Miracle-dz/UniFAR-FTUs huggingface dataset:
Singular dynamics of underscreened magnetic impurity models

We give a comprehensive analysis of the singular dynamics and of the low-energy fixed point of one-channel impurity $s\text{\ensuremath{-}}d$ models with ferromagnetic and underscreened antiferromagnetic couplings. We use the numerical renormalization group (NRG) to perform calculations at $T=0$. The spectral densities of the one-electron Green's functions and t-matrices are found to have very sharp cusps at the Fermi level $(\ensuremath{\omega}=0)$, but do not diverge. The approach of the Fermi level is governed by terms proportional to $1∕{\mathrm{ln}}^{2}(\ensuremath{\omega}∕{T}_{0})$ as $\ensuremath{\omega}\ensuremath{\rightarrow}0$. The scaled NRG energy levels show a slow convergence as $1∕(N+C)$ to their fixed point values, where $N$ is the iteration number and $C$ is a constant dependent on the coupling $J$ from which the low energy scale ${T}_{0}$ can be deduced, with a renormalized coupling $\stackrel{\ifmmode \tilde{}\else \~{}\fi{}}{J}(\ensuremath{\omega})=1∕\mathrm{ln}(\ensuremath{\omega}∕{T}_{0})$. We calculate also the dynamical spin susceptibility, and the elastic and inelastic scattering cross sections as a function of $\ensuremath{\omega}$. The inelastic scattering goes to zero as $\ensuremath{\omega}\ensuremath{\rightarrow}0$, as expected for a Fermi liquid, but anomalously slowly compared to the fully screened case. We obtain the asymptotic forms for the phase shifts for elastic scattering of the quasiparticles in the high-spin and low-spin channels. The asymptotic forms found for the one-electron Green's functions and $t$-matrices do not simply correspond to a perturbation expansion in powers of $\stackrel{\ifmmode \tilde{}\else \~{}\fi{}}{J}(\ensuremath{\omega})$.
Dynamical response to supernova-induced gas removal in two-component spherical galaxies

We investigate the dynamical response, in terms of size and velocity dispersion, to mass loss by supernovae in the formation of two-component spherical galaxies composed of baryons and dark matter. Three-dimensional deprojected de Vaucouleurs-like and exponential-like profiles for baryons embedded in truncated singular isothermal and homogeneous profiles for dark matter are considered. As a more realistic case, we also consider a dark matter profile proposed by Navarro, Frenk & White. For simplicity we assume that the dark matter distribution is not affected by mass loss and that the change of baryonic matter distribution is homologous. We found that the degree of the response depends on the fraction of dark matter in the region where baryons are distributed, so that dwarf spheroidal galaxies would be affected even in a dark halo if they had been formed by galaxy mergers in the envelope of the dark halo. Our results suggest that this scenario, combined with the dynamical response, would result in not only the observed trends but the dispersed characteristics of dwarf spheroidals.
Study of the optical properties of BiFeO3 under different heat treatment temperatures

It is known that the optical absorption property of a material is linked to its crystal structure. Therefore, it can be modified or displaced when the material is subjected to thermal treatments, generating displacements of the unit cell, atomic positions and bond angles of its atoms. In this work, the analysis of three samples of BiFeO3 powders subjected to different heat treatment temperatures was carried out to study their optical properties by analyzing the crystal structure, diffuse reflectance, Raman scattering spectroscopy, density of state and band structure. In the results, the pure phase and the hexagonal structure of the samples were identified, showing an increase in the angles between the Fe-O-Fe atoms when the material is thermally treated. The band gap (Egexperimental) of the BiFeO3 samples without and with treatment temperature showed direct and indirect transitions according to the Tauc equation, these values were 2.36, 2.11 and 2.19 eV for direct band gaps and 2.10, 1.58 and 1.85 eV for indirect band gaps. In the Raman scattering spectroscopy analysis, overtones were observed in the samples when a green laser with a wavelength of 532nm (2.33 eV) was applied. In the density of states, the maximum valence band formed by the O(2p) state and the minimum of the conduction band formed by the hybridization of the Fe(3d) and O(2p) states were identified. In the electronic band structure, indirect band gap values (Egtheoretical) of 2.274, 2.216 (500 °C) and 2.217 eV (600 °C) were found for the samples without and with heat treatment. It is concluded that BiFeO3 absorbs visible light and that its band gap can decrease by increasing the bond angle of Fe-O-Fe atoms when the sample is subjected to heat treatment. These results demonstrate the semiconductor property of BiFeO3 and can be applied to solar cells, batteries, hydrogen production, among other applications.
Characterization of molecular heterogeneity of colorectal cancer among Bangladeshi population by targeted next generation sequencing

Background Since the Sanger sequencing procedure was invented, scientists all over the world have been working to improve and further develop this cutting-edge technology. Next-generation sequencing (NGS) is a game-changing advancement and the ability to profile genetic changes in cancer in great detail has been made possible by recent advances in sequencing technology. Several studies produced high-quality data in terms of mutation identification, particularly in the areas of actionable or rarely mutated genes, epigenetics, and transcriptomics. The goal of this project is to look at genetic heterogeneity in Bangladeshi colorectal cancer patients so that cost-effective precision medicine can be developed applied in Bangladesh. Methods The mutational characteristics of 24 colorectal tumor samples from Bangladeshi patients were investigated using targeted next generation sequencing to explore the association of mutations with clinical aspects. A total of 50 genes were sequenced with an average target depth of 675X. Results The left-sided tumors had higher mutation frequencies in TP53, APC, and ATM, while the right-sided tumors had higher mutation frequencies in EZH2, HNF1A, HRAS, and PIK3CA. Almost all of the samples in this study had a mutation in FGFR3. Deleterious mutations in the APC gene (94%) provided a selective advantage to the nascent intestinal tumor cell via constitutional stimulation of the Wnt signal transduction pathway and chromosomal instability. CDKN2A nonsynonymous mutations were found in almost all patient samples, with the exception of one. In a different patient with three unique mutations, 17 samples (71%) had a mutation in SMAD4 located in exon5 (p.P223N) synonymous and nonsynonymous mutations (two in NGRI04, and one in NGRI10). Several genes, including ATM, CDH1, ERBB4, and FBXW7, have been identified as being significantly affected by TNM stages. Except for a few key colorectal cancer genes, a comparison of mutational characteristics with subjects from other countries independent data revealed that the identified mutational characteristics are largely Bangladesh-specific. Conclusion In Bangladesh, precision medicine development and use in colorectal cancer are poorly addressed. The pilot study will serve as a starting point for genomics research into colon cancer in poor-resource settings like Bangladesh. The relationship between metastasis and genomic markers will aid in the identification of prospective intervention markers and the development of therapeutic options at the individual level, resulting in the development of precision medicine.
Social Media Sensors to Detect Early Warnings of Influenza at Scale

Detecting early signs of an outbreak in a viral process is challenging due to its exponential nature, yet crucial given the benefits to public health it can provide. If available, the network structure where infection happens can provide rich information about the very early stages of viral outbreaks. For example, more central nodes have been used as social network sensors in biological or informational diffusion processes to detect early contagious outbreaks. Here we aim to put together both approaches to detect early warnings of a biological viral process (influenza-like illness, ILI), using its informational epidemic coverage in public social media. We use a large social media dataset covering three years in a country. We demonstrate that it is possible to use highly central users on the platform, more precisely high out-degree users from Twitter, as sensors to detect the early warning outbreaks of ILI in the physical world without monitoring the whole population. We also investigate other behavioral and content features that distinguish those early sensors in social media beyond centrality. We find that while high centrality on Twitter is the most distinctive feature of sensors, we see that they are more likely to talk about local news, language, politics, or government than the rest of the users. Our new approach could detect a better and smaller set of social sensors for epidemic outbreaks and is more operationally efficient and privacy respectful than previous ones, not requiring the collection of vast amounts of data.
Stochastic Tamed Navier–Stokes Equations on R: The Existence and the Uniqueness of Solutions and the Existence of an Invariant Measure

Röckner and Zhang (Probab Theory Relat Fields 145, 211–267, 2009) proved the existence of a unique strong solution to a stochastic tamed 3D Navier–Stokes equation in the whole space and for the periodic boundary case using a result from Stroock and Varadhan (Multidimensional diffusion processes, Springer, Berlin, 1979). In the latter case, they also proved the existence of an invariant measure. In this paper, we improve their results (but for a slightly simplified system) using a self-contained approach. In particular, we generalise their result about an estimate on the L4-norm of the solution from the torus to R3, see Lemma 5.1 and thus establish the existence of an invariant measure on R3 for a time-homogeneous damped tamed 3D Navier–Stokes equation, given by (6.1). Mathematics Subject Classification. Primary 60H15; Secondary 35R60, 35Q30, 76D05.
The cosmic gamma-ray spectrum between 0.3 and 27 MeV measured on Apollo 15.

The spectrum of the total (diffuse and discrete sources) cosmic gamma-ray background over the 0.3 to 27 MeV range was measured with a 7.0 cm diameter x 7.0 cm long uncollimated NaI(Tl) scintillation counter located on a boom 7.6 m from the Apollo 15 service module. Data on cosmic gamma-rays were taken during transearth coast at various boom extensions, detector gains, and with the plastic anticoincidence scintillator enabled and disabled.
A Very Sensitive 21 centimeter Survey for Galactic High-Velocity H I

Very sensitive H I 21 cm observations have been made in 860 directions at δ ≥ -43° in search of weak, Galactic, high-velocity H I emission lines at moderate and high Galactic latitudes. One-third of the observations were made toward extragalactic objects that are visible at optical and UV wavelengths. The median rms noise in the survey spectra is 3.4 mK, resulting in a median 4 σ detection level of N = 8 × 1017 cm-2 averaged over the 21′ beam of the telescope. High-velocity H I emission is detected in 37% of the directions; about half of the lines could not have been detected in previous surveys. The median FWHM of detected lines is 30.3 km s-1. High-velocity H I lines are seen down to the sensitivity limit of the survey, implying that there are likely lines at still lower values of N. The weakest lines have a kinematics and distribution on the sky similar to that of the strong lines and thus do not appear to be a new population. Most of the emission originates from objects which are extended over several degrees; only a few appear to be compact sources. At least 75%, and possibly as many as 90%, of the lines are associated with one of the major high-velocity complexes. With the increased sensitivity of this survey, the Magellanic Stream is seen to extend at least 10° to higher Galactic latitude than previously thought and to be more extended in longitude as well. Wright's Cloud near M33 has an extended low-N component in the direction of the Magellanic Stream. The bright H I features which have dominated most surveys may be mere clumps within larger structures, and not independent objects. Although there are many lines with low column density, their numbers do not increase as rapidly as N, so most of the H I mass in the high-velocity cloud phenomenon likely resides in the more prominent clouds.
The Gunn-Peterson Effect from Underdense Regions in a Photoionized Intergalactic Medium

We use the Zel'dovich approximation and another analytical approximation to calculate the evolution under gravitational instability of the underdense regions of a photoionized intergalactic medium (IGM). We find that over most of the spectrum of a quasar, the optical depth to $\lya$ scattering originates from gas in underdense regions, or voids. This causes the ratio of the median Gunn-Peterson (GP) absorption to the value for a uniform medium containing all the baryons in the universe to be very small, and to decrease as gravitational collapse proceeds. We apply our calculations to the observations of the intensity distribution in a $z=4.11$ quasar by Webb and coworkers. We show that if $\lya$ clouds arise from gravitational collapse, their observations must be interpreted as the first detection of the (fluctuating) GP effect, with a median value $\tau_{GP}\simeq 0.06$ at $z=4$. For typical low-density ($\Omega\sim 0.4$) cosmological models, this is consistent with the predicted baryon density from primordial nucleosynthesis, and the intensity of the ionizing background derived from the proximity effect. From the numerical simulations of Cen \etal, such models also predict correctly the number of $\lya$ absorption lines observed.
The primitive equations in the scaling-invariant space L ∞ ( L 1 )

Consider the primitive equations on R 2 × ( z 0 , z 1 ) with initial data a of the form a = a 1 + a 2 , where a 1 ∈ BUC σ ( R 2 ; L 1 ( z 0 , z 1 )) and a 2 ∈ L ∞ σ ( R 2 ; L 1 ( z 0 , z 1 )) . These spaces are scaling-invariant and represent the anisotropic character of these equations. It is shown that for a 1 arbitrary large and a 2 sufﬁciently small, this set of equations admits a unique strong solution which extends to a global one and is thus strongly globally well posed for these data provided a is periodic in the horizontal variables. The approach presented depends crucially on mapping properties of the hydrostatic Stokes semigroup in the L ∞ ( L 1 ) -setting. It can be seen as the counterpart of the classical iteration schemes for the Navier–Stokes equations, now for the primitive equations in the L ∞ ( L 1 ) -setting. × J , where J = ( z 0 , z 1 ) is an interval. Denoting the horizontal coordinates by x , y ∈ R 2 and the vertical one by z ∈ ( z 1 , z 2 ) , we use the notation ∇ H = (cid:6) ∂ x , ∂ y (cid:7) T , whereas (cid:4) denotes the three-dimensional Laplacian and ∇ and div the three-dimensional gradient and divergence operators. The velocity u of the ﬂuid is
Extinction of light in dispersive media with high particle concentrations: applicability limits of the interference approximation

We investigated the limits of applicability of the interference approximation (ITA), which is often used to calculate light fields in dispersive media with high particle concentrations. We analyzed the conditions under which the use of the ITA leads to an error in calculation of the dispersive-medium extinction coefficient ∊ equal to 10%, 15%, and 25%. The analysis was carried out by comparing the values of ∊ calculated in the ITA with the results of the calculation of ∊ in a much more exact quasi-crystalline approximation (QCA). The validity of the QCA in estimating the error of the ITA is shown by comparing the values of ∊ calculated in the ITA and the QCA with experimental data [J. Opt. Soc. Am.72, 1317 (1982)]. Our investigation shows that the ITA can be used only at relatively small values of the particle size parameter x. When the relative refractive index of the particles is n≳1.8, the applicability of the ITA is limited to the case in which the particle size parameter x⩽xmax≈1.5. A decrease in n leads to an increase in xmax, and for nonabsorbing particles at n≲1.3,xmax is approximately proportional: 1/(n-1). An increase in the imaginary part of the relative refractive index of the particles κ leads to a decrease in xmax. The smaller the n, the greater the dependence of xmax on κ.
Acceleration of X-Ray Emitting Electrons in the Crab Nebula

We study particle acceleration at the termination shock of a striped pulsar wind by integrating trajectories in a prescribed model of the magnetic field and flow pattern. Drift motion on the shock surface maintains either electrons or positrons on “Speiser” orbits in a ring-shaped region close to the equatorial plane of the pulsar, enabling them to be accelerated to very high energy by the first-order Fermi mechanism. A power-law spectrum results: , where αe lies in the range −1.8 to −2.4 and depends on the downstream turbulence level. For sufficiently strong turbulence, we find αe ≃ −2.2, and both the photon index and the flux of 1–100 keV X-rays from the Crab Nebula, as measured by NuSTAR, can be reproduced. The particle spectrum hardens to αe ≃ −1.8 at lower turbulence levels, which may explain the hard photon index observed by the Chandra X-ray Observatory in the central regions of the Nebula.
Superhumps in Cataclysmic Binaries. XXIV. Twenty More Dwarf Novae

We report precise measures of the orbital and superhump period in 20 more dwarf novae. For 10 stars, we report new and confirmed spectroscopic periods—signifying the orbital period Po—as well as the superhump period Psh. These are GX Cas, HO Del, HS Vir, BC UMa, RZ Leo, KV Dra, KS UMa, TU Crt, QW Ser, and RZ Sge. For the remaining 10, we report a medley of Po and Psh measurements from photometry; most are new, with some confirmations of previous values. These are KV And, LL And, WX Cet, MM Hya, AO Oct, V2051 Oph, NY Ser, KK Tel, HV Vir, and RX J1155.4−5641. Periods, as usual, can be measured to high accuracy, and these are of special interest since they carry dynamical information about the binary. We still have not quite learned how to read the music, but a few things are clear. The fractional superhump excess ε[= (Psh - Po)/Po] varies smoothly with Po. The scatter of the points about that smooth curve is quite low, and can be used to limit the intrinsic scatter in M1, the white dwarf mass, and the mass‐radius relation of the secondary. The dispersion in M1 does not exceed 24%, and the secondary‐star radii scatter by no more than 11% from a fixed mass‐radius relation. For the well‐behaved part of ε(Po) space, we estimate from superhump theory that the secondaries are 18% ± 6% larger than theoretical ZAMS stars. This affects some other testable predictions about the secondaries: at a fixed Po, it suggests that the secondaries are (compared with ZAMS predictions) 40% ± 14% less massive, 12% ± 4% smaller, 19% ± 6% cooler, and less luminous by a factor of 2.5(7). The presence of a well‐defined mass‐radius relation, reflected in a well‐defined ε(Po) relation, strongly limits effects of nuclear evolution in the secondaries.
On the Redshift of TeV BL Lac Objects

We report results of a spectroscopic campaign carried out at the 10 m Gran Telescopio Canarias for a sample of 22 BL Lac objects detected (or candidates) at TeV energies, aiming to determine or constrain their redshift. This is of fundamental importance for the interpretation of their emission models and for population studies and is also mandatory for studying the interaction of high-energy photons with the extragalactic background light using TeV sources. Optical spectra with high signal-to-noise ratios in the range 4250–10000 Å were obtained to search for faint emission or absorption lines from both the host galaxy and the nucleus. We determine a new redshift for PKS 1424+240 (z = 0.604) and a tentative one for 1ES 0033+595 (z = 0.467). We are able to set new spectroscopic redshift lower limits for three other sources on the basis of Mg ii and Ca ii intervening absorption features: BZB J1243+3627 (z > 0.483), BZB J1540+8155 (z > 0.672), and BZB 0J2323+4210 (z > 0.267). We confirm previous redshift estimates for four blazars: S3 0218+357 (z = 0.944), 1ES 1215+303 (z = 0.129), W Comae (z = 0.102), and MS 1221.8+2452 (z = 0.218). For the remaining targets, in seven cases (S2 0109+22, 3C 66A, VER J0521+211, S4 0954+65, BZB J1120+4214, S3 1227+25, BZB J2323+4210), we do not validate the proposed redshift. Finally, for all sources of still-unknown redshift, we set a lower limit based on the minimum equivalent width of absorption features expected from the host galaxy.
Stable mode locking via ground- or excited-state transitions in a two-section quantum-dot laser

The authors demonstrate stable mode locking that involves transitions within either the ground state (1260nm) or the excited state (1190nm) in a two-section quantum-dot laser, at repetition frequencies of 21 and 20.5GHz, respectively. The average power of the mode-locked output was in excess of 35mW for operation in the ground state and 25mW in the excited state. The selection of pulse generation between these states in the mode-locking regime is controlled by the electrical biasing conditions.
Hecke algebras for GL n over local ﬁelds

We study the local Hecke algebra H G ( K ) for G = GL n and K a non-archimedean local ﬁeld of characteristic zero. We show that for G = GL 2 and any two such ﬁelds K and L , there is a Morita equivalence H G ( K ) ∼ M H G ( L ), by using the Bernstein decomposition of the Hecke algebra and determining the intertwining algebras that yield the Bernstein blocks up to Morita equivalence. By contrast, we prove that for G = GL n , there is an algebra isomorphism H G ( K ) ∼ = H G ( L ) which is an isometry for the induced L 1 -norm if and only if there is a ﬁeld isomorphism K ∼ = L
Microstructure and continuous phase transition of a Reissner-Nordstrom-AdS black hole

As is well known that RN-AdS black hole has a phase transition which is similar to that of van der Waals system. The phase transition depends on the electric potential of the black hole and is not the one between a large black hole and a small black hole. On this basis, we introduce a new order parameter and use the Landau continuous phase transition theory to discuss the critical phenomenon of RN-AdS black hole and give the critical exponent. By constructing the binary fluid model of black hole molecules, we investigate the microstructure of black holes. Furthermore, by studying the effect of the spacetime scalar curvature on the phase transition, we find that the charged and uncharged molecules of black holes are with different microstructure red which is like fermion gas and boson gas.
p(x)-Laplacian with indefinite weight

We consider the eigenvalue problem −div ( |∇u|p(x)−2∇u ) = λV (x)|u|q(x)−2u, in Ω, u = 0 on ∂Ω, where Ω is a smooth bounded domain in R N , λ > 0, p, q are continuous functions on Ω and V is a given function in a generalized Lebesgue space Ls(x)(Ω) such that V > 0 in an open set Ω0 ⊂ Ω, where |Ω0| > 0. We prove under appropriate conditions on the functions p, q and s that any λ > 0 sufficiently small is an eigenvalue of the above nonhomogeneous quasilinear problem. The proof relies on simple variational arguments based on Ekeland’s variational principle.