Miracle-dz/UniFAR-FTUs huggingface dataset:
Discovery of the supernova remnant G351.0-5.4

Context. While searching the NRAO VLA Sky Survey (NVSS) for diffuse radio emission, we have serendipitously discovered extended radio emission close to the Galactic plane. The radio morphology suggests the presence of a previously unknown Galactic supernova remnant. An unclassified {\gamma}-ray source detected by EGRET (3EG J1744-3934) is present in the same location and may stem from the interaction between high-speed particles escaping the remnant and the surrounding interstellar medium. Aims. Our aim is to confirm the presence of a previously unknown supernova remnant and to determine a possible association with the {\gamma}-ray emission 3EG J1744-3934. Methods. We have conducted optical and radio follow-ups of the target using the Dark Energy Camera (DECam) on the Blanco telescope at Cerro Tololo Inter-American Observatory (CTIO) and the Giant Meterwave Radio Telescope (GMRT). We then combined these data with archival radio and {\gamma}-ray observations. Results. While we detected the extended emission in four different radio bands (325, 1400, 2417, and 4850 MHz), no optical counterpart has been identified. Given its morphology and brightness, it is likely that the radio emission is caused by an old supernova remnant no longer visible in the optical band. Although an unclassified EGRET source is co-located with the supernova remnant, Fermi-LAT data do not show a significant {\gamma}-ray excess that is correlated with the radio emission. However, in the radial distribution of the {\gamma}-ray events, a spatially extended feature is related with SNR at a confidence level $\sim 1.5$ {\sigma}. Conclusions. We classify the newly discovered extended emission in the radio band as the old remnant of a previously unknown Galactic supernova: SNR G351.0-5.4.
Opleiding Informatica Clustering ﬁnancial transactions on inference-accelerator hardware

This thesis compares diﬀerent methods to accurately cluster similar and recurring ﬁnancial transactions, which is similar to clustering short text documents, and examines the use of ‘Tensor Cores’ –dedicated matrix multiplication cores– in NVIDIA hardware to increase performance. To extract features from ﬁnancial transactions, N-gram character tokenization is mainly used. We compare four similarity metrics: Cosine similarity, Kumar-Hassebrook similarity, Dice similarity and Dice squared similarity. We also compare four diﬀerent clustering methods: perceptron-based classiﬁcation similarity learning, hierarchical agglomerative clustering using single-linkage and complete-linkage and HDBSCAN. These methods are applied and compared on a dataset of 2880 ﬁnancial transactions from a personal bank account covering multiple years and on a dataset of about 8000 transactions of the Financial Shared Service Centre of Leiden University, covering one month. In addition to this research, a prototype for a web-based clustering tool has been built.
Universal relation between thermal entropy and entanglement entropy in conformal field theories

Inspired by the holographic computation of large interval entanglement entropy of two dimensional conformal field theory at high temperature, it was proposed that the thermal entropy is related to the entanglement entropy as $S_{th}=\displaystyle{\lim_{l \to 0}(S_{EE}(R-l)-S_{EE}(l))}$. In this letter, we prove this relation for 2D CFT with discrete spectrum in two different ways. Moreover we discuss this relation for a 2D noncompact free scalar, which is a gapless CFT with continuous spectrum. We show that it could be recovered, after appropriately regularizing the theory.
THE NATURE OF DAMPED LYMAN-α AND Mg ii ABSORBERS EXPLORED THROUGH THEIR DUST CONTENTS

We estimate the abundance of dust in damped Lyman-α absorbers (DLAs) by statistically measuring the excess reddening they induce on their background quasars. We detect systematic reddening behind DLAs consistent with the SMC-type reddening curve and inconsistent with the Milky Way type. We find that the derived dust-to-gas ratio is, on average, inversely proportional to the column density of neutral hydrogen, implying that the amount of dust is constant, regardless of the column density of hydrogen. It means that the average metallicity is inversely proportional to the column density of hydrogen, unless the average dust-to-metal ratio varies with the hydrogen column density. This indicates that the prime origin of metals seen in DLAs is not by in situ star formation, with which is expected from the empirical star formation law, contrary to our observation. We interpret the metals observed in absorbers to be deposited dominantly from nearby galaxies by galactic winds ubiquitous in intergalactic space. When extrapolating the relation between dust-to-gas ratio and H i column density to lower column density, we find a value that is consistent with what is observed for Mg ii absorbers.
PAOLO: A Polarimeter Add-On for the LRS Optics at a Nasmyth focus of the TNG†

We describe a new polarimetric facility available at the Istituto Nazionale di AstroFisica / Telescopio Nazionale Galileo at La Palma, Canary islands. This facility, PAOLO (Polarimetric Add-On for the LRS Optics), is located at a Nasmyth focus of an alt-az telescope and requires a specific modeling in order to remove the time- and pointing position-dependent instrumental polarization. We also describe the opto-mechanical structure of the instrument and its calibration and present early examples of applications. (© 2014 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)
Time-resolved resonant photoionization of He using a time-dependent Feshbach method with ultrashort laser pulses

We study the resonant photoionization of the Helium atom subject to ultrashort laser pulses by using a Feshbach formalism in the time domain. We solve the projected time-dependent Schrodinger equation in terms of a configuration interaction spectral method, with a total wave function expanded with configurations defined within bound-like () and scattering-like () halfspaces. The method allows for accurate descriptions of both the atomic structure (energy positions and widths) as well as for the resonant photodynamics using ultrashort laser pulses. Special attention is given to the temporal formation of Fano profiles in the one- and two-photon ionization cross sections.
Simple Siamese Representation Learning with RGB-D Images

Siamese neural networks have become a common mechanism for self-supervised representation learning on images in the past few years. Inspired by the simplicity and strong performance of these models, especially SimSiam, we experiment with using Siamese network structures on representation learning for 3-dimensional data in the form of RGB-D images. While our initial results ﬁnd that our model does not perform as well as the baseline SimSiam, it achieves comparable performance, and we identify a few areas which could lead to model improvement.
A connectomics-based taxonomy of 1 mammals 2

Mammalian taxonomies are conventionally deﬁned by morphological traits and 11 genetics. How species differ in terms of neural circuits and whether inter-species differences in 12 neural circuit organization conform to these taxonomies is unknown. The main obstacle for the 13 comparison of neural architectures have been differences in network reconstruction techniques, 14 yielding species-speciﬁc connectomes that are not directly comparable to one another. Here we 15 comprehensively chart connectome organization across the mammalian phylogenetic spectrum 16 using a common reconstruction protocol. We analyze the mammalian MRI (MaMI) data set, a 17 database that encompasses high-resolution ex vivo structural and diffusion magnetic resonance 18 imaging (MRI) scans of 124 species across 12 taxonomic orders and 5 superorders, collected 19 using a uniﬁed MRI protocol. We assess similarity between species connectomes using two 20 methods: similarity of Laplacian eigenspectra and similarity of multiscale topological features. 21 We ﬁnd greater inter-species similarities among species within the same taxonomic order, 22 suggesting that connectome organization reﬂects established taxonomic relationships deﬁned by 23 morphology and genetics. While all connectomes retain hallmark global features and relative 24 proportions of connection classes, inter-species variation is driven by local regional connectivity 25 proﬁles. By encoding connectomes into a common frame of reference, these ﬁndings establish a 26 foundation for investigating how neural circuits change over phylogeny, forging a link from genes 27 to circuits to behaviour. taxonomies. We determine the extent to which connectome topology conforms to established taxonomic classes, and identify network features 90 that are associated with speciation.
Transporting and Evaluating Predictive Models in Different Environments

In many data-driven applications, transporting a model from one environment to another has always been challenging. When experiments are conducted on a specific location or population, the problem of whether the results can be applied to a new location or population arises. The majority of the work in this area assumes that some conditional probabilities are transportable, even though they can be affected by unmeasured variables. We propose methods for transporting predictive models learned in a source population to target when we have limited information about the target population. These methods can cancel out the effect of the unmeasured variables using the ratio of conditional probabilities. We test the proposed methods using forest fire and stroke datasets.
“ICE CUBES” IN THE CENTER OF THE MILKY WAY: WATER-ICE AND HYDROCARBONS IN THE CENTRAL PARSEC

The close environment of the central supermassive black hole of our Galaxy has been studied thoroughly for decades in order to shed light on the behavior of the central regions of galaxies in general and of active galaxies in particular. The Galactic center (GC) has shown a wealth of structures on different scales with a complicated mixture of early- and late-type stars, ionized and molecular gas, dust, and winds. Here we aim to study the distribution of water-ices and hydrocarbons in the central parsec, as well as along the line of sight. This study is made possible thanks to L-band spectroscopy. This spectral band, from 2.8 to 4.2 μm, hosts important signatures of the circumstellar medium and interstellar dense and diffuse media among which deep absorption features are attributed to water-ices and hydrocarbons. We observed the GC in the L band of the ISAAC spectrograph located on the UT1/VLT ESO telescope. By mapping the central half parsec using 27 slit positions, we were able to build the first data cube of the region in this wavelength domain. Thanks to a calibrator spectrum of the foreground extinction in the L band derived in a previous paper, we corrected our data cube for the line-of-sight extinction and validated our calibrator spectrum. The data show that a residual absorption due to water-ices and hydrocarbons is present in the corrected data cube. This suggests that the features are produced in the local environment of the GC, implying very low temperatures well below 80 K. This is in agreement with our finding of local CO ices in the central parsec described in Moultaka et al.
A Novel Discrete DGM (2, 1, t 2 ) Model Based on Stochastic Oscillation Sequence and Its Application

Tis article aims to improve the prediction accuracy of the grey model for stochastic oscillation sequence, to overcome the defect of the direct span from diference to diferential and to better depict the growth trend of data series. Firstly, the accelerated translation smoothing transformation is constructed, which transforms the stochastic oscillation sequence into the monotonic increasing sequence that is suitable for modeling. Secondly, the quadratic time power term is introduced to establish a novel discrete DGM (2, 1, t 2 ) model, then derive a novel simulation prediction formula, and analyze properties of this novel model; it was concluded that its application scope is expanded. Finally, a novel discrete DGM (2, 1, t 2 ) model based on a stochastic oscillation sequence is established to forecast a group of stochastic oscillation sequences with diferent amplitudes and two diferent city trafc fow series and compare the prediction accuracy with other grey models; the results show that the feasibility of this model is verifed and has good simulated prediction efect in the feld of trafc fow.
LOWER LIMITS ON ULTRAHIGH-ENERGY COSMIC RAY AND JET POWERS OF TeV BLAZARS

Lower limits on the power emitted in ultrahigh-energy cosmic rays (UHECRs), which are assumed to be protons with energy ≳ 1017–1020 eV, are derived for TeV blazars with the assumption that the observed TeV γ-rays are generated due to interactions of these protons with cosmic microwave photons. The limits depend on the spectrum of the injected UHECR protons. While for a −2.2 injection spectrum the lower limits on the powers emitted in UHECRs by 1ES 0229+200, 1ES 1101−232, and 1ES 0347−121 are lower than their respective synchrotron luminosities (∼1046 erg s−1), in the case of 1ES 1426+428 it exceeds the corresponding synchrotron luminosity by up to an order of magnitude. The proposed Auger North Observatory should be able to detect 4 × 1019 eV cosmic-ray (CR) protons from 1ES 1426+428 within a few years of operation and test the TeV γ-ray production model by UHECR energy losses while propagating along the line of sight or constrain the intergalactic magnetic field to be larger than ∼10−16 G in case of no detection. The lower limits on the apparent-isotropic jet power from accelerated 1010–1020 eV proton spectra in the blazar jet is of the order of the Eddington luminosity of a 109 M☉ black hole for a CR injection spectrum −2.2 or harder for all blazars considered except for 1ES 1426+428. In the case of the latter, the apparent-isotropic jet power exceeds the Eddington luminosity by an order of magnitude. For an injection spectrum softer than −2.2, as is required to fit the observed CR data above ∼1017–1018 eV, the Eddington luminosity is exceeded by the lower limits on the jet power for all blazars considered.
Loop quantum cosmology: a status report

Loop quantum cosmology (LQC) is the result of applying principles of loop quantum gravity (LQG) to cosmological settings. The distinguishing feature of LQC is the prominent role played by the quantum geometry effects of LQG. In particular, quantum geometry creates a brand new repulsive force which is totally negligible at low spacetime curvature but rises very rapidly in the Planck regime, overwhelming the classical gravitational attraction. In cosmological models, while Einstein's equations hold to an excellent degree of approximation at low curvature, they undergo major modifications in the Planck regime: for matter satisfying the usual energy conditions, any time a curvature invariant grows to the Planck scale, quantum geometry effects dilute it, thereby resolving singularities of general relativity. Quantum geometry corrections become more sophisticated as the models become richer. In particular, in anisotropic models, there are significant changes in the dynamics of shear potentials which tame their singular behavior in striking contrast to older results on anisotropies in bouncing models. Once singularities are resolved, the conceptual paradigm of cosmology changes and one has to revisit many of the standard issues—e.g. the ‘horizon problem’—from a new perspective. Such conceptual issues as well as potential observational consequences of the new Planck scale physics are being explored, especially within the inflationary paradigm. These considerations have given rise to a burst of activity in LQC in recent years, with contributions from quantum gravity experts, mathematical physicists and cosmologists. The goal of this review is to provide an overview of the current state of the art in LQC for three sets of audiences: young researchers interested in entering this area; the quantum gravity community in general and cosmologists who wish to apply LQC to probe modifications in the standard paradigm of the early universe. In this review, effort has been made to streamline the material so that each of these communities can read only the sections they are most interested in, without loss of continuity.
Properties of white dwarfs in Einstein-Λ gravity

In this paper, we explore the properties of white dwarfs with the modified TOV equation in Einstein-Λ gravity, the equilibrium configurations predict a maximum mass limit for white dwarfs same as the Chandrasekhar limit when Λ was very small (Λ<10−16 m−2), by increasing Λ, the maximum mass and radius of white dwarf decreases. We study effects of the cosmological constant on the physical properties of white dwarf such as M−ρc relation, M−R relation, Schwarzschild radius, average density, compactness, gravitational redshift and dynamical stability. The gravitational redshift is a decreasing function of the cosmological constant, because the gravitational redshift of white dwarf should be positive, we also find an upper limit for Λ, namely, Λ<3×10−14 m−2. Our results show that the white dwarfs follow the dynamical stability in Einstein-Λ gravity.
THE MURMUR OF THE HIDDEN MONSTER: CHANDRA'S DECADAL VIEW OF THE SUPERMASSIVE BLACK HOLE IN M31

The Andromeda galaxy (M31) hosts a central supermassive black hole (SMBH), known as M31*, which is remarkable for its mass (∼108 M☉) and extreme radiative quiescence. Over the past decade, the Chandra X-Ray Observatory has pointed to the center of M31 ∼100 times and accumulated a total exposure of ∼900 ks. Based on these observations, we present an X-ray study of a highly variable source that we associate with M31* based on positional coincidence. We find that M31* remained in a quiescent state from late 1999 to 2005, exhibiting an average 0.5–8 keV luminosity ≲1036 erg s-1, or only ∼10−10 of its Eddington luminosity. We report the discovery of an outburst that occurred on 2006 January 6 during which M31* radiated at ∼4.3 × 1037 erg s-1. After the outburst, M31* entered a more active state that apparently lasts to the present, which is characterized by frequent flux variability around an average luminosity of ∼4.8 × 1036 erg s-1. These flux variations are similar to the X-ray flares found in the SMBH of our Galaxy (Sgr A*), making M31* the second SMBH known to exhibit recurrent flares. Future coordinated X-ray/radio observations will provide useful constraints on the physical origin of the flaring emission and help rule out a possible stellar origin of the X-ray source.
Synthesis and Cytotoxic Activity of 1,2,4-Triazolo-Linked Bis-Indolyl Conjugates as Dual Inhibitors of Tankyrase and PI3K

A series of new 1,2,4-triazolo-linked bis-indolyl conjugates (15a–r) were prepared by multistep synthesis and evaluated for their cytotoxic activity against various human cancer cell lines. It was observed that they were more susceptible to colon and breast cancer cells. Conjugates 15o (IC50 = 2.04 μM) and 15r (IC50 = 0.85 μM) illustrated promising cytotoxicity compared to 5-fluorouracil (5-FU, IC50 = 5.31 μM) against the HT-29 cell line. Interestingly, 15o and 15r induced cell cycle arrest at the G0/G1 phase and disrupted the mitochondrial membrane potential. Moreover, these conjugates led to apoptosis in HT-29 at 2 μM and 1 μM, respectively, and also enhanced the total ROS production as well as the mitochondrial-generated ROS. Immunofluorescence and Western blot assays revealed that these conjugates reduced the expression levels of the PI3K-P85, β-catenin, TAB-182, β-actin, AXIN-2, and NF-κB markers that are involved in the β-catenin pathway of colorectal cancer. The results of the in silico docking studies of 15r and 15o further support their dual inhibitory behaviour against PI3K and tankyrase. Interestingly, the conjugates have adequate ADME-toxicity parameters based on the calculated results of the molecular dynamic simulations, as we found that these inhibitors (15r) influenced the conformational flexibility of the 4OA7 and 3L54 proteins.
Production and decay of radion in Randall–Sundrum model at a photon collider

A warped extra dimension model predicts an extra scalar particle beyond the Standard Model (SM) which is called a radion. Although interactions of the radion are similar to those of the Higgs boson in the SM, a relatively light radion (≲100 GeV) is not severely constrained from the Higgs search experiments at the LHC. In this paper we study discovery potential of the radion at a photon collider as an option of ILC. Owing to the trace anomaly of the energy–momentum tensor, both a production of radion in γγ collision and its decay to gluon pair are enhanced sizably. We find that the photon collider has a sensitivity for discovering the radion in low-mass region up to Λϕ~3 TeV, where Λϕ is a scale parameter which suppresses the interactions of radion to the SM particles.
Implications of a variable IMF for the interpretation of observations of galaxy populations

We investigate the effect of a metallicity-dependent stellar initial mass function (IMF), as deduced observationally by Martin-Navarro et al. (2015c), on the inferred stellar masses and star formation rates (SFRs) of a representative sample of 186,886 SDSS galaxies. Relative to a Chabrier IMF, for which we show the implied masses to be close to minimal, the inferred masses increase in both the low- and high-metallicity regimes due to the addition of stellar remnants and dwarf stars, respectively. The resulting galaxy stellar mass function (GSMF) shifts toward higher masses by 0.5 dex, without affecting the high-mass slope (and thus the need for effective quenching). The implied low-redshift SFR density increases by an order of magnitude. However, these results depend strongly on the assumed IMF parametrisation, which is not directly constrained by the observations. Varying the low-end IMF slope instead of the high-end IMF slope, while maintaining the same dwarf-to-giant ratio, results in a much more modest GSMF shift of 0.2 dex and a 10 per cent increase in the SFR density relative to the Chabrier IMF. A bottom-heavy IMF during the late, metal-rich evolutionary stage of a galaxy would help explain the rapid quenching and the bimodality in the galaxy population by on the one hand making galaxies less quenched (due to the continued formation of dwarf stars) and on the other hand reducing the gas consumption timescale. We conclude that the implications of the observational evidence for a variable IMF could vary from absolutely dramatic to mild but significant.
Regularization of the Hamiltonian constraint compatible with the spinfoam dynamics

We introduce a new regularization for Thiemann's Hamiltonian constraint. The resulting constraint can generate the 1-4 Pachner moves and is therefore more compatible with the dynamics defined by the spinfoam formalism. We calculate its matrix elements and observe the appearance of the 15j Wigner symbol in these.
New Inferences on Magma Dynamics in Melilitite‐Carbonatite Volcanoes: The Case Study of Mt. Vulture (Southern Italy)

This study provides the first micro‐thermometric data of fluid inclusions (FIs) in mafic loose (disaggregated) xenocrysts and ultramafic xenoliths in explosive products of the melilitite‐carbonatite Mt. Vulture volcano (southern Italy). Pure CO2 late stage FIs hosted in rock‐forming minerals of wehrlite xenoliths and clinopyroxene xenocrysts were trapped at the local crust‐mantle boundary (32 km). In contrast, trapping pressures within the loose olivine xenocrysts are from 3.2 to 4.5 kbar (8–13 km). Considering the ongoing degassing of mantle‐derived CO2 rich gases, together with seismic evidences of the presence of low amount of melts at depth, and the tectonic control of the past volcanic activity, our study opens new perspective about the hazardous nature of the “quiescent” melilitite‐carbonatite volcanoes.