Miracle-dz/UniFAR-FTUs huggingface dataset:
Large change in the predicted number of small halos due to a small amplitude oscillating inflaton potential

A smooth inflaton potential is generally assumed when calculating the primordial power spectrum, implicitly assuming that a very small oscillation in the inflaton potential creates a negligible change in the predicted halo mass function. We show that this is not true. We find that a small oscillating perturbation in the inflaton potential in the slow-roll regime can alter significantly the predicted number of small halos. A class of models derived from supergravity theories gives rise to inflaton potentials with a large number of steps and many trans-Planckian effects may generate oscillations in the primordial power spectrum. The potentials we study are the simple quadratic (chaotic inflation) potential with superimposed small oscillations for small field values. Without leaving the slow-roll regime, we find that for a wide choice of parameters, the predicted number of halos change appreciably. For the oscillations beginning in the ${10}^{7}\char21{}{10}^{8}{M}_{\ensuremath{\bigodot}}$ range, for example, we find that only a 5% change in the amplitude of the chaotic potential causes a 50% suppression of the number of halos for masses between ${10}^{7}\char21{}{10}^{8}{M}_{\ensuremath{\bigodot}}$ and an increase in the number of halos for masses $l{10}^{6}{M}_{\ensuremath{\bigodot}}$ by factors $\ensuremath{\sim}15\char21{}50$. We suggest that this might be a solution to the problem of the lack of observed dwarf galaxies in the range ${10}^{7}\char21{}{10}^{8}{M}_{\ensuremath{\bigodot}}$. This might also be a solution to the reionization problem where a very large number of Population III stars in low mass halos are required.
The UK Infrared Telescope M33 monitoring project – II. The star formation history in the central square kiloparsec

We have conducted a near-infrared monitoring campaign at the UK Infrared Telescope, of the Local Group spiral galaxy M33 (Triangulum). The main aim was to identify stars in the very final stage of their evolution, and for which the luminosity is more directly related to the birth mass than the more numerous less-evolved giant stars that continue to increase in luminosity. In this second paper of the series, we construct the birth mass function and hence derive the star formation history. The star formation rate has varied between ∼0.002 and 0.007 M⊙ yr ―1 kpc ―2 . We give evidence of two epochs of a star formation rate enhanced by a factor of a few - one that happened ≥6 Gyr ago and produced ≥80 per cent of the total mass in stars, and one around 250 Myr ago that lasted ∼200 Myr and formed ≤6 per cent of the mass in stars. We construct radial and azimuthal distributions in the image plane and in the galaxy plane for populations associated with old first-ascent red giant branch (RGB) stars, intermediate-age asymptotic giant branch (AGB) stars and young (massive) blue and red supergiants. We find that the RGB stars follow an spheroidal distribution, while younger stars follow a flat-disc distribution. The intermediate-age population displays signs of a pseudo-bulge or possibly a bar. The inner spiral arm pattern as recorded in mid-19th-century drawings is confirmed. We interpret our findings as evidence for an old, pressure-supported component and a younger disc formed 6 Gyr ago, with an accretion event occurring 250 Myr ago giving rise to the compact nucleus in M33. Our study provides support for recent Padova stellar evolution models except that super-AGB stars likely reach low temperatures and thus high mass-loss rates, supporting the super-AGB nature of the progenitors of dust-enshrouded supernovae such as SN 2008S.
Effects of carbon concentration and filament number on advanced internal Mg infiltration-processed MgB2 strands

In this paper we show that an advanced internal Mg infiltration method (AIMI) is effective in producing superconducting wires containing dense MgB2 layers with high critical current densities. The in-field critical current densities of a series of AIMI-fabricated MgB2 strands were investigated in terms of C doping levels, heat treatment (HT) time and filament numbers. The highest layer Jc for our monofilamentary AIMI strands was 1.5 × 105 A cm−2 at 10 T, 4.2 K, when the C concentration was 3 mol% and the strand was heat-treated at 675 ° C for 4 h. Transport critical currents were also measured at 4.2 K on short samples and 1 m segments of 18-filament C doped AIMI strands. The layer Jcs reached 4.3 × 105 A cm−2 at 5 T and 7.1 × 104 A cm−2 at 10 T, twice as high as those of the best powder-in-tube strands. The analysis of these results indicates that the AIMI strands, possessing both high layer Jcs and engineering Jes after further optimization, have strong potential for commercial applications.
Dust Radiative Transfer Modeling of the Infrared Ring around the Magnetar SGR 1900+14

A peculiar infrared ring-like structure was discovered by Spitzer around the strongly magnetized neutron star SGR 1900+14. This infrared (IR) structure was suggested to be due to a dust-free cavity, produced by the Soft Gamma-ray Repeaters (SGRs) Giant Flare occurring in 1998, and kept illuminated by surrounding stars. Using a 3D dust radiative transfer code, we aimed to reproduce the emission morphology and the integrated emission flux of this structure assuming different spatial distributions and densities for the dust, and different positions for the illuminating stars. We found that a dust-free ellipsoidal cavity can reproduce the shape, flux, and spectrum of the ring-like IR emission, provided that the illuminating stars are inside the cavity and that the interstellar medium has high gas density (nH ∼ 1000 cm−3). We further constrain the emitting region to have a sharp inner boundary and to be significantly extended in the radial direction, possibly even just a cavity in a smooth molecular cloud. We discuss possible scenarios for the formation of the dustless cavity and the particular geometry that allows it to be IR-bright.
The Effect of Short Chain Carboxylic Acids as Additives on the Crystallization of Methylammonium Lead Triiodide (MAPI)

Due to their exceptional properties, the study of hybrid perovskite (HyP) structures and applications dominate current photovoltaic prospects. Methylammonium lead tri-iodide perovskite (MAPI) is the model compound of the HyP class of materials that, in a few years, achieved, in photovoltaics, a power conversion efficiency of 25%. The attention on HyP has recently moved to large single crystals as emerging candidates for photovoltaic application because of their improved stability and optoelectronic properties compared to polycrystalline films. To control the quality and symmetry of the large MAPI single crystals, we proposed an original method that consisted of adding short-chain carboxylic acids to the inverse temperature crystallization (ICT) of MAPI in γ-butyrolactone (GBL). The crystals were characterized by single-crystal X-ray diffraction (SC-XRD), X-ray powder diffraction (XRPD) and Raman spectroscopy. Based on SC-XRD analysis, MAPI crystals grown using acetic and trifluoroacetic acids adopt a tetragonal symmetry “I4cm”. MAPI grown in the presence of formic acid turned out to crystallize in the orthorhombic “Fmmm” space group demonstrating the acid’s effect on the crystallization of MAPI.
Ferromagnetic quantum criticality in the quasi-one-dimensional heavy fermion metal YbNi4P2

We present a new Kondo-lattice system, YbNi4P2, which is a clean heavy-fermion metal with a severely reduced ferromagnetic (FM) ordering temperature at TC = 0.17 K, evidenced by distinct anomalies in susceptibility, specific heat and resistivity measurements. The FM nature of the transition, with only a small ordered moment of ∼0. 05μB, is established by a diverging susceptibility at TC with huge absolute values in the ferromagnetically ordered state, severely reduced by small magnetic fields. Furthermore, YbNi4P2 is a stoichiometric system with a quasi-one-dimensional crystal and electronic structure and strong correlation effects which dominate the low-temperature properties. This is reflected by a stronger-than-logarithmically diverging Sommerfeld coefficient and a linear-in-T resistivity above TC, which cannot be explained by current theoretical predictions. These exciting characteristics are unique among all correlated electron systems and make this an interesting material for further in-depth investigations.
Chemical gradients in the Milky Way from the RAVE data I. Dwarf stars

Aims. We aim at measuring the chemical gradients of the elements Mg, Al, Si, and Fe along the Galactic radius to provide new constraints on the chemical evolution models of the Galaxy and Galaxy models such as the Besancon model. Thanks to the large number of stars of our RAVE sample we can study how the gradients vary as function of the distance from the Galactic plane. Methods. We analysed three different samples selected from three independent datasets: a sample of 19 962 dwarf stars selected from the RAVE database, a sample of 10 616 dwarf stars selected from the Geneva-Copenhagen Survey (GCS) dataset, and a mock sample (equivalent to the RAVE sample) created by using the GALAXIA code, which is based on the Besancon model. The three samples were analysed by using the very same method for comparison purposes. We integrated the Galactic orbits and obtained the guiding radii (Rg) and the maximum distances from the Galactic plane reached by the stars along their orbits (Zmax). We measured the chemical gradients as functions of Rg at different Zmax. Results. We found that the chemical gradients of the RAVE and GCS samples are negative and show consistent trends, although they are not equal: at Zmax < 0.4 kpc and 4.5 < Rg(kpc) < 9.5, the iron gradient for the RAVE sample is d[Fe/H]/dRg = −0.065 dex kpc −1 , whereas for the GCS sample it is d[Fe/H]/dRg = −0.043 dex kpc −1 with internal errors of ±0.002 and ±0.004 dex kpc −1 , respectively. The gradients of the RAVE and GCS samples become flatter at larger Zmax. Conversely, the mock sample has a positive iron gradient of d[Fe/H]/dRg =+ 0.053 ± 0.003 dex kpc −1 at Zmax < 0.4 kpc and remains positive at any Zmax. These positive and unrealistic values originate from the lack of correlation between metallicity and tangential velocity in the Besancon model. In addition, the low metallicity and asymmetric drift of the thick disc causes a shift of the stars towards lower Rg and metallicity which, together with the thin-disc stars with a higher metallicity and Rg, generates a fictitious positive gradient of the full sample. The flatter gradient at larger Zmax found in the RAVE and the GCS samples may therefore be due to the superposition of thin- and thick-disc stars, which mimicks a flatter or positive gradient. This does not exclude the possibility that the thick disc has no chemical gradient. The discrepancies between the observational samples and the mock sample can be reduced by i) decreasing the density; ii) decreasing the vertical velocity; and iii) increasing the metallicity of the thick disc in the Besancon model.
Scaling of oscillation frequencies in rotating stars

Abstract We have studied oscillation frequencies of two-dimensional uniformly rotating zero-age main sequence stellar models in the delta Scuti mass range. We identified 370 p and g axisymmetric modes for non-rotating models and then traced their evolution as the rotational velocity was increased. For each mass we considered a rotation sequence of ten models, with the largest rotation rate being about 200 km s−1. We constrained the models to have the same surface shape, which can be characterized for uniform rotation by the ratio between the polar and the equatorial radii. We find that scaling relationships exist among the oscillation frequencies calculated for models with the same shape. For p modes, this scaling closely follows the period root-mean-density relation found in spherical stars. The g modes also scale between models of the same shape, with the scaling reflecting the change in properties outside the convective core as the stellar mass increases. These scaling relationships can be particularly useful in finding specific stellar models to match the oscillation frequencies of individual stars.
Anticancer effects and mechanisms of astragaloside-IV

Astragalus membranaceus Bunge is widely used in Traditional Chinese Medicine to treat various cancers. Astragaloside-IV (AS-IV) is one of the major compounds isolated from A. membranaceus Bunge and has been demonstrated to have antitumor effects by inhibiting cell proliferation, invasion and metastasis in various cancer types. Numerous studies have used in vitro cell culture and in vivo animal models of cancer to explore the antitumor activities of AS-IV. In the present study, the antitumor effects and mechanisms of AS-IV reported in studies recorded in the PubMed database were reviewed. First, the antitumor effects of AS-IV on proliferation, cell cycle, apoptosis, autophagy, invasion, migration, metastasis and epithelial-mesenchymal transition processes in cancer cells and the tumor microenvironment, including angiogenesis, tumor immunity and macrophage-related immune responses to cancer cells, were comprehensively discussed. Subsequently, the molecular mechanisms and related signaling pathways associated with antitumor effects of AS-IV as indicated by in vitro and in vivo studies were summarized, including the Wnt/AKT/GSK-3β (glycogen synthase kinase-3β)/β-catenin, TGF-β/PI3K/AKT/mTOR, PI3K/MAPK/mTOR, PI3K/AKT/NF-κB, Rac family small GTPase 1/RAS/MAPK/ERK, TNF-α/protein kinase C/ERK1/2-NF-κB and Tregs (T-regulatory cells)/IL-11/STAT3 signaling pathways. Of note, several novel mechanisms of Toll-like receptor 4 (TLR4)/NF-κB/STAT3, pSmad3C/3L, nuclear factor erythroid 2-related factor (NrF2)/heme oxygenase 1, circDLST/microRNA-489-3p/eukaryotic translation initiation factor 4A1 and macrophage-related high-mobility group box 1-TLR4 signaling pathways associated with the anticancer activity of AS-IV were also included. Finally, the limitations of current studies that must be addressed in future studies were pointed out to facilitate the establishment of AS-IV as a potent therapeutic drug in cancer treatment.
Very metal-poor galaxies: ionized gas kinematics in nine objects

The study of ionized gas morphology and kinematics in nine extremely metal-deficient (XMD) galaxies with the scanning Fabry-Perot interferometer on the Special Astrophysical Observatory (SAO) 6-m telescope is presented. Some of these very rare objects (with currently known range of O/H of 7.12 < 12 + log(O/H) < 7.65, or Z/35 < Z < Z/10) are believed to be the best proxies of 'young' low-mass galaxies in the high-redshift Universe. One of the main goals of this study is to look for possible evidence of star formation (SF) activity induced by external perturbations. Recent results from H I mapping of a small subsample of XMD star-forming galaxies provided confident evidence for the important role of interaction-induced SF. Our observations provide complementary or new information that the great majority of the studied XMD dwarfs have strongly disturbed gas morphology and kinematics or the presence of detached components. We approximate the observed velocity fields by simple models of a rotating tilted thin disc, which allows us the robust detection of non-circular gas motions. These data, in turn, indicate the important role of current/recent interactions and mergers in the observed enhanced SF. As a by-product of our observations, we obtained data for two Low Surface Brightness (LSB) dwarf galaxies: Anon J012544+075957 that is a companion of the merger system UGC 993, and SAO 0822+3545 which shows off-centre, asymmetric, low star formation rate star-forming regions, likely induced by the interaction with the companion XMD dwarf HS 0822 + 3542.
Planetary Formation and Evolution Revealed with a Saturn Entry Probe: The Importance of Noble Gases

The determination of Saturn's atmospheric noble gas abundances are critical to understanding the formation and evolution of Saturn, and giant planets in general. These measurements can only be performed with an entry probe. A Saturn probe will address whether enhancement in heavy noble gases, as was found in Jupiter, are a general feature of giant planets, and their ratios will be a powerful constraint on how they form. The helium abundance will show the extent to which helium has phase separated from hydrogen in the planet's deep interior. Jupiter's striking neon depletion may also be tied to its helium depletion, and must be confirmed or refuted in Saturn. Together with Jupiter's measured atmospheric helium abundance, a consistent evolutionary theory for both planets, including "helium rain" will be possible. We will then be able to calibrate the theory of the evolution of all giant planets, including exoplanets. In addition, high pressure H/He mixtures under giant planet conditions are an important area of condensed matter physics that are beyond the realm of experiment.
Effects of Diet and Lifestyle on Audio-Vestibular Dysfunction in the Elderly: A Literature Review

Background: The world’s age-related health concerns continue to rise. Audio-vestibular disorders, such as hearing loss, tinnitus, and vertigo, are common complaints in the elderly and are associated with social and public health burdens. Various preventative measures can ease their impact, including healthy food consumption, nutritional supplementation, and lifestyle modification. We aim to provide a comprehensive summary of current possible strategies for preventing the age-related audio-vestibular dysfunction. Methods: A PubMed, Embase, and Cochrane review databases search was conducted to identify the relationship between diet, lifestyle, and audio-vestibular dysfunction. “Diet”, “nutritional supplement”, “lifestyle”, “exercise”, “physical activity”, “tinnitus”, “vertigo” and “age-related hearing loss” were used as keywords. Results: Audio-vestibular dysfunction develops and progresses as a result of age-related inflammation and oxidative stress. Diets with anti-inflammatory and antioxidant effects have been proposed to alleviate this illness. A high-fat diet may induce oxidative stress and low protein intake is associated with hearing discomfort in the elderly. Increased carbohydrate and sugar intake positively correlate with the incidence of audio-vestibular dysfunction, whereas a Mediterranean-style diet can protect against the disease. Antioxidants in the form of vitamins A, C, and E; physical activity; good sleep quality; smoking cessation; moderate alcohol consumption; and avoiding noise exposure are also beneficial. Conclusions: Adequate diet or nutritional interventions with lifestyle modification may protect against developing audio-vestibular dysfunction in elderly individuals.
Magnetar powered GRBs: explaining the extended emission and X-ray plateau of short GRB light curves

Extended emission (EE) is a high-energy, early time rebrightening sometimes seen in the light curves of short gamma-ray bursts (GRBs). We present the first contiguous fits to the EE tail and the later X-ray plateau, unified within a single model. Our central engine is a magnetar surrounded by a fall-back accretion disc, formed by either the merger of two compact objects or the accretion-induced collapse of a white dwarf. During the EE phase, material is accelerated to super-Keplarian velocities and ejected from the system by the rapidly rotating (P � 1 10 ms) and very strong (10 15 G) magnetic field in a process known as magnetic propellering. The X-ray plateau is modelled as magnetic dipole spin-down emission. We first explore the range of GRB phenomena that the propeller could potentially reproduce, using a series of template light curves to devise a classification scheme based on phenomology. We then obtain fits to the light curves of 9 GRBs with EE, simultaneously fitting both the propeller and the magnetic dipole spin-down and finding typical disc masses of a few 10 −3 M⊙ to a few 10 −2 M⊙. This is done for ballistic, viscous disc and exponential accretion rates. We find that the conversion efficiency from kinetic energy toEM emission for propellered material needs to be & 10% and that the best fitting results come from an exponential accretion profile.
New white dwarfs in the Hyades Results from kinematic and photometric studies

Aims. On the basis of the PPMXL catalogue (Roser et al. 2010, AJ, 139, 2440) we searched for white dwarfs that are also member candidates of the Hyades in a region up to 40 pc from the cluster centre. Methods. We used the proper motions from PPMXL in the convergent point method to determine probable kinematic members. We cross-matched the kinematic candidates with catalogues containing white dwarfs and, finally, checked the kinematic with the photometric distances for consistency. Results. We found the 10 classical white dwarfs in the Hyades and determined their individual kinematic distances. Additionally, we identified 17 new probable (former) Hyades white dwarfs, i.e. white dwarfs co-moving with the bulk space motion of the Hyades cluster. At present, none of them can be excluded from membership on the basis of the measured radial velocities. For another 10 objects, the kinematic and the photometric distances disagree, which rates them as probable non-members. Among the probable members, five white dwarfs are in binary systems, three are known, two are new. There is good indication for an empirical magnitudedistance (from centre) relation, such that the dimmer white dwarfs are farther away from the cluster centre than the brighter ones. Our sample becomes incomplete close behind the centre of the cluster. Follow-up observations are encouraged to independently confirm the predicted radial velocities and the distances of the candidates.
Non-Markovian dynamics in two-qubit dephasing channels with an application to superdense coding

We study the performance of two measures of non-Markovianity in detecting memory effects in two-qubit dephasing channels. By combining independent Markovian and non-Markovian noise on the qubits, our results show that the trace distance measure is able to detect the memory effects when at least one of the local channels displays non-Markovianity. A measure based on channel capacity, in turn, becomes non-zero when the global two-qubit dynamics shows memory effects. We apply these schemes to a well-known superdense coding protocol and demonstrate an optimal noise configuration to maximize the information transmission with independent local noises.
Do boys and girls write the same? Analysis of n-grams of morphological categories (¿Niños y niñas escriben igual? Análisis de n-gramas de categorías morfológicas)

ABSTRACT The objective of this study is to characterize writing samples in Catalan written by boys and girls in primary school (from seven to 12 years old) using syntactic patterns. The corpus contains 169 writings divided by sex (76 boys and 93 girls) with an average of 200 words and a total length of 33,763 words. From this corpus, we calculated the 40 n-grams of the most frequent morphological categories (bigrams, trigrams). The data were statistically analysed using ANOVA and Linear Discriminant Analysis, and the accuracy in predicting the writer’s gender in a cross-validation experiment was 60.4% using both bigrams and trigrams. When the children’s age was taken into account, the percentage of accuracy was higher than 70% in both the original classification and the cross-validation. The identification of the most discriminating bigrams and trigrams allowed us to determine that girls show a greater expressive capacity and superior syntactic maturity, and greater lexical and syntactic richness.