Miracle-dz/UniFAR-FTUs huggingface dataset:
Pulsational Pair-instability Supernovae. I. Pre-collapse Evolution and Pulsational Mass Ejection

We calculate the evolution of massive stars, which undergo pulsational pair-instability (PPI) when the O-rich core is formed. The evolution from the main sequence through the onset of PPI is calculated for stars with initial masses of 80–140 M⊙ and metallicities of Z = 10−3−1.0 Z⊙. Because of mass loss, Z ≤ 0.5 Z⊙ is necessary for stars to form He cores massive enough (i.e., mass >40 M⊙) to undergo PPI. The hydrodynamical phase of evolution from PPI through the beginning of Fe-core collapse is calculated for He cores with masses of 40−62 M⊙ and Z = 0. During PPI, electron–positron pair production causes a rapid contraction of the O-rich core, which triggers explosive O-burning and a pulsation of the core. We study the mass dependence of the pulsation dynamics, thermodynamics, and nucleosynthesis. The pulsations are stronger for more massive He cores and result in a large amount of mass ejection such as 3–13 M⊙ for 40−62 M⊙ He cores. These He cores eventually undergo Fe-core collapse. The 64 M⊙ He core undergoes complete disruption and becomes a pair-instability supernova. The H-free circumstellar matter ejected around these He cores is massive enough to explain the observed light curve of Type I (H-free) superluminous supernovae with circumstellar interaction. We also note that the mass ejection sets the maximum mass of black holes (BHs) to be ∼50 M⊙, which is consistent with the masses of BHs recently detected by VIRGO and aLIGO.
Magnetic field generation in PMS stars with and without radiative core

Abstract Recent observations of the magnetic field in pre-main sequence stars suggest that the magnetic field topology changes as a function of age. The presence of a tachocline could be an important factor in the development of magnetic field with higher multipolar modes. In this work we performed MHD simulations using the EULAG-MHD code to study the magnetic field generation and evolution in models that mimic stars at two evolutionary stages. The stratification for both stellar phases was computed by fitting stellar structure profiles obtained with the ATON stellar evolution code. The first stage is at 1.1Myr, when the star is completely convective. The second stage is at 14Myrs, when the star is partly convective, with a radiative core developed up to 30% of the stellar radius. In this proceedings we present a preliminary analysis of the resulting mean-flows and magnetic field. The mean-flow analysis shown that the star rotate almost rigidly on the fully convective phase, whereas at the partially convective phase there is differential rotation with conical contours of iso-rotation. As for the mean magnetic field both simulations show similarities with respect to the field evolution. However, the topology of the magnetic field is different.
AKARI NEAR-INFRARED SPECTROSCOPY OF LUMINOUS INFRARED GALAXIES

We present the AKARI near-infrared (NIR; 2.5–5 μm) spectroscopic study of 36 (ultra)luminous infrared galaxies ((U)LIRGs) at z = 0.01–0.4. We measure the NIR spectral features including the strengths of 3.3 μm polycyclic aromatic hydrocarbon emission and hydrogen recombination lines (Brα and Brβ), optical depths at 3.1 and 3.4 μm, and NIR continuum slope. These spectral features are used to identify optically elusive, buried active galactic nuclei (AGNs). We find that half of the (U)LIRGs optically classified as non-Seyferts show AGN signatures in their NIR spectra. Using a combined sample of (U)LIRGs with NIR spectra in the literature, we measure the contribution of buried AGNs to the infrared luminosity from the spectral energy distribution fitting to the IRAS photometry. The contribution of these buried AGNs to the infrared luminosity is 5%–10%, smaller than the typical AGN contribution of (U)LIRGs including Seyfert galaxies (10%–40%). We show that NIR continuum slopes correlate well with WISE [3.4]–[4.6] colors, which would be useful for identifying a large number of buried AGNs using the WISE data.
Absorption of 10-200 GeV Gamma Rays by Radiation from Broad-Line Regions in Blazars

In this paper, we study the photon-photon pair production optical depth for gamma rays with energies from 10 to 200 GeV emitted by powerful blazars due to the diffuse radiation field of the broad-line region (BLR). There are four key parameters in the BLR model employed to determine the γ-γ attenuation optical depth of these gamma rays. They are the gamma-ray emitting radius Rγ, the BLR luminosity LBLR, the BLR half thickness h, and the ratio τBLR/fcov of the Thomson optical depth to the covering factor of BLR. For FSRQs, on average, it is impossible for gamma rays with energies from 10 to 200 GeV to escape from the diffuse radiation field of the BLR. If GLAST could detect these gamma rays for most of FSRQs, the gamma-ray emitting region is likely to be outside the cavity formed by the BLR. Otherwise, the emitting region is likely to be inside the BLR cavity. As examples, we estimate the photon-photon absorption optical depth of gamma rays with energies from 10 to 200 GeV for two powerful blazars, HFSRQ PKS 0405-123 and FSRQ 3C 279. Comparing our results with GLAST observations in the future could test whether the model employed and the relevant assumptions in this paper are reliable and reasonable, and then limit constraints on the position of the gamma-ray emitting region relative to the BLR and the properties of the BLR.
Co-Treatment of Caco-2 Cells with Doxorubicin and Gold Nanoparticles Produced from Cyclopia intermedia Extracts or Mangiferin Enhances Drug Effects

Mangiferin (MGF) is a natural and valuable polyphenol found in significant levels in many plant species, including Cyclopia intermedia (C. intermedia). In a previous study, we synthesized gold nanoparticles (AuNPs) using MGF and a water extract of C. intermedia and reported that these AuNPs have very low cytotoxicity toward a human colon cancer (Caco-2) cell line. Although the study also showed that these biogenic AuNPs in combination with doxorubic (DOX) significantly augmented the cytotoxic effects of DOX in Caco-2 cells, the mechanism of the enhanced effect was not fully understood, and it was also not known if other cell lines would be sensitive to this co-treatment. In the present study, we examined the cytotoxicity of the co-treatment in Caski, HeLa, HT-29, KMST-6 and MDA-321 cell lines. Additionally, we investigated the mechanistic effects of this co-treatment in Caco-2 cells using several assays, including the adenosine triphosphate (ATP), the oxidative stress, the mitochondrial depolarization, the colony formation, the APOPercentage and the DNA fragmentation assays. We also assessed the intracellular uptake of the biogenic AuNPs. The study showed that the biogenic AuNPs were effectively taken up by the cancer cells, which, in turn, may have enhanced the sensitivity of Caco-2 cells to DOX. Moreover, the combination of the biogenic AuNPs and DOX caused a rapid depletion of ATP levels, increased mitochondrial depolarization, induced apoptosis, reduced the production of reactive oxygen species (ROS) and inhibited the long-term survival of Caco-2 cells. Although the study provided some insight into the mechanism of cytotoxicity induced by the co-treatment, further mechanistic and molecular studies are required to fully elucidate the enhanced anticancer effect of the co-treatment.
Noise and instability of an optical lattice clock

We present an analysis of the different types of noise from the detection and interrogation laser in our strontium lattice clock. We develop a noise model showing that in our setup quantum projection noise--limited detection is possible if more than 130~atoms are interrogated. Adding information about the noise spectrum of our clock laser with sub-$10^{-16}$ fractional frequency instability allows to infer the clock stability for different modes of operation. Excellent agreement with experimental observations for the instability of the difference between two interleaved stabilizations is found. We infer a clock instability of $1.6 \times 10^{-16}/\sqrt{\tau / \mathrm{s}}$ as a function of averaging time $\tau$ for normal clock operation.
VOLATILE-RICH CIRCUMSTELLAR GAS IN THE UNUSUAL 49 CETI DEBRIS DISK

We present Hubble Space Telescope Space Telescope Imaging Spectrograph far-UV spectra of the edge-on disk around 49 Ceti, one of the very few debris disks showing submillimeter CO emission. Many atomic absorption lines are present in the spectra, most of which arise from circumstellar gas lying along the line-of-sight to the central star. We determined the line-of-sight C i column density, estimated the total carbon column density, and set limits on the O i column density. Surprisingly, no line-of-sight CO absorption was seen. We discuss possible explanations for this non-detection, and present preliminary estimates of the carbon abundances in the line-of-sight gas. The C/Fe ratio is much greater than the solar value, suggesting that 49 Cet harbors a volatile-rich gas disk similar to that of β Pictoris.
Dynamics of Metaverse and Medicine: A Review Article

Metaverse is a relatively new concept of technological advancement for the world. Various sectors such as finance, entertainment, and communication are the forefront admirers of these innovations. Alongside these, the field of medicine has recently been on the list of metaverse-benefiting domains. Various aspects of medicine, such as educational and teaching purposes, surgical simulations, conferences and meetings, awareness programmes, research programmes, and many more, are under research. Depending on the requirement, the metaverse is a versatile platform which can be modulated accordingly, thus providing a flexible tool for medical development. In this review article, these domains are discussed in depth along with the pros and cons of the same, which positively affect the productivity of the field of medicine. All these headings have been through minimal study and experimentation, and the results obtained from them are satisfactory in terms of study. The primary purpose of the review article is to provide a suggestive statement regarding domains of the metaverse and their usage as a vital tool of operation in the future of medicine.
Proton CT -- a novel diagnostic tool in cancer therapy.

Radiotherapy is one of the main methods in the successful treatment of cancer. The tumor is irradiated with photons or charged particles (e.g. protons), and in the case of massive charged particles, the treatment results in less unnecessary dose outside the tumor and therefore less side effects for the patient and a faster recovery. However, the dose planning of hadron therapy is calculated from photon CT measurements, which results in large uncertainties in the planning and therefore in a necessary enlargement of the treatment area. This uncertainty can be reduced by performing the CT scan using protons. The current contribution shows the development of a sampling calorimeter for proton CT measurements and describes the state of the project.
So close, so different: characterization of the K2-36 planetary system with HARPS-N

Context. K2-36 is a K dwarf orbited by two small (Rb = 1.43 ± 0.08 R⊕ and Rc = 3.2 ± 0.3 R⊕), close-in (ab = 0.022 au and ac = 0.054 au) transiting planets discovered by the Kepler/K2 space observatory. They are representatives of two distinct families of small planets (Rp < 4 R⊕) recently emerged from the analysis of Kepler data, with likely a different structure, composition and evolutionary pathways. Aims. We revise the fundamental stellar parameters and the sizes of the planets, and provide the first measurement of their masses and bulk densities, which we use to infer their structure and composition. Methods. We observed K2-36 with the HARPS-N spectrograph over ~3.5 yr, collecting 81 useful radial velocity measurements. The star is active, with evidence for increasing levels of magnetic activity during the observing time span. The radial velocity scatter is ~17 m s−1 due to the stellar activity contribution, which is much larger that the semi-amplitudes of the planetary signals. We tested different methods for mitigating the stellar activity contribution to the radial velocity time variations and measuring the planet masses with good precision. Results. We find that K2-36 is likely a ~1 Gyr old system, and by treating the stellar activity through a Gaussian process regression, we measured the planet masses mb = 3.9 ± 1.1 M⊕ and mc = 7.8 ± 2.3 M⊕. The derived planet bulk densities ρb = 7.2−2.1+2.5 g cm−3 and ρc = 1.3−0.5+0.7 g cm−3 point out that K2-36 b has a rocky, Earth-like composition, and K2-36 c is a low-density sub-Neptune. Conclusions. Composed of two planets with similar orbital separations but different densities, K2-36 represents an optimal laboratory for testing the role of the atmospheric escape in driving the evolution of close-in, low-mass planets after ~1 Gyr from their formation. Due to their similarities, we performed a preliminary comparative analysis between the systems K2-36 and Kepler-36, which we deem worthy of a more detailed investigation.
Dual cascade and dissipation mechanisms in helical quantum turbulence

While in classical turbulence helicity depletes nonlinearity and can alter the evolution of turbulent flows, in quantum turbulence its role is not fully understood. We present numerical simulations of the free decay of a helical quantum turbulent flow using the Gross-Pitaevskii equation at high spatial resolution. The evolution has remarkable similarities with classical flows, which go as far as displaying a dual transfer of incompressible kinetic energy and helicity to small scales. Spatio-temporal analysis indicates that both quantities are dissipated at small scales through non-linear excitation of Kelvin waves and the subsequent emission of phonons. At the onset of the decay, the resulting turbulent flow displays polarized large scale structures and unpolarized patches of quiescense reminiscent of those observed in simulations of classical turbulence at very large Reynolds numbers.
Impact evaluation of households participation in agriculture on welfare in Ghana

The role of agriculture in Ghana’s economic development cannot be overstated as it is a major contributor to GDP and employs more people in the rural areas thereby improving on their welfare. However, the sector’s performance in recent time has declined as poverty incidence has remained high among rural agriculture households. This study, therefore, examines how participation in agriculture activities impact households’ welfare in Ghana using the seventh edition of Ghana Living Standard Survey (GLSS) dataset conducted in 2016/2017. The Heckman probit model is applied to determine the drivers of households' probability of engaging in agriculture. The propensity scores matching technique is used to match the farming households to their replica non-farming households as counterfactuals to ascertain the welfare impact of the households. The result shows that the welfare of households in agriculture is multidimensionally deprived than non-agriculture households. In addition, factors such as size of household, sex and age of household head, age at first marriage, location, ethnicity, and educational level of household heads have the likelihood of influencing agriculture participation in Ghana. Therefore, by modernising agriculture to enhance value addition through technology, irrigation, financing and marketing to boost agribusinesses would enhance the welfare in the agriculture households.
Structure Destruction and Content Combination for Generalizable Anti-Spoofing

In securing the face verification systems, prior face anti-spoofing studies excavate hidden cues in original images to discriminate real persons and diverse attacks with the assistance of auxiliary supervision. However, limited by several inherent shortcomings in their training process: 1) Neglect of the multi-scale nature of spoof cues; 2) Complete integral structure in a single image; 3) Implicit subdomains in the whole dataset, these methods are weak to mine comprehensive spoof patterns and may stick on memorization of the entire training dataset, incurring overfitting. In this paper, we propose a new framework named Destruction and Combination Network (DCN) including Multi-scale Representation Extraction Module, Structure Destruction Module, and Content Combination Module to address these limitations respectively. The first mechanism exploits multi-scale representation to learn spoof cues comprehensively. The second one destroys images into patches to construct non-structural inputs, and the last scheme recombines patches from different subdomains or classes into a mixup construction. Based on the above splitting-and-splicing operation, we further introduce Local Relation Modeling Module to model the second-order relationship between patches. To show the generalizable capacity of the proposed framework, besides simple intra-dataset testing, we test our method in cross-domain, cross-content, and cross-attack scenarios. Extensive experiments on different scenarios demonstrate the reliability of our method against state-of-the-art competitors.
Thermodynamic phase transitions from dynamical compact dimensions

We perform a double quotient of global AdS$_4$ and study its thermal properties. We find that a double quotient yields a spacetime with an expanding compact dimension. Studying the entanglement of the dual CFT we find that, at early times, the spacetime has thermal properties which disappear after a critical time. For slow expansion, this critical time depends on the expansion rate as expected, but becomes much more sensitive with more rapid expansion rates.
PROPERTIES OF THE INTERSTELLAR MEDIUM IN STAR-FORMING GALAXIES AT z ∼ 1.4 REVEALED WITH ALMA

We conducted observations of 12CO(J = 5–4) and dust thermal continuum emission toward 20 star-forming galaxies on the main sequence at z ∼ 1.4 using ALMA to investigate the properties of the interstellar medium. The sample galaxies are chosen to trace the distributions of star-forming galaxies in diagrams of stellar mass versus star formation rate and stellar mass versus metallicity. We detected CO emission lines from 11 galaxies. The molecular gas mass is derived by adopting a metallicity-dependent CO-to-H2 conversion factor and assuming a CO(5–4)/CO(1–0) luminosity ratio of 0.23. Masses of molecular gas and its fractions (molecular gas mass/(molecular gas mass + stellar mass)) for the detected galaxies are in the ranges of (3.9–12) × 1010 M⊙ and 0.25–0.94, respectively; these values are significantly larger than those in local spiral galaxies. The molecular gas mass fraction decreases with increasing stellar mass; the relation holds for four times lower stellar mass than that covered in previous studies, and the molecular gas mass fraction decreases with increasing metallicity. Stacking analyses also show the same trends. Dust thermal emissions were clearly detected from two galaxies and marginally detected from five galaxies. Dust masses of the detected galaxies are (3.9–38) × 107 M⊙. We derived gas-to-dust ratios and found they are 3–4 times larger than those in local galaxies. The depletion times of molecular gas for the detected galaxies are (1.4–36) × 108 yr while the results of the stacking analysis show ∼3 × 108 yr. The depletion time tends to decrease with increasing stellar mass and metallicity though the trend is not so significant, which contrasts with the trends in local galaxies.
Interplay between Quantumness, Randomness, and Selftesting

Quantum information processing shows advantages in many tasks, including quantum communication and computation, comparing to its classical counterpart. The essence of quantum processing lies on the fundamental difference between classical and quantum states. For a physical system, the coherent superposition on a computational basis is different from the statistical mixture of states in the same basis. Such coherent superposition endows the possibility of generating true random numbers, realizing parallel computing, and other classically impossible tasks such as quantum Bernoulli factory. Considering a system that consists of multiple parts, the coherent superposition that exists nonlocally on different systems is called entanglement. By properly manipulating entanglement, it is possible to realize computation and simulation tasks that are intractable with classical means. Investigating quantumness, coherent superposition, and entanglement can shed light on the original of quantum advantages and lead to the design of new quantum protocols. This thesis mainly focuses on the interplay between quantumness and two information tasks, randomness generation and selftesting quantum information processing. We discuss how quantumness can be used to generate randomness and show that randomness can in turn be used to quantify quantumness. In addition, we introduce the Bernoulli factory problem and present the quantum advantage with only coherence in both theory and experiment. Furthermore, we show a method to witness entanglement that is independent of the realization of the measurement. We also investigate randomness requirements in selftesting tasks and propose a random number generation scheme that is independent of the randomness source.
PRIMUS: ENHANCED SPECIFIC STAR FORMATION RATES IN CLOSE GALAXY PAIRS

Tidal interactions between galaxies can trigger star formation, which contributes to the global star formation rate (SFR) density of the universe and could be a factor in the transformation of blue, star-forming galaxies to red, quiescent galaxies over cosmic time. We investigate tidally triggered star formation in isolated close galaxy pairs drawn from the Prism Multi-Object Survey (PRIMUS), a low-dispersion prism redshift survey that has measured ∼120,000 robust galaxy redshifts over 9.1 deg2 out to z ∼ 1. We select a sample of galaxies in isolated galaxy pairs at redshifts 0.25 ⩽ z ⩽ 0.75, with no other objects within a projected separation of 300 h−1 kpc and Δz/(1 + z) = 0.01, and compare them to a control sample of isolated galaxies to test for systematic differences in their rest-frame FUV − r and NUV − r colors as a proxy for relative specific star formation rates (SSFRs). We find that galaxies in rp ⩽ 50 h−1 kpc pairs have bluer dust-corrected UV − r colors on average than the control galaxies by −0.134 ± 0.045 mag in FUV − r and −0.075 ± 0.038 mag in NUV − r, corresponding to an ∼15%–20% increase in SSFR. This indicates an enhancement in SSFR due to tidal interactions. We also find that this relative enhancement is greater for a subset of rp ⩽ 30 h−1 kpc pair galaxies, for which the average color offsets are −0.193 ± 0.065 mag in FUV − r and −0.159 ± 0.048 mag in NUV − r, corresponding to an ∼25%–30% increase in SSFR. We test for evolution in the enhancement of tidally triggered star formation with redshift across our sample redshift range and find marginal evidence for a decrease in SSFR enhancement from 0.25 ⩽ z ⩽ 0.5 to 0.5 ⩽ z ⩽ 0.75. This indicates that a change in enhanced star formation triggered by tidal interactions in low-density environments is not a contributor to the decline in the global SFR density across this redshift range.