Miracle-dz/UniFAR-FTUs huggingface dataset:
and the Diffuse Interstellar Bands: An Independent Laboratory Check

In 2015, Campbell et al. presented spectroscopic laboratory gas phase data for the fullerene cation, , that coincide with the reported astronomical spectra of two diffuse interstellar band (DIB) features at 9633 and 9578 Å. In the following year, additional laboratory spectra were linked to three other and weaker DIBs at 9428, 9366, and 9349 Å. The laboratory data were obtained using wavelength-dependent photodissociation spectroscopy of small (up to three) He-tagged ion complexes, yielding rest wavelengths for the bare cation by correcting for the He-induced wavelength shifts. Here we present an alternative approach to derive the rest wavelengths of the four most prominent absorption features, using high-resolution laser dissociation spectroscopy of embedded in ultracold He droplets. Accurate wavelengths of the bare fullerene cation are derived from linear wavelength shifts recorded for species with n up to 32. A careful analysis of all of the available data results in precise rest wavelengths (in air) for the four most prominent bands: 9631.9(1) Å, 9576.7(1) Å, 9427.5(1) Å, and 9364.9(1) Å. The corresponding bandwidths have been derived and the relative band intensity ratios are discussed.
Evidence from gravitational lensing for a non‐thermal pressure support in the cluster of galaxies A2218

The central mass distribution of clusters of galaxies can be inferred from gravitationally lensed arcs with known redshifts. For the Abell cluster 2218, this method yields a core mass which is larger by a factor of 2.5±0.5 than the value deduced from X‐ray observations, under the assumptions that the gas is supported by thermal pressure and that the cluster is spherical. We examine quantitatively various potential causes for this discrepancy, and show that a non‐thermal pressure support is a plausible explanation. Such a pressure can be naturally provided by strong turbulence and equipartition magnetic field (∼50 μG) that are tangled on small scales in the cluster core. The turbulent and magnetic pressures do not affect the measured Sunyaev‐Zel’dovich (SZ) effect for this cluster. Intracluster magnetic fields with a comparable magnitude (∼101–2 μG) have already been detected by Faraday rotation in other clusters. If generic, a small‐scale equipartition magnetic field should affect the structure of cooling.
Spectral and morphological study of the gamma radiation of the middle-aged supernova remnant HB 21

Aims. We investigate the nature of the accelerated particles responsible for the production of the gamma-ray emission observed from the middle-aged supernova remnant (SNR) HB 21. Methods. We present the analysis of more than nine years of Fermi LAT data from the SNR HB 21. We performed morphological and spectral analysis of the SNR by means of a three-dimensional binned likelihood analysis. To assess the intrinsic properties of the parent particle models, we fit the obtained gamma-ray spectral energy distribution of the SNR by both hadronic- and leptonic-induced gamma-ray spectrum. Results. We observe an extended emission positionally in agreement with the SNR HB 21. The bulk of this gamma-ray emission is detected from the remnant; photons up to ~10 GeV show clear evidence of curvature at the lower energies. The remnant is characterized by an extension of 0°. 83, that is, 30% smaller than claimed in previous studies. The increased statistics allowed us also to resolve a point-like source at the edge of the remnant, in proximity to a molecular cloud of the Cyg OB7 complex. In the southern part of the remnant, a hint of an additional gamma-ray excess in correspondence to shocked molecular clouds is observed. Conclusions. The spectral energy distribution of the SNR shows evidence of a break around 400 MeV, which can be properly fitted within both the hadronic and leptonic scenario. The pion-decay mechanism reproduces well the gamma rays, postulating a proton spectrum with a slope ~2.5 and with a steepening around tens of GeV, which could be explained by the energy-dependent escape of particles from the remnant. In the leptonic scenario the electron spectrum within the SNR matches closely the locally measured spectrum. This remarkable and novel result shows that SNR HB 21 could be a direct contributor to the population of Galactic electrons. In the leptonic scenario, we find that the local electron spectrum with a break around 2 GeV, closely evokes the best-fitting parental spectrum within this SNR. If such a scenario is confirmed, this would indicate that the SNR might be a source of Galactic background electrons.
High energy particles from monopoles connected by strings

Monopole-antimonopole pairs connected by strings and monopole-string networks with N{gt}2 strings attached to each monopole can be formed at phase transitions in the early universe. In such hybrid defects, monopoles accelerate under the string tension and can reach ultrarelativistic Lorentz factors {gamma}{gt}1. We study the radiation of gauge quanta by accelerating monopoles. For monopoles with a chromomagnetic charge, we also discuss the high-energy hadron production through emission of virtual gluons and their subsequent fragmentation into hadrons. The relevant parameter for gauge boson radiation is M/a where M is the boson mass and a is the proper acceleration of the monopole. For M{lt}a, the gauge bosons can be considered as massless and the typical energy of the emitted quanta is E{approximately}{gamma}a. In the opposite limit M{gt}a, the radiation power is exponentially suppressed and gauge quanta are emitted with a typical energy E{approximately}{gamma}M in a narrow range {Delta}E/E{approximately}(a/M){sup 1/2}. Cosmological monopole-string networks can produce photons and hadrons of extremely high energies. For a wide range of parameters these energies can be much greater than the Planck scale. {copyright} {ital 1997} {ital The American Physical Society}
Environmental Analysis of GOES-R Proving Ground Convection-Initiation Forecasting Algorithms

AbstractEnhanced temporal and spatial resolution of the Geostationary Operational Environmental Satellite–R Series (GOES-R) will allow for the use of cloud-top-cooling-based convection-initiation (CI) forecasting algorithms. Two such algorithms have been created on the current generation of GOES: the University of Wisconsin cloud-top-cooling algorithm (UWCTC) and the University of Alabama in Huntsville’s satellite convection analysis and tracking algorithm (SATCAST). Preliminary analyses of algorithm products have led to speculation over preconvective environmental influences on algorithm performance. An objective validation approach is developed to separate algorithm products into positive and false indications. Seventeen preconvective environmental variables are examined for the positive and false indications to improve algorithm output. The total dataset consists of two time periods in the late convective season of 2012 and the early convective season of 2013. Data are examined for environmental relati.
An Updated Catalog of 4680 Northern Eclipsing Binaries with Algol-type Light-curve Morphology in the Catalina Sky Surveys

We present an updated catalog of 4680 northern eclipsing binaries (EBs) with Algol-type light-curve (LC) morphology (i.e., with well-defined beginnings and ends of primary and secondary eclipses), using data from the Catalina Sky Surveys. Our work includes revised period determinations, phenomenological parameters of the LCs, and system morphology classifications based on machine-learning techniques. While most of the new periods are in excellent agreement with those provided in the original Catalina catalogs, improved values are now available for ∼10% of the stars. A total of 3456 EBs were classified as detached and 449 were classified as semi-detached, while 145 could not be classified unambiguously into either subtype. The majority of the SD systems seem to be comprised of short-period Algols. By applying color criteria, we searched for K- and M-type dwarfs in these data, and present a subsample of 609 EB candidates for further investigation. We report 119 EBs (2.5% of the total sample) that show maximum quadrature light variations over long timescales, with periods bracketing the range 4.5–18 years and a fractional luminosity variance range of 0.04–0.13. We discuss possible causes for this, making use of models of variable starspot activity in our interpretation of the results.
Small-Scale Systems of Galaxies. III. X-Ray-detected Elliptical+Spiral Galaxy Pairs in Low-Density Environments

We present a comprehensive study of the local environments of four elliptical+spiral (E+S) galaxy pairs with the main goal of investigating their formation/evolution histories. We obtained new XMM-Newton data for two pairs (RR 143 and RR 242) that complement existing ROSAT data for the other two (RR 210 and RR 216). The new observations reveal diffuse X-ray emission in both pairs with luminosities of LX ∼ 3 × 1041 ergs s-1 (0.5-2.0 keV). The emission is asymmetric in both cases and extends out to ∼500″ (120 kpc) and 700″ (160 kpc) in RR 143 and RR 242, respectively. The nucleus of RR 242 hosts a low-luminosity (LX ∼ 1041 ergs s-1 [2.0-10 keV]) mildly absorbed (NH ∼ 1022 cm-2) active galactic nucleus. We find that the early-type components of pairs with diffuse hot gas appear to be relaxed objects, while those in RR 210 and RR 216, where no diffuse emission has been found, display unambiguous signatures of ongoing interaction. New wide-field V- and R-band observations are used to study the photometric properties of the early-type components and to search for candidate faint galaxy populations around each of the pairs. While no diffuse optical light is found for any of the pairs, all of the early-type members show very extended and concentric luminous envelopes. We identify a faint galaxy sample in each field, and we consider whether they could be physically associated with the luminous pairs based on (V - R) colors and photometric properties. We find that the distribution of re and MR for the candidates are similar in three of the fields (RR 143, 216, and 242). The same selection criteria applied to the field of RR 210 suggest a fainter and more compact population, possibly suggesting a larger background fraction than in the other fields.
Nanomodification of aluminum alloys.

NPs are ultrafine-grain crystal or amorphous substances which are as small as 100nm. They have unique physical, chemical and mechanical properties, which are very different from those of large scale materials. This uniqueness is attributed to the fact that the number of atoms in the surface layer and in the bulk is commensurable. As the atoms in the surface layer of nanoparticles have their counterparts from one side only, their balance is impaired, and the resulting structure relaxation leads to the displacement of atomic spacing in a 2-3nm layer. Therefore the surface layers expand while internal layers compressed, as these are exposed to an excessive Laplace pressure of up to hundreds kilobars. Nanoparticles have a highly distorted lattice that has an effect on activation energy of most of the processes they are involved in, by changing their nature and sequence. Nanoscale implies absolutely new effects, properties and processes which are defined by the laws of quantum mechanics, size quantization in small-scale structures, surface-bulk ratio, and other factors. Due to exceptionally small sizes and good reactivity of NP particles, it looks promising to use them in metal melts as crystallization centers to enable structure refinement of cast products. As well known, the grains are finer, the better are mechanical properties of cast products produced from these alloys. After considering a number of options, an efficient method of nanopowder introduction into a liquid metal was proposed. This method avoids all of the above problems and consists in pressing of 5-9.5mm diameter rods or wires that contain aluminum particles (granules and nanopowder). Nanopowder contents in rods added NP to alloys being no more than 0.05%, and sometimes even thousandths of one percent.
Discovery of 6.4 keV line and soft X-ray emissions from G323.7-1.0 with Suzaku

In this paper, the Suzaku X-ray data of the Galactic Supernova Remnant (SNR) candidate G323.7$-$1.0 are analyzed to search for X-ray emission. Spatially-extended enhancements in the 6.4 keV line and in soft X-rays are found inside or on the radio shell. The soft X-ray enhancement would be the hottest part of the shell-like X-ray emission along the radio shell. The 6.4 keV line enhancement is detected at a significance level of $4.1 \sigma$. The lower limit of the equivalent width (EW) is 1.2 keV. The energy centroid of the 6.4 keV line is $6.40 \pm 0.04$ keV, indicating that the iron is less ionized than the Ne-like state. If the 6.4 keV line originates from ionizing non-equilibrium thermal plasma, presence of iron-rich ejecta in a low-ionization state is required, which is disfavored by the relatively old age of the SNR. The 6.4 keV line enhancement would be due to K-shell ionization of iron atoms in a dense interstellar medium by high-energy particles. Since there is no irradiating X-ray source, the origin of the 6.4 keV line enhancement is not likely the photoionization. The large EW can only be explained by K-shell ionization due to cosmic-ray protons with an energy of $\sim 10$ MeV, which might be generated by the shock acceleration in G323.7$-$1.0.
CH 3 GHz Observations of the Galactic Center

A 3 × 3 map of the Galactic center was made at 9' resolution and 10' spacing in the CH 2Π1/2, J = 1/2, F = 1-1 transition at 3335 MHz. The CH emission shows a velocity extent that is close to that of the CO(1-0) line, but the CH line profiles differ markedly from the CO. The 3335 MHz CH transition primarily traces low-density molecular gas in the high-density, high-pressure environment of the Galactic center interstellar medium. If the empirical N(CH)-N(H2) relation derived for molecular clouds in the disk is valid at the Galactic center, then our observations indicate that the mass of the low-density component within ~30 pc of the Galactic center is ~9 × 106 M☉. The CO-H2 conversion factor obtained for the low-density gas in the mapped region is greater than that thought to apply to the dense molecular gas at the Galactic center. The CH spectra show evidence of emission from molecular clouds along the line of sight in both the foreground and the background. The scale height of these clouds ranges from 27 to 109 pc, consistent with previous work based on observations of molecular clouds in the inner Galaxy.
Black hole in a superconducting plasma

The generalized vortical formalism provides an electrodynamic description for superconducting states---in the generalized vortical formalism, a superconducting state may be defined by the vanishing of an appropriate generalized vorticity and characterized by zero generalized helicity for incompressible fluids. In this article, we investigate these states for compressible plasmas in black hole spacetime geometries using the curved spacetime generalization of the grand generalized vortical formalism. If the magnetic field is axisymmetric and the thermodynamic properties are symmetric about the equatorial plane, the resulting states are characterized by a vanishing skin depth and a complete expulsion of the magnetic field at the equator of the black hole horizon. Moreover, if the thermodynamic properties of the plasma are uniform at the horizon, we find that the magnetic field is completely expelled from the horizon, and the plasma behaves as a perfect superconductor near the horizon. This result is independent of the spin of a black hole, holding even for a (nonrotating) Schwarzschild black hole, and demonstrates that the geometry near black hole horizons can have a significant effect on the electrodynamics of surrounding plasmas.
X-rays from the high-redshift universe: The Chandra view

The study of the X-ray properties of z>4 quasars has grown substantially over the last few years, mostly thanks to Chandra. Here we focus on (1) the average X-ray properties of an optically selected, luminous sample of nine z>4 Palomar Digital Sky Survey quasars recently observed by Chandra, and (2) the X-ray spectral properties of three z>4 AGNs in the Chandra Deep Field-North (CDF-N) using the 2 Ms exposure.
Evolution of Compact and Fossil Groups of Galaxies from Semi-analytical Models of Galaxy Formation

We compare the mean mass assembly histories of compact and fossil galaxy groups in the Millennium Dark Matter Simulation and an associated semi-analytic galaxy formation model. Tracing the halo mass of compact groups (CGs) from z = 0 to z = 1 shows that, on average, 55% of the halo mass in CGs is assembled since , compared to 40% of the halo mass in fossil groups (FGs) on the same time interval, indicating that compared to FGs, CGs are relatively younger galaxy systems. At z = 0, for a given halo mass, FGs tend to have a larger concentration than CGs. Investigating the evolution of CG’s parameters reveals that they become more compact with time. CGs at z = 0.5 see their magnitude gaps increase exponentially, but it takes ∼10 Gyr for them to reach a magnitude gap of 2 mag. The slow growth of the magnitude gap leads to only a minority (∼41%) of CGs selected at z = 0.5 turning into a FG by z = 0. Also, while three-quarters of FGs go through a compact phase, most fail to meet the CG isolation criterion, leaving only ∼30% of FGs fully satisfying the CG selection criteria. Therefore, there is no strong link of CGs turning into FGs or FGs originating from CGs. The relation between CGs and FGs is thus more complex, and in most cases, FGs and CGs follow different evolutionary tracks.
Theory of Interacting Bloch Electrons in a Magnetic Field

We study interacting electrons in a periodic potential and a uniform magnetic field B taking the spin-orbit interaction into account. We first establish a perturbation expansion for those electrons with respect to the Bloch states in zero field. It is shown that the expansion can be performed with the zero-field Feynman diagrams of satisfying the momentum and energy conservation laws. We thereby clarify the structures of the self-energy and the thermodynamic potential in a finite magnetic field. We also provide a prescription of calculating the electronic structure in a finite magnetic field within the density functional theory starting from the zero-field energy-band structure. On the basis of these formulations, we derive explicit expressions for the magnetic susceptibility of B → 0 at various approximation levels on the interaction, particularly within the density functional theory, which include the result of Roth [J. Phys. Chem. Solids 23 (1962) 433] as the non-interacting limit. We finally study the.
Finding planes and clusters of objects from 3D line segments with application to 3D motion determination

Abstract We address in this paper how to find clusters based on proximity and planar facets based on coplanarity from 3D line segments obtained from stereo. The proposed methods are efficient and have been tested with many real stereo data. These procedures are indispensable in many applications including scene interpretation, object modeling, and object recognition. We show their application to 3D motion determination. We have developed an algorithm based on the hypothesize-and-verify paradigm to register two consecutive 3D frames obtained from stereo and estimate their transformation/motion. By grouping 3D line segments in each frame into clusters and planes, we can reduce effectively the complexity of the hypothesis generation phase.
Three-dimensional kinematic reconnection in the presence of field nulls and closed field lines

The present investigation of three-dimensional reconnection of magnetic fields with nulls and of fields with closed lines gives attention to the geometry of the former, with a view to their gamma-line and Sigma-surface structures. The geometric structures of configurations with a pair of type A and B nulls permit reconnection across the null-null lines; these are the field lines which join the two nulls. Also noted is the case of magnetostatic reconnection, in which the magnetic field is time-independent and the electrostatic potential is constant along field lines. 31 refs.
THE TIME DEVELOPMENT OF A RESONANCE LINE IN THE EXPANDING UNIVERSE

The time-dependent spectral profile of a resonance line in a homogeneous expanding medium is studied by numerically solving an improved Fokker-Planck diffusion equation. The solutions are used to determine the time required to reach a quasi-static solution near the line center. A simple scaling law for this relaxation time is derived and is fitted to the numerical results. The results are applied to the case of Lyman alpha scattering during primordial recombination of hydrogen. For a wide range of cosmological models it is found that the relaxation times are smaller than the recombination timescale, although not by a very large factor. Thus the standard assumption of a quasi-static solution in cosmological recombination calculations is reasonably valid, and should not cause substantial errors in the solutions.
The one-dimensional Kondo lattice model at partial band filling

The Kondo lattice model introduced in 1977 describes a lattice of localized magnetic moments interacting with a sea of conduction electrons. It is one of the most important canonical models in the study of a class of rare earth compounds, called heavy fermion systems, and as such has been studied intensively by a wide variety of techniques for more than a quarter of a century. This review focuses on the one-dimensional case at partial band filling, in which the number of conduction electrons is less than the number of localized moments. The theoretical understanding, based on the bosonized solution, of the conventional Kondo lattice model is presented in great detail. This review divides naturally into two parts, the first relating to the description of the formalism, and the second to its application. After an all-inclusive description of the bosonization technique, the bosonized form of the Kondo lattice Hamiltonian is constructed in detail. Next the double-exchange ordering, Kondo singlet formation, th.
Relation between phase-space coverage and entanglement for spin-1/2 systems

For systems of two and three spins 1/2 it is known that the second moment of the Husimi function can be related to entanglement properties of the corresponding states. Here, we generalize this relation to an arbitrary number of spins in a pure state. It is shown that the second moment of the Husimi function can be expressed in terms of the lengths of the concurrence vectors for all possible partitions of the N-spin system in two subsystems. This relation implies that the phase space distribution of an entangled state is less localized than that of a nonentangled state. As an example, the second moment of the Husimi function is analyzed for an Ising chain subject to a magnetic field perpendicular to the chain axis.