Miracle-dz/UniFAR-FTUs huggingface dataset:
Finding counterparts for All-sky X-ray surveys with Nway: a Bayesian algorithm for cross-matching multiple catalogues

We release the AllWISE counterparts and Gaia matches to 106,573 and 17,665 X-ray sources detected in the ROSAT 2RXS and XMMSL2 surveys with |b|>15. These are the brightest X-ray sources in the sky, but their position uncertainties and the sparse multi-wavelength coverage until now rendered the identification of their counterparts a demanding task with uncertain results. New all-sky multi-wavelength surveys of sufficient depth, like AllWISE and Gaia, and a new Bayesian statistics based algorithm, NWAY, allow us, for the first time, to provide reliable counterpart associations. NWAY extends previous distance and sky density based association methods and, using one or more priors (e.g., colors, magnitudes), weights the probability that sources from two or more catalogues are simultaneously associated on the basis of their observable characteristics. Here, counterparts have been determined using a WISE color-magnitude prior. A reference sample of 4524 XMM/Chandra and Swift X-ray sources demonstrates a reliability of ~ 94.7% (2RXS) and 97.4% (XMMSL2). Combining our results with Chandra-COSMOS data, we propose a new separation between stars and AGN in the X-ray/WISE flux-magnitude plane, valid over six orders of magnitude. We also release the NWAY code and its user manual. NWAY was extensively tested with XMM-COSMOS data. Using two different sets of priors, we find an agreement of 96% and 99% with published Likelihood Ratio methods. Our results were achieved faster and without any follow-up visual inspection. With the advent of deep and wide area surveys in X-rays (e.g. SRG/eROSITA, Athena/WFI) and radio (ASKAP/EMU, LOFAR, APERTIF, etc.) NWAY will provide a powerful and reliable counterpart identification tool.
Molecular Identification of Grouper Fish (Perciformes: Serranidae) Landed From Pangpang Bay, Banyuwangi

The Pangpang Bay Banyuwangi has a high potential for fisheries, processing and capturing fisheries, especially the order Perciformes of the families Carangidae, Lutjanidae and Serranidae. Grouper (Serranidae) is one of the high-economic marine fish commodities. However, the grouper fishing data in this area is only known as grouper without knowing the type of species. It is challenging to identify grouper species because groupers have a high degree of morphological similarity and colour variation. Therefore, molecular identification is necessary to determine the type of grouper in this region. This study aims to identify the grouper species that landed from Pangpang Bay based on DNA barcoding. In addition, phylogenetic tree analysis between grouper species (Serranidae) was carried out, and genetic distance analysis of the identified species was compared to the NCBI database. Morphological observations on groupers were carried out first, and fish meat samples were taken for experiments on molecular identification. The results of molecular-based identification revealed two grouper species Epinephelus coioides and Cephalopholis miniata. The results of phylogenetic tree reconstruction of the two groupers form a separate clade. The genetic distance between Epinephelus coioides ranged from 0.00-0.122, while the species of Cephalopholis miniata had a genetic distance of 0.00-0.002.
Complete Quasi-Metrics for Hyperspaces, Continuous Valuations, and Previsions

The Kantorovich-Rubinshtein metric is an $L^1$-like metric on spaces of probability distributions that enjoys several serendipitous properties. It is complete separable if the underlying metric space of points is complete separable, and in that case it metrizes the weak topology. We introduce a variant of that construction in the realm of quasi-metric spaces, and prove that it is algebraic Yoneda-complete as soon as the underlying quasi-metric space of points is algebraic Yoneda-complete, and that the associated topology is the weak topology. We do this not only for probability distributions, represented as normalized continuous valuations, but also for subprobability distributions, for various hyperspaces, and in general for different brands of functionals. Those functionals model probabilistic choice, angelic and demonic non-deterministic choice, and their combinations. The mathematics needed for those results are more demanding than in the simpler case of metric spaces. To obtain our results, we prove a few other results that have independent interest, notably: continuous Yoneda-complete spaces are consonant; on a continuous Yoneda-complete space, the Scott topology on the space of $\overline{\mathbb{R}}_+$-valued lower semicontinuous maps coincides with the compact-open and Isbell topologies, and the subspace topology on spaces of $\alpha$-Lipschitz continuous maps also coincides with the topology of pointwise convergence, and is stably compact; we introduce and study the so-called Lipschitz-regular quasi-metric spaces, and we show that the formal ball functor induces a Kock-Z\"oberlein monad, of which all algebras are Lipschitz-regular; and we prove a minimax theorem where one of the spaces is not compact Hausdorff, but merely compact.
Kinematics of Type II Cepheids of the Galactic Halo

In a step toward understanding the origin of the Galactic Halo, we have reexamined Type II Cepheids (T2C) in the field with new input from the second data release (DR2) of Gaia. For 45 T2C with periods from 1 to 20 days, parallaxes, proper motions, and [Fe/H] values are available for 25 stars. Only five show [Fe/H] < −1.5, while the remaining stars show thick disk kinematics and [Fe/H] > −0.90. We have compared the T2C stars of the field with their cousins in the globular clusters of the Halo and found that the globular clusters with T2C stars show metallicities and kinematics of a pure Halo population. The globular cluster may have formed during the overall collapse of the Galaxy, while the individual thick disk T2C stars may have been captured from small systems that self-enriched prior to capture. The relationship of these two populations to the microgalaxies currently recognized as surrounding the Galaxy is unclear.
Deployment and calibration procedures for accurate timing and directional reconstruction of EAS particle-fronts with HELYCON stations

High energy cosmic rays, with energies thousands of times higher than those encountered in particle accelerators, offer scientists the means of investigating the elementary properties of matter. In order to detect high energy cosmic rays, new detection hardware and experimental methods are being developed. In this work, we describe the network of HELYCON (HEllenic LYceum Cosmic Observatories Network) autonomous stations for the detection and directional reconstruction of Extended Atmospheric Showers (EAS) particle-fronts. HELYCON stations are hybrid stations consisting of three large plastic scintillators plus a CODALEMA antenna for the RF detection of EAS particle-fronts. We present the installation, operation and calibration of three HELYCON stations and the electronic components for the remote control, monitor and Data Acquisition. We report on the software package developed for the detailed simulation of the detectors' response and for the stations' operation. The simulation parameters have been fine tuned in order to accurately describe each individual detector's characteristics and the operation of each HELYCON station. Finally, the evaluation of the stations' performance in reconstructing the direction of the EAS particle-front is being presented.
Neutrino-nucleon reaction rates in the supernova core in the relativistic random phase approximation

We calculate neutrino reaction rates with nucleons via the neutral and charged currents in the supernova core in the relativistic random phase approximation (RPA) and study their effects on the opacity of the supernova core. The formulation is based on the Lagrangian employed in the calculation of the nuclear equation of state (EOS) in the relativistic mean field theory (RMF). The nonlinear meson terms are treated appropriately so that the consistency of the density correlation derived in RPA with the thermodynamic derivative obtained from the EOS by the RMF is satisfied in the static and long wavelength limit. We employ pion and rho meson exchange interactions together with the phenomenological Landau-Migdal parameters for the isospin-dependent nuclear interactions. We find that both the charged and neutral current reaction rates are suppressed from Bruenn's standard approximate formula considerably in the high density regime $({\ensuremath{\rho}}_{b}\ensuremath{\gtrsim}{10}^{14}{\mathrm{g}/\mathrm{c}\mathrm{m}}^{3}$ with ${\ensuremath{\rho}}_{b}$ the baryonic density). In the low density regime $({\ensuremath{\rho}}_{b}\ensuremath{\lesssim}{10}^{14}{\mathrm{g}/\mathrm{c}\mathrm{m}}^{3}),$ on the other hand, the vector current contribution to the neutrino-nucleon scattering rate is enhanced in the vicinity of the boundary of the liquid-gas phase transition, while the other contributions are moderately suppressed there also. In the high temperature regime $(T\ensuremath{\gtrsim}40\mathrm{MeV}$ with T the temperature) or in the regime where electrons have a large chemical potential, the latter of which is important only for the electron capture process and its inverse process, the recoil of nucleons cannot be neglected and further reduces the reaction rates with respect to the standard approximate formula which discards any energy transfer in the processes. These issues could have a great impact on the neutrino heating mechanism of collapse-driven supernovae.
The Presence of Turbulent and Ordered Local Structure within the ICME Shock-sheath and Its Contribution to Forbush Decrease

The transient interplanetary disturbances evoke short-time cosmic-ray flux decrease, which is known as Forbush decrease. The traditional model and understanding of Forbush decrease suggest that the sub-structure of an interplanetary counterpart of coronal mass ejection (ICME) independently contributes to cosmic-ray flux decrease. These sub-structures, shock-sheath, and magnetic cloud (MC) manifest as classical two-step Forbush decrease. The recent work by Raghav et al. has shown multi-step decreases and recoveries within the shock-sheath. However, this cannot be explained by the ideal shock-sheath barrier model. Furthermore, they suggested that local structures within the ICME’s sub-structure (MC and shock-sheath) could explain this deviation of the FD profile from the classical FD. Therefore, the present study attempts to investigate the cause of multi-step cosmic-ray flux decrease and respective recovery within the shock-sheath in detail. A 3D-hodogram method is utilized to obtain more details regarding the local structures within the shock-sheath. This method unambiguously suggests the formation of small-scale local structures within the ICME (shock-sheath and even in MC). Moreover, the method could differentiate the turbulent and ordered interplanetary magnetic field (IMF) regions within the sub-structures of ICME. The study explicitly suggests that the turbulent and ordered IMF regions within the shock-sheath do influence cosmic-ray variations differently.
Mode identification of high-quality-factor single-defect nanocavities in quantum dot-embedded photonic crystals

We investigate the quality (Q) factor and the mode dispersion of single-defect nanocavities based on a triangular-lattice GaAs photonic-crystal (PC) membrane, which contain InAs quantum dots (QDs) as a broadband emitter. To obtain a high Q factor for the dipole mode, we modulate the radii and positions of the air holes surrounding the nanocavity while keeping sixfold symmetry. A maximum Q of 17 000 is experimentally demonstrated with a mode volume of V=0.39(λ∕n)3. We obtain a Q∕V of 44 000(n∕λ)3, one of the highest values ever reported with QD-embedded PC nanocavities. We also observe ten cavity modes within the first photonic band gap for the modulated structure. Their dispersion and polarization properties agree well with the numerical results.
A Wide-field Map of Intracluster Globular Clusters in Coma

The large-scale distribution of globular clusters in the central region of the Coma cluster of galaxies is derived through the analysis of Hubble Space Telescope/Advanced Camera for Surveys data. Data from three different HST observing programs are combined in order to obtain a full surface density map of globular clusters in the core of Coma. A total of 22,426 Globular cluster candidates were selected through a detailed morphological inspection and the analysis of their magnitude and colors in two wavebands, F475W (Sloan g) and F814W (I). The spatial distribution of globular clusters defines three main overdensities in Coma that can be associated with NGC 4889, NGC 4874, and IC 4051 but have spatial scales five to six times larger than individual galaxies. The highest surface density of globular clusters in Coma is spatially coincidental with NGC 4889. The most extended overdensity of globular clusters is associated with NGC 4874. Intracluster globular clusters also form clear bridges between Coma galaxies. Red globular clusters, which agglomerate around the center of the three main subgroups, reach higher surface densities than blue ones.
Late-Type Stars in M31. I. Photometric Study of AGB Stars and Metallicity Gradients

We have imaged five 7\arcmin \x 7\arcmin\ fields in M31 spanning galactocentric radii from 4 to 32 kpc along the SW-major axis. The fields were observed through two broad-band (\V\ and \I) and two narrow-band (\CN\ and \TiO) filters. The broad-band data were used to construct \IvsVI\ color-magnitude diagrams (CMDs) and, in some of our fields, we found significant numbers of stars in the Cepheid instability strip. A distance modulus for the Cepheids in the middle field was found that agreed well with other values in the literature values. The width of the giant branch (GB) in the \IvsVI\ CMD of all 5 fields was investigated, and we show that in four of the fields a likely explanation for the GB width is a combination of {\it both} metallicity and mass variations. Using the broad-band data, the asymptotic giant branch (AGB) luminosity functions (LFs) were measured in the five fields, and we show that differences exist between these LFs. We speculate on how the different star forming histories in the fields may lead to the observed AGB LFs and GB widths. Using the narrow-band data along with the broad-band data we separated the AGB stars into carbon-rich (C) and oxygen-rich (M) types. The carbon stars LFs were used to obtain an estimate for the distance modulus of M31 which agrees with the value derived from Cepheids. The ratio of C- to M-stars (C/M) is believed to be an indicator of gaseous chemical abundance at the time of formation of these stars. We show that the C/M ratio increases smoothly with galactocentric distance, suggesting an inverse correlation with metallicity. This is the first demonstration of this effect within a single extragalactic system. We find that differences in the width of the GB and the AGB LFs do not significantly affect the C/M ratio. We consider the effect of the increasing C/M ratio on the ISM in M31, and cite evidence in favor of a model where the grain composition in M31 is a function of galactocentric distance.
Loading a Bose-Einstein condensate onto an optical lattice: An application of optimal control theory to the nonlinear Schrödinger equation

Using a set of general methods developed by Krotov [A. I. Konnov and V. A. Krotov, Automation and Remote Control 60, 1427 (1999)], we extend the capabilities of optimal control theory to the nonlinear Schroedinger equation (NLSE). The paper begins with a general review of the Krotov approach to optimization. Although the linearized version of the method is sufficient for the linear Schroedinger equation, the full flexibility of the general method is required for treatment of the nonlinear Schroedinger equation. Formal equations for the optimization of the NLSE, as well as a concrete algorithm are presented. As an illustration, we consider a Bose-Einstein condensate (BEC) initially at rest in a harmonic trap. A phase develops across the BEC when an optical lattice potential is turned on. The goal is to counter this effect and keep the phase flat by adjusting the trap strength. The problem is formulated in the language of optimal control theory (OCT) and solved using the above methodology. To our knowledge, this is the first rigorous application of OCT to the nonlinear Schroedinger equation, a capability that is bound to have numerous other applications.
Challenging the Eurocentrism in volunteering

ABSTRACT Volunteering practices have largely drawn on theories based on Eurocentric conceptualizations. The dominant Eurocentric models of volunteering, as a significant leisure experience, have served to marginalize other definitions and practices. Thus, this paper argues that, while the Eurocentric conceptualization provides a useful framework to understand volunteering in different cultural contexts, it is critical to embrace the complexities and nuances that exist beyond this. Consequently, the paper presents a critical examination of the limitations of this dominant conceptualization of volunteering. In doing so, the paper challenges Eurocentrism domination in the studies of volunteerism and discourse and examines how volunteering can (and does) differ across cultural contexts, to varying degrees. Overall, this paper shows that volunteering is a more complex and nuanced concept than the dominant Eurocentric models depict. Consequently, this paper offers a potential springboard from which to critically examine potentially contested culturally driven meanings of leisure, of which volunteering is an integral component, empowering people to own their leisure rather than conform to Eurocentric definitions of leisure.
Circuit Modelling of Broadband Antenna Using Vector Fitting and Foster Form Approaches for IoT Applications

Computation of the broadband antenna impedance behavior requires the wideband lumped equivalent circuit. This work aims to provide a comprehensive study of broadband antenna equivalent circuit models over broad frequency ranges for Internet of Things (IoT) applications using multiple approaches. The first approach is a Foster approximation, which is based on the antenna-simulated scattering parameters and impedance data. The second concerns a vector-fitting fitting approximation, which is based on the antenna-simulated impedance/admittance data. The studied antenna is modeled based on the radiating element’s geometry and the multifractal slots, in addition to the DGS (Defected Ground Plane) effects. Applying these techniques, wideband lumped equivalent circuits of the antenna have been computed which are in good agreement with measurement data. These models could be useful for the enhancement of the performance of a broadband antenna and its systematic design as well as offering the advantage of saving computation time for full-wave simulations and facilitating the solution of problems that have both an electromagnetic part as well as a circuit part. For further analysis, the Gaussian pulse has been generated to drive a time-domain analysis of the current and power response waveforms antenna behavior under load.
Angle-resolved soft x-ray spectroscopy study of the electronic states of single-crystal MgB2

Angle-resolved soft x-ray measurements made at the boron K edge in single-crystal MgB 2 provide insights into the B 2p local partial density of both unoccupied and occupied band states. The strong variation of absorption with incident angle of exciting x rays permits the clear separation of contributions from σ states in the boron plane and π states normal to the plane. A careful comparison with theory accurately determines the energy of selected critical k points in the conduction band. Resonant inelastic x-ray emission at an incident angle of 15° shows a large enhancement of the emission spectra within about 0.5 eV of the Fermi level that is absent at 45° and is much reduced at 60°. We conclude that momentum transferred from the resonant inelastic x-ray scattering process couples empty and filled states across the Fermi level.
A compilation of known QSOs for the Gaia mission

Quasars are essential for astrometry in the sense that they are spatially stationary because of their large distance from the Sun. The European Space Agency (ESA) astrometric satellite Gaia is scanning the whole sky with unprecedented accuracy up to the level of a few μas. However, Gaia’s two-fields-of-view-observation strategy may introduce a parallax bias in the Gaia catalog. Since it presents no significant parallax, a quasar is the perfect natural object to detect such bias. More importantly, quasars can be used to construct a celestial reference frame in the optical wavelengths for the Gaia mission. In this paper, we compile a list of known quasars that have been published in the literatures. The final compilation (designated as Known Quasars Catalog for Gaia mission, KQCG) contains 1 842 076 objects, among which 797 632 objects are found in Gaia DR1 after cross-identifications. Redshift, color information and position uncertainties of the objects are also provided if available. This catalog will be very useful for the Gaia mission.
The photometric structure of the inner Galaxy

The light distribution in the inner few kiloparsecs of the Milky Way is recovered non­ parametrically from a dust-corrected near-infrared COBEIDIRBE surface brightness map of the inner Galaxy. The best fits to the photometry are obtained when the Sun is assumed to lie -14 ± 4 pc above the plane. The recovered density distributions clearly show an elongated three-dimensional bulge set in a highly non-axisymmetric disc. In the favoured models, the bulge has axis ratios 1 : 0.6: 0.4 and semi-major axis length -2 kpc. Its nearer long axis lies in the first quadrant. The bulge is surrounded by an elliptical disc that extends to -2 kpc on the minor axis and -3.Skpc on the major axis. In all models there is a local density minimum -2.2kpc down the minor axis. The subsequent maximum - 3 kpc down the minor axis (corresponding to I = -22° and I = 17°) may be associated with the Lagrange point L4 . From this identification and the length of the bulge-bar, we infer a pattern speed Db = 60-70 km s -1 kpc -1 for the bar. Experiments in which pseudo-data derived from models with spiral structure were deprojected under the assumption that the Galaxy is either eight-fold or four-fold symmetric indicate that the highly non-axisymmetric discs recovered from the COBE data could reflect spiral structure within the Milky Way if that structure involves density contrasts greater than ~3 at near-infrared wavelengths. These experiments indicate that the angle CPo between the Sun-centre line and a major axis of the bulge lies near 20°.
Entanglement entropy in 
TT¯
-deformed CFT

In this paper, we study the entanglement entropy of a single interval on a cylinder in two-dimensional $T\overline{T}$-deformed conformal field theory. For such case, the (R\'enyi) entanglement entropy takes a universal form in a CFT. We compute the correction due to the deformation up to the leading order of the deformation parameter in the framework of the conformal perturbation theory. We find that the correction to the entanglement entropy is nonvanishing in the finite temperature case, while it is vanishing in the finite size case. For the deformed holographic large $c$ CFT, which is proposed to be dual to a AdS$_3$ gravity in a finite region, we find the agreement with the holographic entanglement entropy via the Ryu-Takayanagi formula. Moreover, we compute the leading order correction to the R\'enyi entropy, and discuss its holographic picture as well.