Miracle-dz/UniFAR-FTUs huggingface dataset:
Short-range order in iron-rich Fe-Cr alloys as revealed by Mössbauer spectroscopy

Distribution of Cr atoms in Fe_{100-x}Cr_x alloys with x \le 25 within the first two coordination shells, 1NN-2NN, around probe 57Fe atoms was studied by means of the M\"ossbauer Spectroscopy. Clear evidence was found that the distribution is characteristic of a given atomic configuration. Only the configurations with Cr atoms situated in 2NN exhibit a quiasi-random distribution, while those with Cr atoms present in 1NN shell and those with Cr atoms in both shells is evidently not random showing clastering or anticlastering features. These findings are novel and much more complete than the up-to-date knowledge according to which there is an inversion of the short-range order parameter at x = 11. The inversion in the present study was found only for the configuration with one Cr atom in 1NN. On average, Cr atoms are distributed almost randomly within the 1NN-2NN volume for x \eq ~10, and do cluster for larger x.
TSD-Truncated Structurally Aware Distance for Small Pest Object Detection

As deep learning has been successfully applied in various domains, it has recently received considerable research attention for decades, making it possible to efficiently and intelligently detect crop pests. Nevertheless, the detection of pest objects is still challenging due to the lack of discriminative features and pests’ aggregation behavior. Recently, intersection over union (IoU)-based object detection has attracted much attention and become the most widely used metric. However, it is sensitive to small-object localization bias; furthermore, IoU-based loss only works when ground truths and predicted bounding boxes are intersected, and it lacks an awareness of different geometrical structures. Therefore, we propose a simple and effective metric and a loss function based on this new metric, truncated structurally aware distance (TSD). Firstly, the distance between two bounding boxes is defined as the standardized Chebyshev distance. We also propose a new regression loss function, truncated structurally aware distance loss, which consider the different geometrical structure relationships between two bounding boxes and whose truncated function is designed to impose different penalties. To further test the effectiveness of our method, we apply it on the Pest24 small-object pest dataset, and the results show that the mAP is 5.0% higher than other detection methods.
Effect of the consumption of a cocoa paste bar (Theobroma cacao L.) on metabolic indicators in university students

The aim of this study was to determine the effect on metabolic indicators (total cholesterol, triacylglycerides, HDL, LDL and glycemia) in university students, after the daily consumption of 1.00 g of a cocoa paste bar (PCB) and 0.50 g of a white chocolate bar (BCB) during two months. The population was characterized according to their sex, weight, height, body mass index (BMI), physical activity and diet. The pre- and post-metabolic levels were measured in the control group (BCB) and experimental group (BPC). The students have normal weight (22.90 kg/m2 and 24.99 kg/m2), average physical activity was predominat (55.60 %) and their nutrition was inadequate. The study groups presented metabolic levels within the normal parameter. However, the consumption of 1 g of PCB for two months increases HDL levels (36.94 ± 13.42 mg/dL vs 59.74 ± 9.41 mg/dL), an effect that is highly desirable in a food
CO OBSERVATIONS OF THE HOST GALAXY OF GRB 000418 AT z = 1.1

We performed CO (J = 2–1) observations of the host galaxy of GRB 000418 at z = 1.1181 with the Plateau de Bure Interferometer. Previous studies show that the host galaxy has properties similar to those of an ultraluminous infrared galaxy (ULIRG). The star formation rate (SFR) of the host galaxy as derived from submillimeter and radio continuum emission is a few 100 M☉ yr−1, which is an order of magnitude greater than the SFR derived from optical line emission. The large discrepancy between the SFRs derived from different observing wavelengths indicates the presence of a bulk of dust-obscured star formation and molecular gas that is enough to sustain the intense star formation. We failed to detect CO emission and derived 2σ upper limits on the velocity-integrated CO (2–1) luminosity of L′CO < 6.9 × 109 K km s−1 pc2 and the molecular gas mass of M☉ by adopting a velocity width of 300 km s−1 and a CO-to-H2 conversion factor of αCO = 0.8 M☉ (K km s−1 pc2)−1, which are standard values for ULIRGs. The lower limit on the ratio of far-infrared luminosity to CO luminosity, a measure of the star formation efficiency, is higher compared to that of other gamma-ray burst hosts and other galaxy populations, which is consistent with active star formation taking place in this galaxy.
TOWARD CHEMICAL CONSTRAINTS ON HOT JUPITER MIGRATION

The origin of hot Jupiters—gas giant exoplanets orbiting very close to their host stars—is a long-standing puzzle. Planet formation theories suggest that such planets are unlikely to have formed in situ but instead may have formed at large orbital separations beyond the snow line and migrated inward to their present orbits. Two competing hypotheses suggest that the planets migrated either through interaction with the protoplanetary disk during their formation, or by disk-free mechanisms such as gravitational interactions with a third body. Observations of eccentricities and spin–orbit misalignments of hot Jupiter systems have been unable to differentiate between the two hypotheses. In the present work, we suggest that chemical depletions in hot Jupiter atmospheres might be able to constrain their migration mechanisms. We find that sub-solar carbon and oxygen abundances in Jovian-mass hot Jupiters around Sun-like stars are hard to explain by disk migration. Instead, such abundances are more readily explained by giant planets forming at large orbital separations, either by core accretion or gravitational instability, and migrating to close-in orbits via disk-free mechanisms involving dynamical encounters. Such planets also contain solar or super-solar C/O ratios. On the contrary, hot Jupiters with super-solar O and C abundances can be explained by a variety of formation–migration pathways which, however, lead to solar or sub-solar C/O ratios. Current estimates of low oxygen abundances in hot Jupiter atmospheres may be indicative of disk-free migration mechanisms. We discuss open questions in this area which future studies will need to investigate.
Coxeter groups and Kähler groups

Abstract We study homomorphisms from Kähler groups to Coxeter groups. As an application, we prove that a cocompact complex hyperbolic lattice (in complex dimension at least 2) does not embed into a Coxeter group or a right-angled Artin group. This is in contrast with the case of real hyperbolic lattices.
TIDAL TORQUING OF ELLIPTICAL GALAXIES IN CLUSTER ENVIRONMENTS

Observational studies of galaxy isophotal shapes have shown that galaxy orientations are anisotropic: a galaxy's long axis tends to be oriented toward the center of its host. This radial alignment is seen across a wide range of scales, from galaxies in massive clusters to small Milky Way type satellite systems. Recently, this effect has also been detected in dark matter (DM) simulations of cosmological structure, but the degree of alignment of DM substructures in these studies is significantly stronger than seen in observations. In this paper, we attempt to reconcile these two results by performing high-resolution numerical experiments on N-body multi-component models of triaxial galaxies orbiting in an external analytical potential. The large number of particles employed allows us to probe deep into the inner structure of the galaxy: we show that the discrepancy between observed galaxies and simulated DM halos is a natural consequence of induced radial shape twisting in the galaxy by the external potential. The degree of twisting depends strongly on the orbital phase and eccentricity of the satellite, and it can, under certain conditions, be significant at radii smaller than the DM scale radius. Such internal misalignments will have important consequences, both for the dynamical evolution of the galaxy itself and for mass modeling of galaxies in clustered environments.
Some general aspects of thin-shell wormholes with cylindrical symmetry

In this article we study a general class of nonrotating thin-shell wormholes with cylindrical symmetry. We consider two physically sound definitions of the flare-out condition and we show that the less restrictive one allows for the construction of wormholes with positive energy density at the throat. We also analyze the mechanical stability of these objects under perturbations preserving the symmetry, proving that previous results are particular cases of a general property. We present examples of wormholes corresponding to Einstein-Maxwell spacetimes.
Lifting of xz/yz orbital degeneracy at the structural transition in detwinned FeSe

We study superconducting FeSe (Tc = 9 K) exhibiting the tetragonal-orthorhombic structural transition (Ts = 90 K) without any antiferromagnetic ordering, by utilizing angle-resolved photoemission spectroscopy. In the detwinned orthorhombic state, the energy position of the dyz orbital band at the Brillouin zone corner is 50 meV higher than that of dxz, indicating the orbital order similar to NaFeAs and BaFe2As2 families. Evidence of orbital order also appears in the hole bands at the Brillouin zone center. Precisely measured temperature dependence using strain-free samples shows that the onset of the orbital ordering (To) occurs very close to Ts, thus suggesting that the electronic nematicity above Ts is considerably weaker in FeSe compared to BaFe2As2 family.
CLEARING THE GAS FROM GLOBULAR CLUSTERS AND DWARF SPHEROIDALS WITH CLASSICAL NOVAE

Observations of the intra-cluster medium (ICM) in galactic globular clusters (GCs) show a systematic deficiency in ICM mass as compared to that expected from accumulation of stellar winds in the time available between galactic plane crossings. In this paper, we re-examine the original hypothesis of Scott & Durisen that hydrogen-rich explosions on accreting white dwarfs, classical novae (CNe), will sweep out the ICM from the cluster more frequently than galactic plane crossings. From the CNe rate and stellar mass loss rate, this clearing mechanism predicts that ≈0.03 M☉ should be present in ⩽105 M☉ GCs. We model the expanding remnant made from the 10−4 M☉ nova ejecta and show that it escapes long before it has cooled. We discuss the few positive ICM measurements and use a Monte Carlo simulation of the accumulation and CNe recurrence times to reveal the possible variance in the ICM masses for the higher-mass (>5 × 105 M☉) GCs. We find that nova shells are effective at clearing the ICM in low-mass GCs (⩽105 M☉), whereas higher-mass clusters may experience a quiescent time between novae long enough to prevent the next nova shell from escaping. The nova clearing mechanism will also operate in ultra-faint Milky Way satellites, where many upper limits on gas masses are available.
UNIFICATION OF LUMINOUS TYPE 1 QUASARS THROUGH C iv EMISSION

Using a sample of ∼30,000 quasars from the 7th Data Release of the Sloan Digital Sky Survey, we explore the range of properties exhibited by high-ionization, broad emission lines, such as C iv λ1549. Specifically, we investigate the anti-correlation between continuum luminosity and emission-line equivalent width (the Baldwin Effect (BEff)) and the “blueshifting” of the high-ionization emission lines with respect to low-ionization emission lines. Employing improved redshift determinations from Hewett & Wild, the blueshift of the C iv emission line is found to be nearly ubiquitous, with a mean shift of ∼810 km s−1 for radio-quiet (RQ) quasars and ∼360 km s−1 for radio-loud (RL) quasars. The BEff is present in both RQ and RL samples. We consider these phenomena within the context of an accretion disk-wind model that is modulated by the nonlinear correlation between ultraviolet and X-ray continuum luminosity. Composite spectra are constructed as a function of C iv emission-line properties in an attempt to reveal empirical relationships between different line species and the continuum. Within a two-component disk+wind model of the broad emission-line region (BELR), where the wind filters the continuum seen by the disk component, we find that RL quasars are consistent with being dominated by the disk component, while broad absorption line quasars are consistent with being dominated by the wind component. Some RQ objects have emission-line features similar to RL quasars; they may simply have insufficient black hole (BH) spin to form radio jets. Our results suggest that there could be significant systematic errors in the determination of Lbol and BH mass that make it difficult to place these findings in a more physical context. However, it is possible to classify quasars in a paradigm where the diversity of BELR parameters is due to differences in an accretion disk wind between quasars (and over time); these differences are underlain primarily by the spectral energy distribution, which ultimately must be tied to BH mass and accretion rate.
Cartan's Supersymmetry and the Decay of a $H^0(0^+)$

We compare the decay of a Higgs boson $H^0(0^+)\to\ell\bar\ell \ell\bar\ell\to\gamma\gamma$, $H^0(0^+)\to W\bar W\to \ell\bar\nu\bar\ell\nu$, and $H^0(0^+)\to Z\bar Z\to\ell\bar\ell\ell\bar\ell$ using Cartan's supersymmetry, that defines coupling of a vector particle $x_i$ and Dirac spinors $\psi$ and $\phi$. Apparent discrepancy of $H^0(0^+)\to\gamma\gamma/\ell\bar\ell \ell\bar\ell$ experimental data of ATLAS and CMS collaborations disappears, since the sum of transition to $\ell\bar\ell \ell\bar\ell$ and $\gamma\gamma$ have the meaning. The trilinearity of leptons vector fields coupling and the initial wave functions to be large components define Higgs-leptons couplings. The ratio of Higgs boson decay branching ratios $H\to WW=21.6\pm 0.9$, $H\to\gamma\gamma=0.228\pm 0.011$ can be reproduced when we multiply coupling constant $\alpha_s\simeq 1$ for $WW$ and $\alpha_e=1/137$ for $\gamma\gamma$ to the number of independent diagrams. Comparison with Atiyah-Witten's quark-gluon dynamics on a manifold of $G_2$ holonomy theory is added.
Acceleration of electric current-carrying string loop near a Schwarzschild black hole immersed in an asymptotically uniform magnetic field

We study the acceleration of an electric current-carrying and axially-symmetric string loop initially oscillating in the vicinity of a Schwarzschild black hole embedded in an external asymptotically uniform magnetic field. The plane of the string loop is orthogonal to the magnetic field lines and the acceleration of the string loop occurs due to the transmutation effect turning in the deep gravitational field the internal energy of the oscillating strings to the energy of their translational motion along the axis given by the symmetry of the black hole spacetime and the magnetic field. We restrict our attention to the motion of string loop with energy high enough, when it can overcome the gravitational attraction and escape to infinity. We demonstrate that for the current-carrying string loop the transmutation effect is enhanced by the contribution of the interaction between the electric current of the string loop and the external magnetic field and we give conditions that have to be fulfilled for an efficient acceleration. The Schwarzschild black hole combined with the strong external magnetic field can accelerate the current-carrying string loop up to the velocities close to the speed of light $v \sim c$. Therefore, the string loop transmutation effect can potentially well serve as an explanation for acceleration of highly relativistic jets observed in microquasars and active galactic nuclei.
Mass-dependent evolution of the relation between the supermassive black hole mass and host spheroid mass since z ~ 1

We investigate the evolutions of supermassive black hole mass (M BH ) and host spheroid mass (M s p h ) in order to track the history of the M BH -M sph relationship. The typical mass increase in M BH is calculated by a continuity equation and accretion history, which is estimated from the active galactic nucleus luminosity function. The increase in M s p h is also calculated by using a continuity equation and a star formation model, which uses observational data for the formation rate and stellar mass function. We find that the black hole to spheroid mass ratio is expected to be substantially unchanged since z ~ 1.2 for high mass objects (M BH > 10 8.5 M ⊙ and M s p h > 10 11.3 M ⊙ ). In the same redshift range, the spheroid mass is found to increase more rapidly than the black hole mass if M sph > 10 11 M ⊙ . The proposed mass-dependent model is consistent with the current available observational data in the M BH -M sph diagram.
The Herschel Virgo Cluster Survey

To assess the e ﬀ ects of the cluster environment on the di ﬀ erent components of the interstellar medium, we analyse the far-infrared (FIR) and submillimetre (submm) properties of a sample of star-forming dwarf galaxies detected by the Herschel Virgo Cluster Survey (HeViCS). We determine dust masses and dust temperatures by ﬁtting a modiﬁed black body function to the spectral energy distributions (SEDs). Stellar and gas masses, star formation rates (SFRs), and metallicities are obtained from the analysis of a set of ancillary data. Dust is detected in 49 out of a total 140 optically identiﬁed dwarfs covered by the HeViCS ﬁeld; considering only dwarfs brighter than m B = 18 mag, this gives a detection rate of 43%. After evaluating di ﬀ erent emissivity indices, we ﬁnd that the FIR-submm SEDs are best-ﬁt by β = 1 . 5, with a median dust temperature T d = 22 . 4 K. Assuming β = 1 . 5, 67% of the 23 galaxies detected in all ﬁve Herschel bands show emission at 500 μ m in excess of the modiﬁed black-body model. The fraction of galaxies with a submillimetre excess decreases for lower values of β , while a similarly high fraction (54%) is found if a β -free SED modelling is applied. The excess is inversely correlated with SFR and stellar masses. To study the variations in the global properties of our sample that come from environmental e ﬀ ects, we compare the Virgo dwarfs to other Herschel surveys, such as the Key Insights into Nearby Galaxies: Far-Infrared Survey with Herschel (KINGFISH), the Dwarf Galaxy Survey (DGS), and the HeViCS Bright Galaxy Catalogue (BGC). We explore the relations between stellar mass and H i fraction, speciﬁc star formation rate, dust fraction, gas-to-dust ratio over a wide range of stellar masses (from 10 7 to 10 11 M (cid:3) ) for both dwarfs and spirals. Highly H i -deﬁcient Virgo dwarf galaxies are mostly characterised by quenched star formation activity and lower dust fractions giving hints for dust stripping in cluster dwarfs. However, to explain the large dust-to-gas mass ratios observed in these systems, we ﬁnd that the fraction of dust removed has to be less than that of the H i component. The cluster environment seems to mostly a ﬀ ect the gas component and star formation activity of the dwarfs. Since the Virgo star-forming dwarfs are likely to be crossing the cluster for the ﬁrst time, a longer timescale might be necessary to strip the more centrally concentrated dust distribution.
Impact of mineral nutrients on powdery mildew and quality attributes in umran ber (Ziziphus mauritiana)

An experiment was conducted at the Fruit Research Farm of Punjab Agricultural University, Ludhiana, Punjab during 2019–20 to study the impact of mineral nutrients on fruit drop, powdery mildew and quality attributes of ber (Ziziphus mauritiana Lam.) cv. Umran. A 15 year’s old ber plants were sprayed with nutrients like calcium nitrate @0.25 and 0.50%; potassium sulphate @0.25 and 0.50%; boric acid @0.40 and 0.60% and liquid sulphur @0.25 and 0.50% along with control (water spray) during mid-November, mid-December and mid-January (2019–20). Fruit drop and powdery mildew incidence was recorded periodically from November-March. Ber fruits were analysed for physical and bio-chemical parameters after harvesting. Among all the foliar applications, potassium sulphate @0.50% resulted in minimum fruit drop (65.52%). Maximum fruit length (4.86 cm), fruit diameter (3.06 cm), pulp content (93.96%) and fruit colour values (59.50, -4.0 and 33.46) was also recorded in potassium sulphate applied @0.50%. Maximum TSS (15.63 0B), TSS/acid ratio (120.23), ascorbic acid content (110.25 mg/100 g), total sugars (12.70%), reducing sugars (5.75%), non-reducing sugars (6.60%) and minimum titrable acidity (0.130%) was recorded with boric acid @0.60% which was statistically at par with potassium sulphate @0.50%. However, minimum incidence of powdery mildew was observed in liquid sulphur (0.50%) followed by potassium sulphate (0.50%). From the present studies, it is concluded that 3 foliar applications of potassium sulphate @0.50% resulted in improved quality attributes, reduction in fruit drop as well as reduced incidence of powdery mildew in ber cv. Umran.
Sea slugs (Gastropoda: Heterobranchia) from Rio Grande do Norte, Northeastern Brazil

Heterobranch sea slugs (Gastropoda) present reduction, internalization, or absence of shell, and include more than 6,000 described species. Approximately 250 species are recorded from Brazil but only 14 had been previously recorded from Rio Grande do Norte, on the Brazilian northeastern coast. As a result of different expeditions conducted between 2008 and 2020, species were collected and identified. Among them, five species were recorded for the first time from the South Atlantic Ocean: Chelidonura hirundinina (Quoy & Gaimard, 1833); Sclerodoris prea (Ev. Marcus & Er. Marcus, 1967); Thuridilla malaquita Ortea & Buske, 2014; Berthella nebula Ghanimi, Schrödl, Goddard, Ballesteros, Gosliner & Valdés, 2020 and Berthella vialactea Ghanimi, Schrödl, Goddard, Ballesteros, Gosliner & Valdés, 2020. Thirty-six species are recorded for the first time from Rio Grande do Norte. The present survey expands the knowledge of the diversity of sea slugs from Brazil and supports the hypothesis of similarity between the heterobranch sea slug fauna from the northeastern Brazil and the Caribbean Sea.
Low-redshift Lyman limit systems as diagnostics of cosmological inflows and outflows

We use cosmological hydrodynamic simulations with stellar feedback from the FIRE (Feedback In Realistic Environments) project to study the physical nature of Lyman limit systems (LLSs) at z ≤ 1. At these low redshifts, LLSs are closely associated with dense gas structures surrounding galaxies, such as galactic winds, dwarf satellites and cool inflows from the intergalactic medium. Our analysis is based on 14 zoom-in simulations covering the halo mass range M_h ≈ 10^9–10^(13) M⊙ at z = 0, which we convolve with the dark matter halo mass function to produce cosmological statistics. We find that the majority of cosmologically selected LLSs are associated with haloes in the mass range 10^(10) ≲ M_h ≲ 10^(12) M⊙. The incidence and H I column density distribution of simulated absorbers with columns in the range 10^(16.2)≤N_(HI)≤2×10^(20) Cm^(−2) are consistent with observations. High-velocity outflows (with radial velocity exceeding the halo circular velocity by a factor of ≳ 2) tend to have higher metallicities ([X/H] ∼ −0.5) while very low metallicity ([X/H] < −2) LLSs are typically associated with gas infalling from the intergalactic medium. However, most LLSs occupy an intermediate region in metallicity-radial velocity space, for which there is no clear trend between metallicity and radial kinematics. The overall simulated LLS metallicity distribution has a mean (standard deviation) [X/H] = −0.9 (0.4) and does not show significant evidence for bimodality, in contrast to recent observational studies, but consistent with LLSs arising from haloes with a broad range of masses and metallicities.