Miracle-dz/UniFAR-FTUs huggingface dataset:
Mass profiles and concentration-dark matter relation in X-ray luminous galaxy clusters

Context. Galaxy clusters represent valuable cosmological probes us ing tests that mainly rely on measurements of cluster masses and baryon fractions. X-ray observations represent one of the m ain tools for uncovering these quantities. Aims. We aim to constrain the cosmological parameters Ωm andσ8 using the observed distribution of the both values of the con centrations and dark mass within R200 and of the gas mass fraction within R500. Methods. We applied two different techniques to recover the profiles t he gas and dark mass, described according to the Navarro, Frenk & White (1997, ApJ, 490, 493) functional form, of a samp le of 44 X-ray luminous galaxy clusters observed with XMM-Newton in the redshift range0.1− 0.3. We made use of the spatially resolved spectroscopic data an d of the PSF–deconvolved surface brightness and assumed that hydrostatic equilibrium holds betwee n the intracluster medium and the gravitational potential. We evaluated several systematic uncertainties that affect our reconstr uction of the X-ray masses. Results. We measured the concentration c200, the dark massM200 and the gas mass fraction in all the objects of our sample, pro viding the largest dataset of mass parameters for galaxy clu sters in the redshift range 0.1 − 0.3. We confirm that a tight correlation betweenc200 andM200 is present and in good agreement with the predictions from nu erical simulations and previous observations. When we consider a subsample of relaxed clusters that host a l w entropy core, we measure a flatter c − M relation with a total scatter that is lower by 40 per cent. We conclude, however, th at the slope of thec−M relation cannot be reliably determined from the fitting over a narrow mass range as the one considered in the pr es nt work. From the distribution of the estimates of c200 andM200, with associated statistical (15–25%) and systematic (5–15 %) errors, we used the predicted values from semi-analytic p rescriptions calibrated through N-body numerical runs and obtain σ8 Ω m = 0.45 ± 0.01 (at 2σ level, statistical only) for the subsample of the clusters where the mass reconstruction has been obtai ned more robustly and σ8 Ω m = 0.39 ± 0.02 for the subsample of the 11 more relaxed LEC objects. With the further constrai n from the gas mass fraction distribution in our sample, we b reak the degeneracy in the σ8 − Ωm plane and obtain the best-fit values σ8 ≈ 1.0± 0.2 (0.83± 0.1 when the subsample of the more relaxed objects is considered) and Ωm = 0.26 ± 0.02. Conclusions. We demonstrate that the analysis of the distribution of the c200 −M200 − fgas values represents a mature and competitive technique in the present era of precision cosmology, e ven though it needs more detailed analysis of the output of la rger sets of cosmological numerical simulations to provide definitive a nd robust results.
Assessment of Zinc, Boron, and Iron Foliar Application on Wheat Yield and Yield Components Under Drought Stress

ABSTRACT While eliminating their deficiency, leaf consumption of micronutrients enhances the quantitative and qualitative yield of the plant. To examine the impact of irrigation regimes and foliar application of zinc, boron, and iron on wheat yield and yield components, an experiment was conducted in the form of split plots in Varamin (Iran) over two crop years 2016–17 and 2017–18. The main factor of irrigation regimes included three levels (Tr: regular irrigation, Ts: irrigation interruption at the onset of stem growth and Tss: irrigation interruption at the onset of stem growth and seed filling) and the secondary factor included foliar application of micronutrients at eight levels (MC: control), MB: foliar application of boron (B), MZ: zinc (Zn), MI: iron (Fe), MZB: Zn + B, MBI: Fe + B, MZI: Zn + Fe and MZBI: Zn + B + Fe). Irrigation interruption at the onset of stem growth and seed filling (Tss) led to a significant reduction in seed yield and its components. With an average of 6788 kg ha−1, the highest seed yield belonged to normal irrigation treatment. With an average of 6549 kg ha−1, Fe + Zn + B treatment had the highest seed yield, indicating a 17% increase compared to the control treatment. Given the positive effect of iron, zinc, and boron micronutrients on wheat agronomic characteristics, these treatments under normal irrigation and drought stress conditions are suggested to be applied for the development of wheat cultivation in cold temperate areas with semi-arid climate.
ON THE (NON-)ENHANCEMENT OF THE Lyα EQUIVALENT WIDTH BY A MULTIPHASE INTERSTELLAR MEDIUM

It has been suggested that radiative transfer effects may explain the unusually high equivalent widths (EWs) of the Lyα line, observed occasionally from starburst galaxies, especially at high redshifts. If the dust is locked up inside high-density clouds dispersed in an empty intercloud medium, the Lyα photons could scatter off of the surfaces of the clouds, effectively having their journey confined to the dustless medium. The continuum radiation, on the other hand, does not scatter, and would thus be subject to absorption inside the clouds. This scenario is routinely invoked when Lyα EWs higher than what is expected theoretically are observed, although the ideal conditions under which the results are derived usually are not considered. Here we systematically examine the relevant physical parameters in this idealized framework, testing whether any astrophysically realistic scenarios may lead to such an effect. It is found that although clumpiness indeed facilitates the escape of Lyα, it is highly unlikely that any real interstellar media should result in a preferential escape of Lyα over continuum radiation. Other possible causes are discussed, and it is concluded that the observed high EWs are more likely to be caused by cooling radiation from cold accretion and/or anisotropic escape of the Lyα radiation.
Development and Testing a Method for Retrieving Atmospheric Aerosol Optical Thickness based on the Solar Intensity from the Sun-photometer Data

The context of atmospheric aerosols is an indispensable aspect in studying the Earth’s radiation budget, climate change, and air quality. Therefore, the quality technique in retrieving aerosol parameters is important for a better understanding their characteristics. The precise calculating of the aerosol physical parameter in the planetary boundary layer will increase the accuracy of evaluation of their impact on environmental conditions. In several atmospheric corrections of optical remote sensing using satellite sensors, the AOT’s values play an important role in arranging a Look Up Table (LUT) for scattering parameters. Therefore, this study aims to develop a method for processing and correcting the sun-photometer data to obtain the original AOT in the planetary boundary layer. In AOT calculation using the sun-photometer data, the solar radiation at the extraterritorial of the atmosphere is determined using the Langley plot. Then, using the target data at the same season as the data for the Langley plot, the temporal change of AOT is estimated by employing the Lambert-Beer Law with some corrections. The major correction for the AOT’s values computation in the measurement target is the contribution of molecule from the local station and Ozone (O3) from the GOME-2 satellite data. The result has been compared with an independent measurement using a sky-radiometer at the same time as the sun-photometer monitoring. From the overall procedure, the AOT’s values have uncertainties at approximately 2-5% compared to the sky-radiometer. Therefore, the procedure will be useful for studying aerosol optical properties in the lower troposphere.
Panchromatic properties of galaxies in wide-field optical spectroscopic and photometric surveys

Abstract The past 15 years have seen an explosion in the number of redshifts recovered via wide area spectroscopic surveys. At the current time there are approximately 2 million spectroscopic galaxy redshifts known (and rising) which represents an extraordinary growth since the pioneering work of Marc Davis and John Huchra. Similarly there has been a parallel explosion in wavelength coverage with imaging surveys progressing from single band, to multi-band, to truly multiwavelength or pan-chromatic involving the coordination of multiple facilities. With these empirically motivated studies has come a wealth of new discoveries impacting almost all areas of astrophysics. Today individual surveys, as best demonstrated by the Sloan Digital Sky Survey, now rank shoulder-to-shoulder alongside major facilities. In the coming years this trend is set to continue as we begin the process of designing and conducting the next generation of spectroscopic surveys supported by multi-facility wavelength coverage.
The long-term evolution of photoevaporating transition discs with giant planets

Photo-evaporation and planet formation have both been proposed as mechanisms responsible for the creation of a transition disc. We have studied their combined effect through a suite of 2d simulations of protoplanetary discs undergoing X-ray photoevaporation with an embedded giant planet. In a previous work we explored how the formation of a giant planet triggers the dispersal of the inner disc by photo-evaporation at earlier times than what would have happened otherwise. This is particularly relevant for the observed transition discs with large holes and high mass accretion rates that cannot be explained by photo-evaporation alone. In this work we significantly expand the parameter space investigated by previous simulations. In addition, the updated model includes thermal sweeping, needed for studying the complete dispersal of the disc. After the removal of the inner disc the disc is a non accreting transition disc, an object that is rarely seen in observations. We assess the relative length of this phase, to understand if it is long lived enough to be found observationally. Depending on the parameters, especially on the X-ray luminosity of the star, we find that the fraction of time spent as a non-accretor greatly varies. We build a population synthesis model to compare with observations and find that in general thermal sweeping is not effective enough to destroy the outer disc, leaving many transition discs in a relatively long lived phase with a gas free hole, at odds with observations. We discuss the implications for transition disc evolution. In particular, we highlight the current lack of explanation for the missing non-accreting transition discs with large holes, which is a serious issue in the planet hypothesis.
A coherent understanding of low-energy nuclear recoils in liquid xenon

Liquid xenon detectors such as XENON10 and XENON100 obtain a significant fraction of their sensitivity to light (10 GeV) particle dark matter by looking for nuclear recoils of only a few keV, just above the detector threshold. Yet in this energy regime a correct treatment of the detector threshold and resolution remains unclear. The energy dependence of the scintillation yield of liquid xenon for nuclear recoils also bears heavily on detector sensitivity, yet numerous measurements have not succeeded in obtaining concordant results. In this article we show that the ratio of detected ionization to scintillation can be leveraged to constrain the scintillation yield. We also present a rigorous treatment of liquid xenon detector threshold and energy resolution. Notably, the effective energy resolution differs significantly from a simple Poisson distribution. We conclude with a calculation of dark matter exclusion limits, and show that existing data from liquid xenon detectors strongly constrain recent interpretations of light dark matter.
Localization and reference frames in 
κ
-Minkowski spacetime

We study the limits to the localizability of events and reference frames in the $\kappa$-Minkowski quantum spacetime. Our main tool will be a representation of the $\kappa$-Minkowski commutation relations between coordinates, and the operator and measurement theory borrowed from ordinary quantum mechanics. Spacetime coordinates are described by operators on a Hilbert space, and a complete set of commuting observables cannot contain the radial coordinate and time at the same time. The transformation between the complete sets turns out to be the Mellin transform, which allows us to discuss the localizability properties of states both in space and time. We then discuss the transformation rules between inertial observers, which are described by the quantum $\kappa$-Poincar\'e group. These too are subject to limitations in the localizability of states, which impose further restrictions on the ability of an observer to localize events defined in a different observer's reference frame.
The black holes of radio galaxies during the “Quasar Era”: masses, accretion rates, and evolutionary stage

We present an analysis of the AGN broad-line regions of 6 powerful radio galaxies at z ∼ 2 (HzRGs), which is part of a study of a sample of 50 HzRGs with rest-frame optical imaging spectroscopy obtained at the VLT. In 6 galaxies we detect luminous (L(Hα) = few x 10 44 erg s ―1 ), spatially unresolved, broad (FWHM ≥ 10 000 km s ―1 ) Hα line emission from the nucleus (HαBLRs), consistent with broad-line regions of supermassive black holes with masses of few x 10 9 M ⊙ and accretion luminosities of a few percent of the Eddington luminosity. In two galaxies we also detect HβBLRs, suggesting relatively low extinction of A V ∼ 1 mag, which agrees with constraints from X-ray observations. Overall, we find HαBLRs in ∼20% of the galaxies where Hα is observed. By relating black hole and bulge mass, we find a possible offset towards higher black-hole masses of at most ∼0.6 dex relative to nearby galaxies at a given host mass, although each individual galaxy is within the scatter of the local relationship. If not entirely from systematic effects, this would then suggest that the masses of the host galaxies have increased by at most a factor ≈4 since z ∼ 2 relative to the black-hole masses, perhaps through accretion of satellite galaxies or because of a time lag between star formation in the host galaxy and AGN fueling. We also compare the radiative and mechanical energy output (from jets) of our targets with predictions of recent models of "synthesis" or "grand unified" AGN feedback, which postulate that AGN with similar radiative and mechanical energy output rates to those found in our HzRGs may be nearing the end of their period of active growth. We discuss evidence that they may reach this stage at the same time as their host galaxies.
Spectroscopy of V341 Arae: A Nearby Nova-like Variable Inside a Bow Shock Nebula

V341 Arae is a 10th-magnitude variable star in the southern hemisphere, discovered over a century ago by Henrietta Leavitt, but relatively little studied since then. Although historically considered to be a Cepheid, it is actually blue and coincides with an X-ray source. The star lies near the edge of the large, faint Hα nebula Fr 2–11, discovered by D. Frew, who showed that V341 Ara is actually a cataclysmic variable (CV). His deep imaging of the nebula revealed a bow-shock morphology in the immediate vicinity of the star. We have carried out spectroscopic monitoring of V341 Ara, and we confirm that it is a nova-like CV, with an orbital period of 0.15216 days (3.652 hr). We show that V341 Ara is remarkably similar to the previously known BZ Cam, a nova-like CV with a nearly identical orbital period, associated with the bow shock nebula EGB 4. Archival sky-survey photometry shows that V341 Ara normally varies between V ≃ 10.5 and 11, with a characteristic timescale ranging from about 10 to 16 days. V341 Ara lies well off-center within Fr 2–11. We speculate that either the star is undergoing a chance high-speed encounter with a small interstellar cloud, or that the nebula was ejected from the star itself in a nova outburst in the fairly distant past. At a distance of only 156 pc, V341 Ara is one of the nearest and brightest known nova-like variables, and we encourage further studies.
High-mass Outflows Identified from COHRS CO (3–2) Survey

An unbiased search of molecular outflows within the region of the CO High Resolution survey has identified 157 high-mass outflows from a sample of 770 APEX Telescope Large Area Survey of the Galaxy clumps with a detection rate of 20%. The detection rate of outflows increases for clumps with higher Mclump, Lbol, Lbol/Mclump, N H 2 , and Tdust compared to the clumps with no outflow. The detection rates of the outflow increase from protostellar (8%) to young stellar object clump (17%) to massive star-forming clump (29%). The detection rate 26% for quiescent clump is preliminary, because the sample of quiescent clumps is small. A statistical relation between the outflow and clump masses for our sample is log ( M out / M ⊙ ) = ( − 1.1 ± 0.21 ) + ( 0.9 ± 0.07 ) log ( M clump / M ⊙ ) . The detection rate of outflows and the outflow mass-loss rate show an increase with increasing Mclump, Lbol, N H 2 , and Tdust, which indicates that clumps with outflow with higher parameter values are at a more advanced evolutionary stage. The outflow mechanical force increases with increasing bolometric luminosities. No clear evidence has yet been found that higher-mass outflows have different launching conditions than low-mass outflows.
THE HARD X-RAY SHORTAGES PROMPTED BY THE CLOCK BURSTS IN GS 1826–238

We report on a study of GS 1826–238 using all available Rossi X-Ray Timing Explorer observations, concentrating on the behavior of the hard X-rays during type-I bursts. We find a hard X-ray shortage at 30–50 keV prompted by the shower of soft X-rays coming from type-I bursts. This shortage happens with a time delay after the peak of the soft flux of 3.6 ± 1.2 s. The behavior of hard X-rays during bursts indicates cooling and reheating of the corona, during which a large amount of energy is required. We speculate that this energy originates from the feedback of the type-I bursts to the accretion process, resulting in a rapid temporary increase of the accretion rate.
The Influence of Protean Career Attitude, Passion for Work, and Self-Management on Proactive Work Behavior in the Millennial Generation

This research's background is the phenomenon of drastic changes in the work environment due to the pandemic, the high number of millennial generation employees, and many employees in control of their careers. This study aims to analyze the effect of Protean Career Attitude, Passion for Work, and Self-Management on Proactive Work Behavior in the millennial generation. The number of respondents is 92 people. The research approach used is descriptive. The population in this study were all employees at PT Satria Parang Tritis, totaling 120 employees. The sample used in this study was 92 respondents. The sampling technique is purposive sampling. The method of data analysis is multiple linear regression. The results of the partial study, Protean Career Attitude has a positive and significant effect on Proactive Work Behavior) with a t-count value of 2.485 > t-table 1.986 and a sig value of 0.015 <0.05. Passion For work has a positive and significant effect on Proactive Work Behavior with a value of t-count 4.220 > t-table 1.986 and sig value 0.000 <0.05. Self-Management positively and significantly affects Proactive Work Behavior with t-count value 2.323 > t-table 1.986 and sig value 0.022 <0.05 in generation millennials at PT Satria Parang Tritis. Simultaneously, Protean Career Attitude, Passion For Work, and self-management positively and significantly affect Proactive Work Behavior in the millennial generation at PT Satria Parang Tritis.
The very-high-energy gamma-ray view of the Galactic Centre as of early 2010

Progress in the Imaging Atmospheric Cherenkov Technique has enabled first sensitive observations of the innermost few 100 pc of the Milky Way in Very High Energy (VHE; >100 GeV) gamma rays. Observations by the H.E. S.S. instrument deliver the at date most precise data on this peculiar region, and provide an interesting view onto the acceleration and propagation of energetic particles near the Galactic Centre. Besides two point-like sources -- one coincident with the supermassive black hole (SMBH) Sgr A* -- diffuse VHE emission has been discovered within a 1 deg region around the centre. The current VHE gamma-ray view of the region is reviewed, and possible counterparts of the gamma-ray sources and the origin of the diffuse emission are discussed.
A MULTI-WAVELENGTH LOOK AT THE YOUNG PLERIONIC SUPERNOVA REMNANT 0540-69.3

We present a study of the plerionic supernova remnant 0540-69.3 in the LMC in X-ray, radio, optical, and infrared. We find that the shell of 0540-69.3 is characterized in the X-ray by thermal nonequilibrium plasma with depleted Mg and Si abundances and a temperature of kT ∼ 0.7 keV. This thermal emission is superimposed with synchrotron emission in several regions. Based on X-ray spectra and on morphological considerations in all surveyed wavebands, we conclude that the shell is expanding into a clumpy and highly inhomogeneous medium. In one region of the shell we find an overabundance of Ne, suggesting the presence of ejecta near the edge of the remnant. We also see evidence for reheating of material via a reverse shock originating from the interaction of the supernova blast wave with a particularly dense cloud in the surrounding medium. Finally, we perform the first detailed study of the “halo” region extending 1.2–2.2 pc from the central pulsar. We detect the presence of thermal and nonthermal spectral components but do not find evidence for mixing or ejecta. We conclude that the thermal component is not a counterpart to similar optical and infrared halos and that it is most likely due to the projection of shell material along the line of sight.
Occupational Preferences of Skilled Workers in the Presence of a Large Development Sector

Abstract Aid and the resulting development sector have expanded in developing countries in the past decades. Many studies have explored the effects of aid, but few have studied the effects of the development sector on decisions around labor supply and occupational choice. Using primary data from Sierra Leone, this article contributes to the literature by exploring how the presence of a large development sector influences the occupational preferences of skilled workers. Four key findings emerge. First, the development sector is an attractive employment choice as the largest share of skilled jobseekers (44 percent) opt for early-career employment working for a donor organization, international NGO or local NGO. Second, there is an ability-effect as workers with higher cognitive ability are more likely to choose the development sector over the public and private sectors. Third, more prosocial jobseekers and those seeking social status from employment are more likely to prefer the development sector. And fourth, favorable perceptions of the development sector reduce the probability of choosing the public and private sectors. These findings speak to policy and should encourage development organizations to reflect on their impact on the dynamics of the labor market in countries in which they operate.