSS 1004+4112, and Q 2237+0305. Through a detailed spectral analysis for each lens we find that simple power-law models plus Gaussian emission lines give good fits to the spectra. We detect intrinsic spectral variability in two epochs of Q 2237+0305, and differential absorption between images in QJ 0158−4325 and Q2237+0305. We also detect the Fe Kα emission line in all six lenses, and the Ni xxvii Kα line in two images of Q 2237+0305. The rest-frame equivalent widths of the Fe Kα lines are measured to be 0.4–1.2 keV, significantly higher than those measured in typical active galactic nuclei of similar X-ray luminosities. This suggests that the Fe Kα emission region is more compact or centrally concentrated than the continuum emission region.
The impact of galaxy formation on the total mass, mass profile and abundance of haloes

We use cosmological hydrodynamical simulations to investigate how the inclusion of physical processes relevant to galaxy formation (star formation, metal-line cooling, stellar winds, supernovae and feedback from Active Galactic Nuclei, AGN) change the properties of haloes, over four orders of magnitude in mass. We find that gas expulsion and the associated dark matter (DM) expansion induced by supernova-driven winds are important for haloes with masses M200 < 10^13 Msun, lowering their masses by up to 20% relative to a DM-only model. AGN feedback, which is required to prevent overcooling, has a significant impact on halo masses all the way up to cluster scales (M200 ~ 10^15 Msun). Baryonic physics changes the total mass profiles of haloes out to several times the virial radius, a modification that cannot be captured by a change in the halo concentration. The decrease in the total halo mass causes a decrease in the halo mass function of about 20%. This effect can have important consequences for abundance matching technique as well as for most semi-analytic models of galaxy formation. We provide analytic fitting formulae, derived from simulations that reproduce the observed baryon fractions, to correct halo masses and mass functions from DM-only simulations. The effect of baryonic physics (AGN feedback in particular) on cluster number counts is about as large as changing the cosmology from WMAP7 to Planck, even when a moderately high mass limit of M500 ~ 10^14 Msun is adopted. Thus, for precision cosmology the effects of baryons must be accounted for.
The merger Seyfert galaxy Arp 220: line and continuum absorption and emission

The line and continuum spectra of the merger galaxy Arp 220 are analysed with the aim of investigating the ionizing and heating sources. We refer to radio, optical, infrared and X-ray spectra. The results show that in agreement with other merger galaxies, the optical lines are emitted from gas photoionised by the AGN and heated by the shocks in the extended NLR. The infrared lines are better explained by the emission from gas close to the starburst. The starburst dominates the infrared emission. [OI] and [CI] lines in the far-infrared are formed in the internal region of extended clouds and are therefore absorbed, while [CII] lines are emitted from the external edges of outflowing clouds. The O/H relative abundances are about solar and N/H are higher than solar by a factor of 1.5, throughout the starburst region, while in the AGN extended NLR the O/H ratio is half solar. A relatively high dust-to-gas ratio is indicated by modelling the dust reprocessed radiation peak consistently with bremsstrahlung emitted from the clouds. The observed radio emission is thermal bremsstrahlung, while synchrotron radiation created by the Fermi mechanism at the shock front is absorbed.
Perturbation theory approach for the power spectrum: from dark matter in real space to massive haloes in redshift space

We investigate the accuracy of Eulerian perturbation theory for describing the matter and galaxy power spectra in real and redshift space in light of future observational probes for precision cosmology. Comparing the analytical results with a large suite of N-body simulations (160 independent boxes of 13.8 (Gpc/h){sup 3} volume each, which are publicly available), we find that re-summing terms in the standard perturbative approach predicts the real-space matter power spectrum with an accuracy of ∼<2% for k ≤ 0.20 h/Mpc at redshifts z∼<1.5. This is obtained following the widespread technique of writing the resummed propagator in terms of 1-loop contributions. We show that the accuracy of this scheme increases by considering higher-order terms in the resummed propagator. By combining resummed perturbation theories with several models for the mappings from real to redshift space discussed in the literature, the multipoles of the dark-matter power spectrum can be described with sub-percent deviations from N-body results for k ≤ 0.15 h/Mpc at z∼<1. As a consequence, the logarithmic growth rate, f, can be recovered with sub-percent accuracy on these scales. Extending the models to massive dark-matter haloes in redshift space, our results describe the monopole term from N-body data within 2% accuracy formore » scales k ≤ 0.15 h/Mpc at z∼<0.5; here f can be recovered within < 5% when the halo bias is known. We conclude that these techniques are suitable to extract cosmological information from future galaxy surveys. « less
Sciatic Histological, Ultrastructural and Biochemical Investigations on Improving the Effect of Pregabalin by Flaxseed Oil on Diabetic Peripheral Neuropathy Induced in Albino Rats

Background : The most common complication of diabetes mellitus is peripheral diabetic neuropathy associated with neurodegenerative effects. Food and Drug Association approved pregabalin as an anticonvulsant drug, for the treatment of diabetic neuropathy. There were many studies that reported no interest in the effect of this drug because it did not achieve complete recovery of diabetic neuropathy. So, this study aimed to improve toxicity in rats: hematological, biochemical, and histopathological study.