Miracle-dz/UniFAR-FTUs huggingface dataset:
The evolution of late-type galaxies from CASSOWARY lensing systems

We explore the properties of lensing galaxies and lensed faint sources at redshifts between 1.5 and 3.0. Our sample consists of 9 carefully selected strongly-lensed galaxies discovered by the CASSOWARY survey in the Sloan Digital Sky Survey (SDSS) data. We find that, despite some limitations of the original SDSS data, the homogeneous sample of lensing systems can provide a useful insight into lens and source properties. We also explore the limitations of using low-resolution data to model and analyse galaxy-galaxy lensing. We derive the relative alignment of mass and light in fitted lens profiles. The range of magnification extends above 5, hence we are able to analyse potentially small and low-mass galaxies at high redshifts. We confirm the likely evolution of the size-luminosity relation for blue star-forming galaxies as a function of redshift
MAGNETIC UNTWISTING IN SOLAR JETS THAT GO INTO THE OUTER CORONA IN POLAR CORONAL HOLES

We study 14 large solar jets observed in polar coronal holes. In EUV movies from the Solar Dynamics Observatory/Atmospheric Imaging Assembly (AIA), each jet appears similar to most X-ray jets and EUV jets that erupt in coronal holes; but each is exceptional in that it goes higher than most, so high that it is observed in the outer corona beyond 2.2 RSun in images from the Solar and Heliospheric Observatory/Large Angle Spectroscopic Coronagraph (LASCO)/C2 coronagraph. From AIA He ii 304 Å movies and LASCO/C2 running-difference images of these high-reaching jets, we find: (1) the front of the jet transits the corona below 2.2 RSun at a speed typically several times the sound speed; (2) each jet displays an exceptionally large amount of spin as it erupts; (3) in the outer corona, most of the jets display measureable swaying and bending of a few degrees in amplitude; in three jets the swaying is discernibly oscillatory with a period of order 1 hr. These characteristics suggest that the driver in these jets is a magnetic-untwisting wave that is basically a large-amplitude (i.e., nonlinear) torsional Alfvén wave that is put into the reconnected open field in the jet by interchange reconnection as the jet erupts. From the measured spinning and swaying, we estimate that the magnetic-untwisting wave loses most of its energy in the inner corona below 2.2 RSun. We point out that the torsional waves observed in Type-II spicules might dissipate in the corona in the same way as the magnetic-untwisting waves in our big jets, and thereby power much of the coronal heating in coronal holes.
Photometric Redshifts and Model Spectral Energy Distributions of Galaxies From the SDSS-III BOSS DR10 Data

We construct a set of model spectra specifically designed to match the colours of the BOSS CMASS galaxies and to be used with photometric redshift template fitting techniques. As a basis we use a set of spectral energy distributions (SEDs) of single and composite stellar population models. These models cannot describe well the whole colour range populated by the CMASS galaxies at all redshifts, wherefore we modify them by multiplying the SEDs with $\lambda^{-\beta}$ for $\lambda>\lambda_i$ for different values of $\lambda_i$ and $\beta$. When fitting these SEDs to the colours of the CMASS sample, with a burst and dust components in superposition, we can recreate the location in colour spaces inhabited by the CMASS galaxies. From the best fitting models we select a small subset in a two-dimensional plane, whereto the galaxies were mapped by a self-organizing map. These models are used for the estimation of photometric redshifts with a Bayesian template fitting code. The photometric redshifts with the novel templates have a very small outlier rate of $0.22\,\%$, a low bias $\langle\Delta z/(1+z)\rangle=2.0\cdot10^{-3}$, and scatter of $\sigma_{68}=0.026$ in the restframe. Using our models, the galaxy colours are reproduced to a better extent with the photometric redshifts of this work than with photometric redshifts of SDSS.
THE DIFFUSE GAMMA-RAY FLUX ASSOCIATED WITH SUB-PEV/PEV NEUTRINOS FROM STARBURST GALAXIES

One attractive scenario for the excess of sub-PeV/PeV neutrinos recently reported by IceCube is that they are produced by cosmic rays in starburst galaxies colliding with the dense interstellar medium. These proton–proton (pp) collisions also produce high-energy gamma rays, which finally contribute to the diffuse high-energy gamma-ray background. We calculate the diffuse gamma-ray flux with a semi-analytic approach and consider that the very high energy gamma rays will be absorbed in the galaxies and converted into electron–positron pairs, which then lose almost all of their energy through synchrotron radiation in the strong magnetic fields in the starburst region. Since the synchrotron emission goes into energies below GeV, this synchrotron loss reduces the diffuse high-energy gamma-ray flux by a factor of about two, thus leaving more room for other sources to contribute to the gamma-ray background. For an neutrino spectrum, we find that the diffuse gamma-ray flux contributes about 20% of the observed diffuse gamma-ray background in the 100 GeV range. However, for a steeper neutrino spectrum, this synchrotron loss effect is less important, since the energy fraction in absorbed gamma rays becomes lower.
A survey on graphs with convex quadratic stability number

ABSTRACT A graph with convex quadratic stability number is a graph for which the stability number is determined by solving a convex quadratic program. Since the very beginning, where a convex quadratic programming upper bound on the stability number was introduced, a necessary and sufficient condition for this upper bound be attained was deduced. The recognition of graphs with convex quadratic stability number has been deeply studied with several consequences from continuous and combinatorial point of view. This survey starts with an exposition of some extensions of the classical Motzkin–Straus approach to the determination of the stability number of a graph and its relations with the convex quadratic programming upper bound. The main advances, including several properties and alternative characterizations of graphs with convex quadratic stability number are described as well as the algorithmic strategies developed for their recognition. Open problems and a conjecture for a particular class of graphs, herein called adverse graphs, are presented, pointing out a research line which is a challenge between continuous and discrete problems.
Universal horizons in maximally symmetric spaces

Universal horizons in Ho\v{r}ava-Lifshitz gravity and Einstein-{\ae}ther theory are the equivalent of causal horizons in general relativity and appear to have many of the same properties, including a first law of horizon thermodynamics and thermal radiation. Since universal horizons are infrared solutions of a putative power counting renormalizable quantum gravitational theory, fully understanding their thermodynamics will shed light on the interplay between black hole thermodynamics and quantum gravity. In this paper, we provide a complete classification, including asymptotic charges, of all four dimensional static and spherically symmetric universal horizon solutions with maximally symmetric asymptotics -- the equivalents of the Schwarzschild, Schwarzschild de Sitter or Schwarzschild anti-de Sitter spacetimes. Additionally we derive the associated first laws for the universal horizon solutions. Finally we prove that independent of asymptotic boundary conditions, any spherically symmetric solution in Ho\v{r}ava-Lifshitz gravity with a universal horizon is also a solution of Einstein-{\ae}ther theory, thereby broadening and complementing the known equivalence region of the solution spaces.
IMPACT OF DIGITAL PAYMENTS ON THE ECONOMIC GROWTH OF A COUNTRY- A CASE OF THE CZECH REPUBLIC

: The way we pay has been evolving over a large period now with the slow fade out of paper money the digital system of payments is seen to pique the interests of consumers, institutions, and businesses. It is simply due to the more efficient features it displays over fiat money and this is what the paper tries to identify if whether there exists an impact of these digital payments over the economy of the Czech Republic by carrying out a linear and multiple regression employing selected indicators from 2015 to 2020. To test for heteroscedasticity in the obtained regression models the Breusch pagan test was employed. The results showed us that there does exist an impact of these digital payments but not enough that a switch or larger usage be employed to such a payment system this could also be due to the insufficient transactional value data available for such digital payments the access to more data can also allow to recognize the real demand of digital payment products by consumer which will enable more supply of digital payment system and providers, thus more wide-ranging research with more digital payment inclusive data could be carried out to identify the real impact of these payment systems over an economy.
Warm gas in the rotating disk of the Red Rectangle: accurate models of molecular line emission

We aim to study the excitation conditions of the molecular gas in the rotating disk of the Red Rectangle, the only post-Asymptotic-Giant-Branch object in which the existence of an equatorial rotating disk has been demonstrated. For this purpose, we developed a complex numerical code that accurately treats radiative transfer in 2-D, adapted to the study of molecular lines from rotating disks. We present far-infrared Herschel/HIFI observations of the 12CO and 13CO J=6-5, J=10-9, and J=16-15 transitions in the Red Rectangle. We also present our code in detail and discuss the accuracy of its predictions, from comparison with well-tested codes. Theoretical line profiles are compared with the empirical data to deduce the physical conditions in the disk by means of model fitting. We conclude that our code is very efficient and produces reliable results. The comparison of the theoretical predictions with our observations reveals that the temperature of the Red Rectangle disk is typically ~ 100-150 K, about twice as high as previously deduced from mm-wave observations of lower-J lines. We discuss the relevance of these new temperature estimates for understanding the thermodynamics and dynamics of this prototype object, as well as for interpreting observations of other rarely studied post-AGB disks. Despite our sophisticated treatment of the line formation, our model cannot explain the relatively strong line-wing emission for intermediate-J transitions. We argue that a model including a rotating disk only cannot reproduce these data and suggest that there is an additional extended (probably bipolar) structure expanding at about 7--15 km/s.
Communication Ethics in Online Learning at Vocational School of Sebelas Maret University During the Pandemic

For almost four semesters online learning has been implemented. From it, we want to describe the communication ethics of Vocational School of student class of 2020 at the University of Sebelas Maret (UNS) in online lectures during the pandemic by using the Zoom Meeting application. A descriptive survey is used in this research, data collection uses open-ended questionnaires. The unit being sampled is 20% of the population with simple random sampling and 34 lecturers returned the questionnaire with fill out google form, from a total sample of 40 lecturers. Purposeful sampling was also used for the first time to know legal rules regarding online lecture etiquette. The principal results are students adapt more quickly but the frequency that often appears in online lectures is students closing the camera, communication is more one-way, even though some show their IT skills above their friends. This major conclusion is normative ethics in online learning is not fully owned.
The Octave (Birmingham-Sheffield Hallam) automated pipeline for extracting oscillation parameters of solar-like main-sequence stars

The number of main-sequence stars for which we can observe solar-like oscillations is expected to increase considerably with the short-cadence high-precision photometric observations from the NASA Kepler satellite. Because of this increase in the number of stars, automated tools are needed to analyse these data in a reasonable amount of time. In the framework of the asteroFLAG consortium, we present an automated pipeline which extracts frequencies and other parameters of solar-like oscillations in main-sequence and subgiant stars. The pipeline uses only the time series data as input and does not require any other input information. Tests on 353 artificial stars reveal that we can obtain accurate frequencies and oscillation parameters for about three quarters of the stars. We conclude that our methods are well suited for the analysis of main-sequence stars, which show mainly p-mode oscillations.
An ab-initio study on physical properties of Pd2+ incorporated double perovskites CaPd3B4O12 (B = Ti, V)

Numerous physical properties of CaPd3Ti4O12 (CPTO) and CaPd3V4O12 (CPVO) double perovskites have been explored based on density functional theory (DFT). The calculated structural parameters fairly agree with the experimental data to confirm their stability. The mechanical stability of these two compounds was clearly observed by the Born stability criteria. To rationalize the mechanical behavior, we investigate elastic constants, bulk, shear and Young's modulus, Pugh's ratio, Poisson's ratio and elastic anisotropy index. The ductility index confirms that both materials are ductile in nature. The electronic band structure of CPTO and CPVO reveals the direct band gap semiconducting in nature and metallic characteristics, respectively. The calculated partial density of states indicates the strong hybridization between Pd 4d and O 2p orbital electrons for CPTO and Pd 4d and V 3d O 2p for CPVO. The study of electronic charge density map confirms the coexistence of covalent, ionic and metallic bonding for both compounds. Fermi surface calculation of CPVO ensures both electron and hole like surfaces indicating the multiple band nature. In the midst of optical properties, photoconductivity and absorption coefficient of both compounds reveal well qualitative compliance with consequences of band structure computations. Among the thermodynamic properties, the Debye temperature has been calculated to correlate its topical features including thermoelectric behavior. The studied thermoelectric transport properties of CPTO yielded the Seebeck coefficient (186 microVK-1), power factor (11.9 microWcm-1K-2) and figure of merit (ZT) value of about 0.8 at 800 K indicate that this material could be a promising candidate for thermoelectric device application.
A New Technique for Measuring Polycyclic Aromatic Hydrocarbon Emission in Different Environments

We present a new method to decompose the emission features of polycyclic aromatic hydrocarbons (PAHs) from mid-infrared spectra using theoretical PAH templates in conjunction with modified blackbody components for the dust continuum and an extinction term. The primary goal is to obtain robust measurements of the PAH features, which are sensitive to the star formation rate, in a variety of extragalactic environments. We demonstrate the effectiveness of our technique, starting with the simplest Galactic high-latitude clouds to extragalactic systems of ever-increasing complexity, from normal star-forming galaxies to low-luminosity active galaxies, quasars, and heavily obscured infrared-luminous galaxies. In addition to providing accurate measurements of the PAH emission, including the upper limits thereof, our fits can reproduce reasonably well the overall continuum shape and constrain the line-of-sight extinction. Our new PAH line flux measurements differ systematically and significantly from those of previous methods by ∼15% to as much as a factor of ∼6. The decomposed PAH spectra show remarkable similarity among different systems, suggesting a uniform set of conditions responsible for their excitation.
Dead Zone Accretion Flows in Protostellar Disks

Planets form inside protostellar disks in a dead zone where the electrical resistivity of the gas is too high for magnetic forces to drive turbulence. We show that much of the dead zone nevertheless is active and flows toward the star while smooth, large-scale magnetic fields transfer the orbital angular momentum radially outward. Stellar X-ray and radionuclide ionization sustain a weak coupling of the dead zone gas to the magnetic fields, despite the rapid recombination of free charges on dust grains. Net radial magnetic fields are generated in the magnetorotational turbulence in the electrically conducting top and bottom surface layers of the disk, and reach the midplane by ohmic diffusion. A toroidal component to the fields is produced near the midplane by the orbital shear. The process is similar to the magnetization of the solar tachocline. The result is a laminar, magnetically driven accretion flow in the region where the planets form.
Design of a coaxial and compact TM01–TE01 mode converter based on helical corrugated waveguide for high-power microwave system

In this paper, a novel X-band TM01–TE01 mode converter for high-power microwave (HPM) system is proposed. To realize the compact design, a helical corrugated waveguide with large deformation is employed to convert the TM01 mode into TE01 mode. By optimizing the structure parameters, the simulation results demonstrate that the maximum conversion efficiency of the proposed TM01–TE01 mode converter reaches 98.8% at 9.2 GHz. Moreover, this mode converter exhibits a conversion efficiency of over 95% in the operation band from 8.7 to 9.42 GHz, and the power capacity of the mode converter reaches GW-level in theory. More importantly, the overall longitudinal and transverse dimensions of the mode converter are less than three wavelengths. The results show the compact structure and high conversion efficiency of this mode converter, which has great potential application value in the HPM system.
Bayesian analysis of inflationary features in Planck and SDSS data

We perform a Bayesian analysis to study possible features in the primordial inflationary power spectrum of scalar perturbations. In particular, we analyse the possibility of detecting the imprint of these primordial features in the anisotropy temperature power spectrum of the Cosmic Microwave Background (CMB) and also in the matter power spectrum P (k). We use the most recent CMB data provided by the Planck Collaboration and P (k) measurements from the eleventh data release of the Sloan Digital Sky Survey. We focus our analysis on a class of potentials whose features are localised at different intervals of angular scales, corresponding to multipoles in the ranges 10 < l < 60 (Oscill-1) and 150 < l < 300 (Oscill-2). Our results show that one of the step-potentials (Oscill-1) provides a better fit to the CMB data than does the featureless LCDM scenario, with a moderate Bayesian evidence in favor of the former. Adding the P (k) data to the analysis weakens the evidence of the Oscill-1 potential relative to the standard model and strengthens the evidence of this latter scenario with respect to the Oscill-2 model.
Learning Based Multi-Channel Access in Vehicular Networks With Illegal Operators and Users

This paper investigates the multi-channel access (MCA) problem for vehicular networks in presence of illegal operators and users. Due to the limited spectrum resource, vehicle-to-vehicle (V2V) links need to reuse the frequency spectrum allocated for vehicle-to-infrastructure (V2I) links in networks. For high-mobility environments of vehicular networks, the fast-varying channel conditions will inevitably lead to the significant uncertainty of the acquired channel state information (CSI). Hence, the traditional centralized MCA methods, which rely on the CSI, could not be performed in a timely manner. We formulate the MCA of the vehicle users as a distributed optimization problem, by maximizing the sum capacity of V2I links while guaranteeing the reliability of V2V links as well as reducing the cost due to frequency hopping. A Multi-Agent Deep Deterministic Policy Gradient (MADDPG) framework is introduced to tackle this problem, where each vehicle user, connecting with either a V2I or V2V link, acts as a learning agent to make spectrum access decisions rapidly and locally to meet the latency requirement. In order to adapt to the dynamic environment, we further propose a delayed interaction aided MADDPG algorithm, which enables online training for the distributed MCA problem. Moreover, to guarantee the proposed algorithm to converge stably, we optimize the selecting weights of experience traces and propose a Batch Prioritized Experience Replay (BPER) strategy to ensure that the high priority traces can be learned timely. Compared with baselines, simulation results showcase remarkable performance gain of our proposed algorithm.
Eclipses and dust formation by WC9 type Wolf–Rayet stars

Visual photometry of 16 WC8-9 dust-making Wolf-Rayet (WR) stars during 2001--2009 was extracted from the All Sky Automated Survey All Star Catalogue (ASAS-3) to search for eclipses attributable to extinction by dust formed in clumps in our line of sight. Data for a comparable number of dust-free WC6-9 stars were also examined to help characterise the dataset. Frequent eclipses were observed from WR 104, and several from WR 106, extending the 1994-2001 studies by Kato et al. (2002a,b), but not supporting their phasing the variations in WR 104 with its `pinwheel' rotation period. Only four other stars showed eclipses, WR 50 (one of the dust-free stars), WR 69, WR 95 and WR 117, and there may have been an eclipse by WR 121, which had shown two eclipses in the past. No dust eclipses were shown by the `historic' eclipsers WR 103 and WR 113. The atmospheric eclipses of the latter were observed but the suggestion by David-Uraz et al. (2012) that dust may be partly responsible for these is not supported. Despite its frequent eclipses, there is no evidence in the infrared images of WR 104 for dust made in its eclipses, demonstrating that any dust formed in this process is not a significant contributor to its circumstellar dust cloud and suggesting that the same applies to the other stars showing fewer eclipses.
Supersymmetric Wilson loops with general contours in ABJM theory

We consider general supersymmetric Wilson loops in ABJM model, which is Chern–Simons-matter theory in (2+1) dimensions with 𝒩 = 6 supersymmetry. The Wilson loops of our interest are so-called Zarembo-type: they have generic contours in spacetime, but the scalar field coupling is arranged accordingly so that there are unbroken supersymmetries. Following the supermatrix construction of Wilson loops by Drukker and Trancanelli and the generalization by Griguolo et al., we study 1/6-BPS Wilson loops and check that their expectation value is protected using perturbation up to two loops. We also study the dual string configuration in AdS4×ℂℙ3 background and check the supersymmetry.