Miracle-dz/UniFAR-FTUs huggingface dataset:
Towards the forecast of atmospheric parameters and optical turbulence above an astronomical site on 24h time scale

Forecast of the atmospheric parameters and optical turbulence applied to the ground-based astronomy is very crucial mainly for the queue scheduling. So far, most efforts have been addressed by our group in developing algorithms for the optical turbulence (C2N) and annexed integrated astroclimatic parameters and quantifying the performances of the Astro-Meso-Nh package in reconstructing such parameters. Besides, intensive analyses on the Meso-Nh performances= in reconstructing atmospheric parameters relevant for the ground-based astronomy has been carried out. Our studies referred always to the night time regime. To extend the applications of our studies to the day time regime, we present, in this contribution, preliminary results obtained by comparing model outputs and measurements of classical atmospheric parameter relevant for the ground-based astronomy in night and day time. We chose as a test case, the Roque de los Muchachos Observatory (Canary Islands), that offers a very extended set of measurements provided by different sensors belonging to different telescopes on the same summit/Observatory. The convective regime close to the ground typical of the day time is pretty different from the stable regime characterising the night time. This study aims therefore to enlarge the domain of validity of the Astro-Meso-Nh code to new turbulence regimes and it permits to cover the total 24 hours of a day. Such an approach will permit not only an application to solar telescopes (e.g. EST) but also applications to a much extended set of scientific fields, not only in astronomical context such as satellite communications.
Slicing Through Multicolor Space: Galaxy Redshifts from Broadband Photometry

As a means of better understanding the evolution of optically selected galaxies we consider the distribution of galaxies within the multicolor space $U$, $B_J$, $R_F$ and $I_N$. We find that they form an almost planar distribution out to $B_J =22.5$ and $z<0.3$. The position of a galaxy within this plane is dependent on its redshift, luminosity and spectral type. While in the original $U$, $B_J$, $R_F$ and $I_N$ space these properties are highly correlated we can define an optimal rotation of the photometric axes that makes much of this information orthogonal. Fitting the observed spectroscopic redshifts with a quadratic function of the four magnitudes we show that redshifts for galaxies can be estimated to an accuracy better than $\Delta z =0.05$. This dispersion is due to the photometric uncertainties within the photographic data. Assuming no galaxy evolution we derive a set of simulated galaxy fluxes in the U, J, F and N passbands. Using these data we investigate how the redshift is encoded within the broadband magnitudes and the intrinsic dispersion of the photometric-redshift relation. We find that the signal that defines a galaxy's photometric redshift is not related to specific absorption or emission lines but comes from the break in the overall shape of the galaxy continuum at around 4000 \AA. Using high signal-to-noise photometric data we estimate that it is possible to achieve an intrinsic dispersion of less than $\Delta z =0.02$.
EUS-guided left lobe liver biopsy: Safer modality with similar diagnostic yield as right lobe: a pilot study

Abstract Background and study aims Percutaneous liver biopsy is traditionally done on the right lobe of the liver. Endoscopic ultrasound-guided liver biopsy (EUS-LB) can be performed on either the left or right lobe or as a combined bi-lobar biopsy. Earlier studies did not compare the benefit of bi-lobar biopsies to single-lobe biopsy for reaching a tissue diagnosis. The current study compared the degree of agreement of pathological diagnosis between the left lobe of the liver compared to right-lobe and with bi-lobar biopsy. Patients and methods Fifty patients fulfilling the inclusion criteria were enrolled in the study. EUS-LB with a 22G core needle was performed separately on both the liver lobes. Three pathologists, who were blinded to the site of biopsy independently reviewed the liver biopsies. Sample adequacy, safety, and concordance of pathological diagnosis between left- and right-lobe biopsy of the liver were analyzed. Results The pathological diagnosis was made in 96 % of patients. Specimen lengths from the left lobe and the right lobe were 2.31 ± 0.57 cm and 2.28 ± 0.69 cm, respectively ( P = 0.476). The respective number of portal tracts were 11.84 ± 6.71 versus 9.58 ± 7.14; P = 0.106. Diagnosis between the two lobes showed substantial (κ = 0.830) concordance. Left-lobe (κ value 0.878) and right-lobe (κ = 0.903) biopsies showed no difference when compared with bi-lobar biopsies. Adverse events were observed in two patients, both of whom had biopsies of the right lobe. Conclusions EUS-guided left-lobe liver biopsy is safer than right-lobe biopsy with similar diagnostic yield.
A novel infrared forehead thermometer with ambient temperature compensation for body temperature measurement in low-temperature environment

Body temperature screening and measurement using infrared forehead thermometer (IFT), a non-contact thermometer, is an important method to prevent the spread of COVID-19 at present. However, low accuracy and unreliability of current IFT due to ambient temperature effect prevent it application in most of low-temperature environment. The aim of this study was to measure the body temperature accurately using IFT in low-temperature environment. A novel IFT with broad working temperature range and ambient temperature compensation was designed and fabricated, and the performance was evaluated. Also an ambient temperature compensation method based on Bluetooth module was introduced to improve the accuracy of body temperature measurement for the first time. The experiment results demonstrated that the laboratory indication error and repeatability in test mode of this developed IFT were all below 0.2℃ in ambient temperature range of (3~35) ℃. While the extended uncertainty for laboratory indication error was less than 0.1℃ (k=2). Compared with the contact electronic clinical thermometer, the difference of body temperature was improved within the scope of (-0.3~﹢0.3)℃ in low-temperature measurement environment. All the results showed that the IFT fabricated in this paper is sufficient and competent for body temperature screening and clinical body temperature measurement in most of low-temperature environment
Off-Policy Model-Free Learning for Multi-Player Non-Zero-Sum Games With Constrained Inputs

In this paper, multi-player non-zero-sum games with control constraints are studied by utilizing a novel model-free approach based on adaptive dynamic programming framework. First, the model-based policy iteration (PI) method is provided, which requires the system dynamics, and the convergence is demonstrated. Then, aiming to eliminate the need for the system dynamics, a model-free iterative method is obtained by using the off-policy integral reinforcement learning (IRL) scheme based on the PI approach. Moreover, the system data is collected in order to construct the model-free approach. Besides, we analyze the convergence of the off-policy IRL approach by proving the equivalence between the model-free iterative approach and the model-based iterative approach. Remarkably, in the implementation of the scheme, the control policy and cost function are approximated by utilizing the actor-critic networks. The least square algorithm is utilized to learn the actor-critic networks weights depended on the collected data sets. Finally, two cases are provided to demonstrate the effectiveness of the established framework.
Time‐domain modeling of pulsed finite‐amplitude sound beams

A time‐domain algorithm that solves the Khokhlov–Zabolotskaya–Kuznetsov (KZK) nonlinear parabolic wave equation is described. The algorithm models the propagation of pulsed finite amplitude sound beams radiated from axisymmetric sources in homogeneous, thermoviscous fluids. Numerical results are presented for waveform distortion and shock formation in directive beams radiated by pulsed circular pistons. Waveforms are calculated through the shock region and out to far‐field locations where they are dominated by the nonlinearly generated low‐frequency components. Effects of pulse duration, frequency modulation, and noise are examined. Methods for including relaxation and focusing are described.
Conductivity and capacitance of streamers in avalanche model for streamer propagation in dielectric liquids

Propagation of positive streamers in dielectric liquids, modeled by the electron avalanche mechanism, is simulated in a needle–plane gap. The streamer is modeled as an RC-circuit where the channel is a resistor and the extremities of the streamer have a capacitance towards the plane. The addition of the RC-model introduces a time constant to the propagation model. Increase in capacitance as a streamer branch propagates reduces its potential, while conduction through the streamer channel increases its potential, as a function of the time constant of the RC-system. Streamer branching also increases the capacitance and decreases the potential of the branches. If the electric field within the streamer channel exceeds a threshold, a breakdown occurs in the channel, and the potential of the streamer is equalized with the needle electrode. This is interpreted as a re-illumination. According to this model, a low conductive streamer branch can propagate some distance before its potential is reduced to below the propagation threshold, and then the RC time constant controls the streamer propagation speed. Channel breakdowns, or re-illuminations, are less frequent when the channels are conductive and more frequent for more branched streamers.
HST/WFPC2 morphologies and color maps of distant luminous infrared galaxies

Using HST/WFPC2 imaging in F606W (or F450W) and F814W filters, we obtained the color maps in observed frame for 36 distant (0.4 < z < 1.2) luminous infrared galaxies (LIRGs, L IR (8-1000 μm) ≥ 10 11 L ○. ), with average star formation rates of ∼100 M ○. yr -1 . Stars and compact sources are taken as references to align images after correction of geometric distortion. This leads to an alignment accuracy of 0.15 pixel, which is a prerequisite for studying the detailed color properties of galaxies with complex morphologies. A new method is developed to quantify the reliability of each pixel in the color map without any bias against very red or blue color regions. Based on analyses of two-dimensional structure and spatially resolved color distribution, we carried out morphological classification for LIRGs. About 36% of the LIRGs were classified as disk galaxies and 22% as irregulars. Only 6 (17%) systems are obvious ongoing major mergers. An upper limit of 58% was found for the fraction of mergers in LIRGs with all the possible merging/interacting systems included. Strikingly, the fraction of compact sources is as high as 25%, similar to that found in optically selected samples. From their K band luminosities, LIRGs are relatively massive systems, with an average stellar mass of about 1.1 x 10 11 M ○. They are related to the formation of massive and large disks, from their morphologies and also from the fact that they represent a significant fraction of distant disks selected by their sizes. If sustained at such large rates, their star formation can double their stellar masses in less than I Gyr. The compact LIRGs show blue cores, which could be associated with the formation of the central region of these galaxies. We find that all LIRGs are distributed along a sequence which relate their central color to their concentration index. This sequence links compact objects with blue central color to extended ones with relatively red central color, which are closer to the local disks. We suggest that there are many massive disks which have been forming a large fraction of their stellar mass since z = 1. For most of them, their central parts (bulge? ) were formed prior to the formation of their disks.
A Search for TeV Gamma-Ray Emission from the PSR B1259–63/SS 2883 Binary System with the CANGAROO-II 10 Meter Telescope

Observations of the PSR B1259-63/SS 2883 binary system using the CANGAROO-II Cerenkov telescope are reported. This nearby binary consists of a 48 ms radio pulsar in a highly eccentric orbit around a Be star and offers a unique laboratory to investigate the interactions between the outflows of the pulsar and Be star at various distances. It has been pointed out that the relativistic pulsar wind and the dense mass outflow of the Be star may result in the emission of gamma rays up to TeV energies. We have observed the binary in 2000 and 2001, ~47 and ~157 days after the 2000 October periastron. Upper limits at the 0.13-0.54 crab level are obtained. A new model calculation for high-energy gamma-ray emission from the Be star outflow is introduced, and the estimated gamma-ray flux, considering bremsstrahlung, inverse Compton scattering, and the decay of neutral pions produced in proton-proton interactions, is found to be comparable to the upper limits of these observations. Comparing our results with these model calculations, we constrain the mass-outflow parameters of the Be star.
Comparison of the blood gas analyser Edan i15 Vet with the blood gas analyser Gem Premier 3000 for the analysis of blood gases, electrolytes, hemoglobin and hematocrit in lactating Holstein

A point-of-care blood gas analyser, Edan i15 Vet (EDAN), was compared with a benchtop blood gas analyser, GEM Premier 3000 (GEM). GEM and EDAN were used to analyse whole blood from 123 lactating Holsteins within one month of calving for blood gases, electrolytes, hematocrit and hemoglobin. EDAN and GEM showed significant linear correlations for blood gases, electrolytes, Hct and Hb. The 95% confidence intervals (CI) of intercept in Passing-Bablok regressions included zero in pCO2, bicarbonate, TCO2, BE ecf, BE B, hematocrit, and pH, but not for Na+, K+, pO2 and sO2. The CI of the slope included 1.0 for Na+, K+, pCO2, bicarbonate, TCO2, BE ecf, BE B, hematocrit, and pH, but not for pO2, sO2, and hemoglobin. The Bland-Altman plots between EDAN and GEM showed a bias of 1.4% for Na+, 2.4% for K+, –1.6% for pCO2, 3.0% for pO2, –5.3% for bicarbonate, 2.8% for SO2, –7.3% for TCO2, 10.4% for Hct, 21.2% for Hb, –25.1% for BE B and –38.5% for BE ecf. The biases in the analysis of certain estimated parameters were much higher (> 5%) than for measured parameters except for Hct. Parity did not correlate with blood gas parameters but blood pH correlated negatively with K+, pCO2 and positively with pO2, TCO2, sO2, bicarbonate, BE ecf and BE B. The postpartum time correlated positively with pCO2, TCO2, BE and bicarbonate and negatively with Hct and Hb values. Reference values (2.5-97.5% quartiles) were determined for each parameter. Conclusively, EDAN can be used interchangeably with GEM for the analysis of blood pH, K+, pCO2 and HCO3 – as they show acceptable moderate agreement. However, they did not agree for other parameters such as TCO2, BE ecf, BE B, Hb, Hct, sO2, Na+, and pO2, therefore, reference values for each parameter were set for GEM and EDAN.
Spectral-spatial classification of hyperspectral images based on non-linear principal component analysis and deep learning models

ABSTRACT Hyperspectral sensors, due to the acquisition of a large number of spectral bands, always have particular importance in monitoring the phenomena of the earth’s surface. The classification of hyperspectral images is the most crucial method of processing hyperspectral data, and many efforts have been made to increase its accuracy. In recent years, convolutional neural networks (CNNs) and spatial features have been a big part of how well hyperspectral images can be classified. CNNs, due to the automatic generation of features and reduction of parameters, compared to multilayer perceptron neural networks by sharing parameters in each layer, have received much attention from researchers in the field of pattern recognition. In previous research, much attention has not been paid to the simultaneous use of spatial feature extraction methods in CNNs. For this reason, in this paper, a new CNNs architecture has been introduced to classify hyperspectral images, which uses the spectral-spatial vector obtained from the morphological profiles method as the network’s input. Morphological profiles, which include a set of opening and closing filters, are generally applied to the components of the image that contain the most information. In this research, non-linear principal component analysis (non-linear PCA) implemented by neural networks was used to summarize hyperspectral image information. Therefore, the main innovation of this paper is to provide a three-stage framework for applying deep learning. The first step is to reduce the dimensions of the hyperspectral image using non-linear PCA, the second stage is to extract spatial features using the morphological profiles method, and the third step is to prepare the inputs and design the CNNs architecture. The proposed method was evaluated on three benchmark hyperspectral images of Pavia, Berlin and Telops. The results of the experiments show the superiority of the proposed method by 13, 11 and 17% in the overall accuracy parameter compared to the support vector machines (SVM) classification algorithm in the Pavia, Berlin and Telops images, respectively.
Tsallis Entropy for Loss Models and Survival Models Involving Truncated and Censored Random Variables

The aim of this paper consists in developing an entropy-based approach to risk assessment for actuarial models involving truncated and censored random variables by using the Tsallis entropy measure. The effect of some partial insurance models, such as inflation, truncation and censoring from above and truncation and censoring from below upon the entropy of losses is investigated in this framework. Analytic expressions for the per-payment and per-loss entropies are obtained, and the relationship between these entropies are studied. The Tsallis entropy of losses of the right-truncated loss random variable corresponding to the per-loss risk model with a deductible d and a policy limit u is computed for the exponential, Weibull, χ2 or Gamma distribution. In this context, the properties of the resulting entropies, such as the residual loss entropy and the past loss entropy, are studied as a result of using a deductible and a policy limit, respectively. Relationships between these entropy measures are derived, and the combined effect of a deductible and a policy limit is also analyzed. By investigating residual and past entropies for survival models, the entropies of losses corresponding to the proportional hazard and proportional reversed hazard models are derived. The Tsallis entropy approach for actuarial models involving truncated and censored random variables is new and more realistic, since it allows a greater degree of flexibility and improves the modeling accuracy.
Electrically charged compact stars and formation of charged black holes

We study the effect of electric charge in compact stars assuming that the charge distribution is proportional to the mass density. The pressure and the density of the matter inside the stars are large, and the gravitational field is intense. This indicates that electric charge and a strong electric field can also be present. The relativistic hydrostatic equilibrium equation, i.e., the Tolman-Oppenheimer-Volkoff equation, is modified in order to include electric charge. We perform a detailed numerical study of the effect of electric charge using a polytropic equation of state. We conclude that in order to see any appreciable effect on the phenomenology of the compact stars, the electric fields have to be huge $(\ensuremath{\sim}{10}^{21}$ V/m), which implies that the total charge is $Q\ensuremath{\sim}{10}^{20}$ Coulomb. From the local effect of the forces experienced on a single charged particle, it is expected that each individual charged particle is quickly ejected from the star. This in turn produces a huge force imbalance, and the gravitational force overwhelms the repulsive Coulomb and fluid pressure forces. The star can then collapse to form a charged black hole before all the charge leaves the system.
Catalog of High Protostellar Surface Density Regions in Nearby Embedded Clusters

We analyze high-quality stellar catalogs for 24 young and nearby (within 1 kpc) embedded clusters and present a catalog of 32 groups which have a high concentration of protostars. The median effective radius of these groups is 0.17 pc. The median protostellar and pre-main-sequence star surface densities are 46 M⊙ pc−2 and 11 M⊙ pc−2, respectively. We estimate the age of these groups using a model of constant birthrate and random accretion stopping and find a median value of 0.25 Myr. Some groups in Aquila, Serpens, Corona Australia, and Ophichus L1688 show high protostellar surface density and high molecular gas surface density, and seem to be undergoing vigorous star formation. These groups provide an excellent opportunity to study the initial conditions of clustered star formation. Comparisons of protostellar and pre-main-sequence stellar surface densities reveal continuous low-mass star formation of these groups over several Myr in some clouds. For groups with typical protostellar separations of less than 0.4 pc, we find that these separations agree well with the thermal Jeans fragmentation scale. On the other hand, for groups with typical protostellar separations larger than 0.4 pc, these separations are always larger than the associated Jeans length.
Broadband Dynamic Rupture Modeling With Fractal Fault Roughness, Frictional Heterogeneity, Viscoelasticity and Topography: The 2016 Mw 6.2 Amatrice, Italy Earthquake

Advances in physics‐based earthquake simulations, utilizing high‐performance computing, have been exploited to better understand the generation and characteristics of the high‐frequency seismic wavefield. However, direct comparison to ground motion observations of a specific earthquake is challenging. We here propose a new approach to simulate data‐fused broadband ground motion synthetics using 3D dynamic rupture modeling of the 2016 Mw 6.2 Amatrice, Italy earthquake. We augment a smooth, best‐fitting model from Bayesian dynamic rupture source inversion of strong‐motion data (<1 Hz) with fractal fault roughness, frictional heterogeneities, viscoelastic attenuation, and topography. The required consistency to match long periods allows us to quantify the role of small‐scale dynamic source heterogeneities, such as the 3D roughness drag, from observational broadband seismic waveforms. We demonstrate that 3D data‐constrained fully dynamic rupture synthetics show good agreement with various observed ground‐motion metrics up to ∼5 Hz and are an important avenue toward non‐ergodic, physics‐based seismic hazard assessment.