Miracle-dz/UniFAR-FTUs huggingface dataset:
A Spectroscopic Survey of a Sample of Active M Dwarfs

A moderate-resolution spectroscopic survey of Fleming's sample of 54 X-ray–selected M dwarfs with photometric distances less than 25 pc is presented. All the objects consist of one or two dMe stars, some being doubles or spectroscopic binaries. Radial and rotation velocities have been measured by fits to the Hα profiles. Radial velocities have been measured by cross correlation. Artificial broadening of an observed spectrum has produced a relationship between Hα FWHM and rotation speed, which we use to infer rotation speeds for the entire sample by measurement of the Hα emission line. We find three ultrafast rotators (UFRs, v sin i ≥ 100 km s-1) and eight stars with 30 km s-1 ≤ v sin i < 100 km s-1. We find that the UFRs have quite variable emission and should be observed for photometric variability. Cross-correlation velocities measured for UFRs are shown to depend on rotation speed and the filtering used. The radial velocity dispersion of the sample is 17 km s-1. A new double emission line spectroscopic binary with a period of 3.55 days has been discovered, RX J1547.4+4507, and another known one is in the sample, the Hyades member RX J0442.5+2027. Three other objects are suspected spectroscopic binaries, and at least six are visual doubles. The only star in the sample observed to have significant lithium happens to be a known TW Hya association member, TWA 8A. These results all show that there are a number of young (<108 yr) and very young (<107 yr) low-mass stars in the immediate solar neighborhood. The Hα activity strength does not depend on rotation speed. Our fast rotators are less luminous than similarly fast rotators in the Pleiades. They are either younger than the Pleiades or gained angular momentum in a different way.
Long-Term Datasets for the Understanding of Solar and Stellar Magnetic Cycles

The properties of the acoustic modes are sensitive to magnetic activity. The unprecedented long-term Kepler photometry, thus, allows stellar magnetic cycles to be studied through asteroseismology. We search for signatures of magnetic cycles in the seismic data of Kepler solar-type stars. We find evidence for periodic variations in the acoustic properties of about half of the 87 analysed stars. In these proceedings, we highlight the results obtained for two such stars, namely KIC 8006161 and KIC 5184732.
Regional visa-waiver program for open tourism development

ABSTRACT Tourism development is known to have an important impact on the economic growth and the competitiveness of the region. For tourism development, the Jeju local government introduced a visa-waiver program that is valid only for the Jeju region. In addition, the regional visa-waiver program was possible in Korea, which has a stronger centralized system, because of strong cooperation in tourism from the central government. To our knowledge, few countries have introduced a visa policy at regional level like Jeju. Therefore, it is important to study the relationship between this unique regional visa policy and tourism development from the open tourism perspective. Meanwhile, citizens of countries that do not have a visa agreement with Korea must have a direct flight from the departure point to Jeju to benefit from this program. To alleviate this problem, domestic airports where inbound travelers whose final destinations is Jeju can transit without a Korean visa having been designated. The purpose of this study is to examine the effects of these programs on inbound tourism demand. For this, a Difference-In-Differences estimator has been used. From the results, both programs were found to have a statistically significant effect on the increase of inbound tourism in Jeju.
Early evolution of newly born proto-neutron stars

A proto-neutron star (PNS) is the first phase of life of a neutron star, and is likely to origin from a core-collapse supernova. After about 200 ms from core-collapse, the PNS evolution may be modeled as a sequence of quasi-stationary configurations. These configurations depend on the PNS thermodynamic profiles, whose evolution largely depends upon the neutrino diffusion. We developed a new PNS evolutionary code that solves by iteration the neutrino number and energy transport equations together with the relativistic stellar structure equations assuming spherical symmetry. The neutrino cross sections are determined consistently with the underlying equation of state (EoS). To include the EoSs in the evolution, we devised and tested a new fitting formula for the interacting part of the baryon free-energy, valid at finite temperature and arbitrary degeneracy. Using our code, we provide estimates for the neutrino signal in the Super-Kamiokande III detector and the frequencies of the gravitational waves due to stellar oscillations, for three stellar masses and three nucleonic EoSs. For the first time we evolve a PNS with a nuclear many-body theory EoS in a consistent way, that is, we take into account realistic nuclear interactions in the computation of the neutrino cross sections. By including rotation in an effective way, we have also determined the time variation of the rotation frequency due to PNS contraction and neutrino angular momentum loss, and the gravitational wave signal due to rotation. We find that the mass shedding limit restricts the initial angular momentum. Consequently, the final rotation frequency has to be smaller than about 300 Hz for a PNS of about 1.6 solar masses whose EoS is described by the GM3 mean-field model.
EXPLORING THE UNUSUALLY HIGH BLACK-HOLE-TO-BULGE MASS RATIOS IN NGC 4342 AND NGC 4291: THE ASYNCHRONOUS GROWTH OF BULGES AND BLACK HOLES

We study two nearby early-type galaxies, NGC 4342 and NGC 4291, that host unusually massive black holes relative to their low stellar mass. The observed black-hole-to-bulge mass ratios of NGC 4342 and NGC 4291 are 6.9+3.8 − 2.3% and 1.9% ± 0.6%, respectively, which significantly exceed the typical observed ratio of ∼0.2%. As a consequence of the exceedingly large black-hole-to-bulge mass ratios, NGC 4342 and NGC 4291 are ≈5. 1σ and ≈3. 4σ outliers from the M•–Mbulge scaling relation, respectively. In this paper, we explore the origin of the unusually high black-hole-to-bulge mass ratio. Based on Chandra X-ray observations of the hot gas content of NGC 4342 and NGC 4291, we compute gravitating mass profiles, and conclude that both galaxies reside in massive dark matter halos, which extend well beyond the stellar light. The presence of dark matter halos around NGC 4342 and NGC 4291 and a deep optical image of the environment of NGC 4342 indicate that tidal stripping, in which ≳ 90% of the stellar mass was lost, cannot explain the observed high black-hole-to-bulge mass ratios. Therefore, we conclude that these galaxies formed with low stellar masses, implying that the bulge and black hole did not grow in tandem. We also find that the black hole mass correlates well with the properties of the dark matter halo, suggesting that dark matter halos may play a major role in regulating the growth of the supermassive black holes.
The connection between globular cluster systems and the host galaxies

ABSTRA C T A large number of early-type galaxies are now known to possess blue and red subpopulations of globular clusters. We have compiled a data base of 28 such galaxies exhibiting bimodal globular cluster colour distributions. After converting to a common V‐I colour system, we investigate correlations between the mean colour of the blue and red subpopulations with galaxy velocity dispersion. We support previous claims that the mean colours of the blue globular clusters are unrelated to their host galaxy. They must have formed rather independently of the galaxy potential they now inhabit. The mean blue colour is similar to that for halo globular clusters in our Galaxy and M31. The red globular clusters, on the other hand, reveal a strong correlation with galaxy velocity dispersion. Furthermore, in well-studied galaxies the red subpopulation has similar, and possibly identical, colours to the galaxy halo stars. Our results indicate an intimate link between the red globular clusters and the host galaxy; they share a common formation history. A natural explanation for these trends would be the formation of the red globular clusters during galaxy collapse.
How Urinary Incontinence Affects Sexual Activity in Polish Women: Results from a Cross-Sectional Study

Urinary incontinence (UI) in women can cause a number of sexual dysfunctions and reduce their quality of life. Sexual health is essential to the self-esteem, emotional state, and overall quality of life. We aimed to assess the quality of sexual life of women with UI. The study included a group of 145 sexually active women diagnosed with UI. The research was conducted using the diagnostic survey method with authorial and validated questionnaires. As many as 49.1% of the respondents reported a deterioration of sexual relations in comparison with the time before the onset of UI symptoms. According to the FSDS-R results, 83.45% of respondents were dissatisfied with their sex life. The higher the result obtained by respondents in the FSDS-R scale, the lower was their quality of life in the IIQ-7 scale (p ≤ 0.002, R = 0.53). The greatest impact was observed in the domains of emotional health and physical activity. The more incontinence symptoms reported by the respondent in the UDI-6 scale, the worse was her sexual satisfaction in the FSDS-R (p = 0.003, R = 0.39). UI in women contributes to the development of sexual dysfunctions, including decreased interest in sexual life, limited intercourse, and dissatisfaction with sexual life.
Plant Waste as Green Reinforcement for Polymer Composites: A Case Study of Pteris Vittata Roots

ABSTRACT Pteris vittata is a hyperaccumulator fern able to uptake arsenic by roots accumulating it in the fronds. Recent studies showed that Pteris vittata can be used efficiently for arsenic-contaminated water treatment, paving the way for long-lasting decontamination strategies established on nature-based solutions. This raises the issue of biomass disposal, which rather than being incinerated could represent a valuable untapped source of fibers for sustainable and higher-value biocomposites. Here, Pteris vittata waste roots were collected and used to develop composites based on high-density polyethylene. Composites with two amounts of filler (10 wt.% and 20 wt.%) added with 5 wt. % of maleic anhydride grafted polyethylene, were manufactured and tested in terms of mechanical and thermal properties. Mechanical property analysis showed that, compared to neat high-density polyethylene, composites at 20 wt. % filler content with coupling agent displayed an increase around 54% in tensile strength, 100% in Young’s modulus, 46% in flexural strength and 45% in flexural modulus. These results demonstrate the potential of Pteris vittata waste roots application for sustainable composite materials production.
Ultraefficient Internal Shocks

Gamma-ray bursts are believed to originate from internal shocks that arise in an irregular relativistic wind. The process has been thought to be inefficient, converting only a few percent of the kinetic energy into gamma rays. We define ultraefficient internal shocks as those in which the fraction of emitted energy is larger than the fraction of energy given to the radiating electrons at each collision. We show that such a scenario is possible and even plausible. In our model, colliding shells that do not emit all their internal energy are reflected from each other, causing subsequent collisions and thereby allowing more energy to be emitted. As an example, we obtain about 60% overall efficiency even if the fraction of energy that goes to electrons is ϵe = 0.1, provided that the shells' Lorentz factor varies between 10 and 104. The numerical temporal profile reflects well the activity of the source that ejects the shells, though numerous collisions take place in this model.
Regularization ambiguities in loop quantum gravity

One of the main achievements of loop quantum gravity is the consistent quantization of the analog of the Wheeler-DeWitt equation which is free of ultraviolet divergences. However, ambiguities associated to the intermediate regularization procedure lead to an apparently infinite set of possible theories. The absence of an UV problem--the existence of well-behaved regularization of the constraints--is intimately linked with the ambiguities arising in the quantum theory. Among these ambiguities is the one associated to the SU(2) unitary representation used in the diffeomorphism covariant 'point-splitting' regularization of the nonlinear functionals of the connection. This ambiguity is labeled by a half-integer m and, here, it is referred to as the m ambiguity. The aim of this paper is to investigate the important implications of this ambiguity. We first study 2+1 gravity (and more generally BF theory) quantized in the canonical formulation of loop quantum gravity. Only when the regularization of the quantum constraints is performed in terms of the fundamental representation of the gauge group does one obtain the usual topological quantum field theory as a result. In all other cases unphysical local degrees of freedom arise at the level of the regulated theory that conspire against the existence of the continuummore » limit. This shows that there is a clear-cut choice in the quantization of the constraints in 2+1 loop quantum gravity. We then analyze the effects of the ambiguity in 3+1 gravity exhibiting the existence of spurious solutions for higher representation quantizations of the Hamiltonian constraint. Although the analysis is not complete in 3+1 dimensions - due to the difficulties associated to the definition of the physical inner product - it provides evidence supporting the definitions quantum dynamics of loop quantum gravity in terms of the fundamental representation of the gauge group as the only consistent possibilities. If the gauge group is SO(3) we find physical solutions associated to spin-two local excitations. « less
Molecular epidemiology of carbapenem-resistant Acinetobacter baumannii isolates in Turkiye: Systematic review

The World Health Organization has designated carbapenem-resistant Acinetobacter baumannii (CRAB) as a “critical” pathogen on the global priority list of antibiotic-resistant bacteria. This study aims to discuss the molecular epidemiology of CRAB isolates in Turkiye in the last 12 years and the prevalence of gene regions associated with resistance or pathogenesis using a systematic review method. Our study consists of a literature search, determination of eligibility and exclusion criteria, qualitative analysis of studies, data extraction, and statistical analysis. All studies were analyzed according to the Preferred Reporting Items for Systematic Reviews and Meta-Analysis Guidelines. The incidence rates of blaOXA-23, blaOXA-23-like, blaOXA-24/40, blaOXA-24/40-like, blaOXA-51, blaOXA-51-like, blaOXA-58, and blaOXA-58-like genes in CRAB strains were 76.4%, 68.6%, 1.2%, 3.4%, 97.0%, 98.6%, 8.4%, and 17.1%, respectively. It was determined that the prevalence of the blaOXA-23 and blaOXA-58 gene regions showed a statistically significant change over the years. Due to the high prevalence of A. baumannii strains carrying the blaOXA-23 variant, it is necessary to follow its geographical distribution and transposon and plasmid movements. Based on available data, molecular surveillance of CRAB strains should be standardized. In addition, sterilization and disinfection processes applied within the scope of an effective struggle against CRAB strains that can remain live on surfaces for a long time should be reviewed frequently.
On redundancy, dilations and canonical duals of $g$-frames in Hilbert spaces

In Hilbert spaces, the redundancy property of g -frames is diﬀerent from that of frames, and the dilation theory is interesting and important in many mathematical ﬁelds. In this paper, we study the redundancy and dilations of g -frames in Hilbert spaces. First, we characterize g -Riesz bases and exact g -frames under some constraints, then obtain some dilation results for (normalized tight) g -frames, and give some properties about them. Finally we prove some interesting properties on the canonical duals of g -frames.
Testing the Evolutionary Link between Type 1 and Type 2 Quasars with Measurements of the Interstellar Medium

In a popular scenario for the coevolution of massive black holes and galaxies, major mergers of gas-rich galaxies fuel vigorous star formation and obscured (type 2) quasar activity until energy feedback from the active galactic nucleus (AGN) clears away the gas and dust to reveal an unobscured (type 1) quasar. Under this scenario, the precursor type 2 quasars should be more gas-rich than their type 1 counterparts, and both types of quasars are expected to be gas-deficient relative to normal, star-forming galaxies of similar stellar mass. We test this evolutionary hypothesis by investigating the infrared (∼1–500 μm) spectral energy distribution of 86 optically selected z < 0.5 type 2 quasars, matched in redshift and [O iii] luminosity to a comparison sample of type 1 quasars. Contrary to expectations, the gas content of the host galaxies of type 2 quasars is nearly indistinguishable from that of type 1 quasar hosts, and neither type exhibits the predicted deficit in gas relative to normal galaxies. The gas mass fraction of quasar hosts appears unaffected by the bolometric luminosity of the active nucleus, although their interstellar radiation field is preferentially higher than that of normal galaxies, potentially implicating AGN heating of the large-scale galactic dust.
Black hole spin from wobbling and rotation of the M87 jet and a sign of a magnetically arrested disc

New long-term Very Long Baseline Array observations of the well-known jet in the M87 radio galaxy at 43 GHz show that the jet experiences a sideways shift with an approximately 8-10 yr quasi-periodicity. Such jet wobbling can be indicative of a relativistic Lense-Thirring precession resulting from a tilted accretion disc. The wobbling period together with up-to-date kinematic data on jet rotation opens up the possibility for estimating angular momentum of the central supermassive black hole. In the case of a test-particle precession, the specific angular momentum is $J/Mc=(2.7\pm1.5)\times10^{14}$ cm, implying moderate dimensionless spin parameters $a=0.5\pm0.3$ and $0.31\pm0.17$ for controversial gas-dynamic and stellar-dynamic black hole masses. However, in the case of a solid-body-like precession, the spin parameter is much smaller for both masses, $0.15\pm0.05$. Rejecting this value on the basis of other independent spin estimations requires the existence of a magnetically arrested disc in M87.
Emotional Temperament and Character Dimensions and State Anger as Predictors of Preference for Rap Music in Italian Population

The objective of the current work was to examine the relationships between affective temperaments dimensions, trait anger, and the preference for rap music in a sample of Italian adults. An online survey was administered to 662 subjects. We assessed preference for rap music using a Likert scale. Ina addition, we investigated the sample’ affective temperament traits using the Memphis, Pisa, Paris, and San Diego (TEMPS-A) short scale and the trait anger by using the Trait Anger component of the State Trait Anger Expression Inventory 2 (STAXI-2). Multiple linear regression indicated that cyclothymic temperament score, hyperthymic temperament score, and trait anger scores were positive predictors while older age, and depressive temperament and higher education score were negative predictors of preference for rap music. The results expand previous literature on personality and music preference indicating the association of high energy/high activity temperaments and trait anger to preference for rap music.
Consistent hydrodynamic theory of chiral electrons in Weyl semimetals

The complete set of the Maxwell's and hydrodynamic equations for the chiral electrons in Weyl semimetals is presented. The formulation of the Euler equation takes into account the explicit breaking of the Galilean invariance by the ion lattice. The Chern-Simons (or Bardeen-Zumino) contributions to the electric current and charge densities are also included and their role in the hydrodynamic regime is discussed. These topological contributions play a crucial role in the Maxwell's equations by providing the information on the separation of Weyl nodes in energy and momentum. On the other hand, they do not directly affect the Euler equation and the energy conservation relation for the electron fluid. By making use of the proposed consistent hydrodynamic framework, we show that the topological effects can strongly modify the dispersion relations of collective modes in Weyl semimetals. This is reflected, in particular, in the existence of distinctive anomalous Hall waves which are sustained by the local anomalous Hall currents.
Accurate pre- and post-eruption orbital periods for the dwarf/classical nova V1017 Sgr

V1017 Sgr is a classical nova (in 1919) that displayed an earlier dwarf nova eruption (in 1901), and two more dwarf nova events (in 1973 and 1991). Previous work on this bright system in quiescence (V=13.5) has only been a few isolated magnitudes, a few spectra, and an ambiguous claim for an orbital period of 5.714 days as based on nine radial velocities. To test this period, we have collected 2896 magnitudes (plus 53 in the literature) in the UBVRIJHKL bands from 1897 to 2016, making an essentially complete photometric history of this unique cataclysmic variable. We find that the light curve in all bands is dominated by the ellipsoidal modulations of a G giant companion star, with a post-eruption (after the 1919 nova event) orbital period of 5.786290 +- 0.000032 days. This is the longest period for any classical nova, the accretion must be powered by the nuclear evolution of the companion star, and the dwarf nova events occur only because the outer parts of the large disk are cool enough to be unstable. Furthermore, we measure the pre-eruption orbital period (from 1907 to 1916), and there is a small steady period change in quiescence. The orbital period has decreased by 273 +- 61 parts-per-million across the 1919 eruption, with the significance of the period change being at the 5.7-sigma confidence level. This is startling and mystifying for nova-theory, because the three known period change effects cannot account for a period decrease in V1017 Sgr, much less one of such a large size.
Feasibility of the debris ring transit method for the solar-like star HD 107146 by an occulted galaxy

Occulting galaxy pairs have been used to determine the transmission and dust composition within the foreground galaxy. Observations of the nearly face-on ring-like debris disk around the solar-like star HD 107146 by HST/ACS in 2004 and HST/STIS in 2011 reveal that the debris ring is occulting an extended background galaxy over the subsequent decades. Our aim is to use 2004 HST observations of this system to model the galaxy and apply this to the 2011 observation in order to measure the transmission of the galaxy through the outer regions of the debris disk. We model the galaxy with an exponential disk and a S\'{e}rsic pseudo-bulge in the V- and I-band, but irregularities due to small scale structure from star forming regions limits accurate determination of the foreground dust distribution. We show that debris ring transit photometry is feasible for optical depth increases of $\Delta \tau \geq$ 0.04 ($1 \sigma$) on tens of au scales the width of the background galaxy { when the 2011 STIS data are compared directly with new HST/STIS observations, instead of the use of a smoothed model as a reference.