Miracle-dz/UniFAR-FTUs huggingface dataset:
FAR-ULTRAVIOLET OBSERVATIONS OF OUTFLOWS FROM INFRARED-LUMINOUS GALAXIES

We obtained medium-resolution ultraviolet (UV) spectra between 1150 and 1450 Å of the four UV-bright, infrared-luminous starburst galaxies IRAS F08339+6517, NGC 3256, NGC 6090, and NGC 7552 using the Cosmic Origins Spectrograph on board the Hubble Space Telescope. The selected sightlines toward the starburst nuclei probe the properties of the recently formed massive stars and the physical conditions in the starburst-driven galactic superwinds. Despite being metal-rich and dusty, all four galaxies are strong Lyα emitters with equivalent widths ranging between 2 and 13 Å. The UV spectra show strong P Cygni-type high-ionization features indicative of stellar winds and blueshifted low-ionization lines formed in the interstellar and circumgalactic medium. We detect outflowing gas with bulk velocities of ∼400 km s−1 and maximum velocities of almost 900 km s−1. These are among the highest values found in the local universe and comparable to outflow velocities found in luminous Lyman-break galaxies at intermediate and high redshift. The outflow velocities are unlikely to be high enough to cause escape of material from the galactic gravitational potential. However, the winds are significant for the evolution of the galaxies by transporting heavy elements from the starburst nuclei and enriching the galaxy halos. The derived mass outflow rates of ∼100 M☉ yr−1 are comparable to or even higher than the star formation rates. The outflows can quench star formation and ultimately regulate the starburst as has been suggested for high-redshift galaxies.
The space density of magnetic cataclysmic variables

We use the complete, X-ray flux-limited ROSAT Bright Survey (RBS) to measure the space density (ρ) of magnetic cataclysmic variables (mCVs). The survey provides complete optical identification of all sources with count rate >0.2 s −1 (corresponding to FX 2 × 10 −12 erg cm −2 s −1 ) over half the sky (|b| > 30 ◦ ), and detected 6 intermediate polars (IPs) and 24 polars. If we assume that the 30 mCVs included in the RBS are representative of the intrinsic population, the space density of mCVs is 8 +4 −2 × 10 −7 pc −3 . Considering polars and IPs separately, we find ρpolar = 5 +3 −2 × 10 −7 pc −3 and ρIP = 3
Evaluation of “Bell Let’s Talk in the Classroom”: A Guide for Improving Teachers’ Confidence in Providing Mental Health Education

The Let’s Talk in the Classroom (LTIC) Guide was designed to provide teachers with the education and support required to feel confident delivering mental health-related material in the Grade 7/8 classroom. The overall goal of this preliminary evaluation was to explore the acceptability, feasibility, and utility of the Guide using a mixed methods approach. A matched, pre/post-test evaluation of the Guide was conducted during the 2017/2018 school year among a sample of educators in Ontario, Canada (n = 42). Quantitatively and qualitatively, results demonstrated that teachers felt more confident and expressed fewer worries associated with teaching mental health-related lessons after engaging with the Guide and were suggestive of acceptability and utility, with continued challenges associated with feasibility identified.
Circular motion in NUT space-time

We consider circular motion in the NUT (Newman–Unti–Tamburino) space-time. Among other things, we determine the location of circular time-like geodesic orbits, in particular of the innermost stable circular orbit (ISCO) and of the marginally bound circular orbit. Moreover, we discuss the von Zeipel cylinders with respect to the stationary observers and with respect to the zero angular momentum observers (ZAMOs). We also investigate the relation of von Zeipel cylinders to inertial forces, in particular in the ultra-relativistic limit. Finally, we generalise the construction of thick accretion tori (‘Polish doughnuts’) which are well known on the Schwarzschild or Kerr background to the case of the NUT metric. We argue that, in principle, an NUT source could be distinguished from a Schwarzschild or Kerr source by observing the features of circular matter flows in its neighbourhood.
Testing Lorentz invariance with the ultrahigh energy cosmic ray spectrum

The Greisen-Zatsepin-Kuzmin cutoff predicted at the ultrahigh energy cosmic ray spectrum has been observed by the HiRes and Auger experiments. The results put severe constraints on the effect of Lorentz invariance violation (LIV), which has been introduced to explain the absence of the Greisen-Zatsepin-Kuzmin cutoff indicated in the AGASA data. Assuming a homogeneous source distribution with a single power-law spectrum, we calculate the ultrahigh energy cosmic ray spectrum observed on the Earth by taking photopion production, e(+)e(-) pair production, and the adiabatic energy loss into account. The effect of LIV is also taken into account in the calculation. By fitting the HiRes monocular spectra and the Auger combined spectra, we show that the LIV parameter is constrained to xi=-0.8(-0.5)(+3.2)x10(-23) and 0.0(-0.4)(+1.0)x10(-23), respectively, which is very consistent with strict Lorentz invariance up to the highest energy.
Mucin1 expression and gustatory function in postmenopausal females: A case-control observational study

Background Investigating possible relationship between Mucin1 expression levels in saliva, gustatory function, and taste perception in postmenopausal females. Material and Methods Using whole mouth taste test, twenty-five post-menopausal females (51.35 ± 5.22 years) and twenty-five premenopausal females (39.65 ± 6.46 years) were prospectively evaluated for gustatory function. The expression of mucin1 was investigated; RNA was isolated from stimulated whole saliva samples and real-time PCR was used to determine mucin1 mRNA levels relative to bactin and GAPDH mRNA levels. Results Significant difference was observed between postmenopausal and premenopausal women regarding intensity judgments of all tastants. The difference was more evident for sucrose taste perception (p<0.00001). Mucin1 expression levels were significantly decreased in postmenopausal females compared with premenopausal ones (p<0.00001). Mucin1 expression level had significant negative correlation with the salt taste sensitivity but did not correlate significantly with intensity judgments of the other tastants. Conclusions Postmenopausal women have a reduced gustatory function, especially sucrose. Mucin1 expression was significantly decreased in postmenopausal females and had a significant negative correlation with the salt taste sensitivity. However, no correlation was found between mucin1 expression level and taste sensitivity of other tastants. Key words:Gustatory function, MUC1, taste, postmenopausal.
Self-employment, income, and poor with disabilities: the 2016 inclusion of people with disabilities act in Brazil

ABSTRACT We exploit the implementation of the Inclusion of People with Disabilities Act in Brazil in early 2016 and use stigma theory to focus on the poor with disabilities, a double-stigmatized group, in a developing country setting. We hypothesize after the passage of the law, the poor with disabilities will pursue more self-employment than employment, but their income will remain low, with only the income of the employed improving. Contrary to expectations, the results show that the odds of self-employment were not higher than employment after the law. But as predicted, only the income of the employed improved, with the income gap between the employed and self-employed with disabilities growing wider after the passage of the law. The findings demonstrate that the law mainly benefitted the poor with disabilities who were able to gain employment but not the self-employed.
Enhancement of Antibacterial Efficiency of Face Masks Using Metal Nanoparticles

In this study, the antibacterial activity of commercial face masks made from polypropylene against gram-negative and positive bacteria was enhanced by dipping in gold nanoparticle (Au NPs) prepared in water using simple chemical precipitation route. The XRD for mask sample shows the typical diffraction lines of polypropylene for untreated mask, compared to samples soaked in the Au NPs suspensions at different concentrations which showed small peaks of gold structure. These diffraction peaks increased in intensity with the concentration of Au NPs in the samples. The strain-stress study shows slightly increasing the sample strength with increasing the Au NPs concentration, while the maximum strain reduced. The antibacterial efficiency of mask soaked in the Au NPs displays a decent inhibition zone toward E. coli and S. aureus bacteria, of diameter about 2.4 cm, and 2 cm respectively. The variation in efficiency of killing comes from the different nature of the composition of these two species.
Isospin violation in $J/\Psi to \phi \pi^0 \eta$ decay and the $f_0 - a_0$ mixing

The isospin violating $J/\Psi\to \phi \pi^0 \eta$ decay is thought to be dominated by the mixing of the $f_0(980)$ and $a_0(980)$ scalar resonances. We make a theoretical evaluation of the $J/\Psi\to \phi \pi^0 \eta$ decay extending our own previous model for other $J/\Psi$ decays into one vector meson and two pseudoscalars using the techniques of the chiral unitary approach. The scalar resonances are dynamically generated through the final state interaction of the pseudoscalar mesons implementing unitarity from the lowest order ChPT amplitudes. Besides the direct $J/\Psi\phi PP$ vertex, other mechanisms like the sequential exchange of vector and axial-vector mesons are shown to be important in order to obtain the actual strength of the mixing. We get a very good agreement with the $\pi^0 \eta$ invariant mass distribution and branching ratio with recent BESIII data. Quantification of the $f_0(980)-a_0(980)$ mixing is done and compared with results from several experiments.
Lyman continuum leaking AGN in the SSA22 field

Subaru/SuprimeCam narrowband photometry of the SSA22 field reveals the presence of four Lyman continuum (LyC) candidates among a sample of 14 AGN. Two show offsets and likely have stellar LyC in nature or are foreground contaminants. The remaining two LyC candidates are Type I AGN. We argue that the average LyC escape fraction of high redshift low luminosity AGN is not likely to be unity, as often assumed in the literature. From direct measurement we obtain the average LyC-to-UV flux density ratio and ionizing emissivity for a number of AGN classes and find it at least a factor of two lower than values obtained assuming f_esc = 1. Comparing to recent Ly{\alpha} forest measurements, AGNs at redshift z~3 make up at most ~12% and as little as ~5% of the total ionizing budget. Our results suggest that AGNs are unlikely to dominate the ionization budget of the Universe at high redshifts.
Excessive functions, Appell polynomials and optimal stopping

The main topic of the thesis is optimal stopping. This is treated in two research articles. In the first article we introduce a new approach to optimal stopping of general strong Markov processes. The approach is based on the representation of excessive functions as expected suprema. We present a variety of examples, in particular, the Novikov-Shiryaev problem for Levy processes. In the second article on optimal stopping we focus on differentiability of excessive functions of diffusions and apply these results to study the validity of the principle of smooth fit. As an example we discuss optimal stopping of sticky Brownian motion. The third research article offers a survey like discussion on Appell polynomials. The crucial role of Appell polynomials in optimal stopping of Levy processes was noticed by Novikov and Shiryaev. They described the optimal rule in a large class of problems via these polynomials. We exploit the probabilistic approach to Appell polynomials and show that many classical results are obtained with ease in this framework. In the fourth article we derive a new relationship between the generalized Bernoulli polynomials and the generalized Euler polynomials.
CONSTRAINING THE RATE OF RELATIVISTIC JETS FROM TIDAL DISRUPTIONS USING RADIO SURVEYS

Tidal disruptions of stars by massive black holes produce transient accretion flows that flare at optical, UV, and X-ray wavelengths. At late times, these accretion flows may launch relativistic jets that can be detected through the interaction of the jet with the dense interstellar medium of the galaxy. We present an upper limit for the flux density of a radio counterpart to a tidal disruption event detected by GALEX that is a factor of six below theoretical predictions. We also examine existing radio surveys for transients with a timescale of 1 yr and use these to set a 2σ upper limit on the rate of tidal disruption events producing relativistic jets of ∼14 × 10−7 Mpc-3 yr−1. This rate is an order of magnitude lower than the highest values from theoretical models and is consistent with detection rates from optical and X-ray surveys.
Cloud Data System Design for Mental Crisis State Recognition of College Students Based on Machine Learning

At present, Chinese college students are facing a lot of psychological pressure; whether it is teaching pressure or life pressure, it will have a certain adverse impact on college students’ psychological state, and if timely guidance is not provided, it will result in some adverse consequences. Therefore, it is necessary to timely identify the psychological crisis situation of college students, but the existing form of manual identification has high limitations, which cannot obtain the psychological state of students more accurately and efficiently, so it is necessary to optimize and improve with the help of network technology. Cloud computing data system is one of the mature big data systems at present. The combination of cloud computing system and machine learning technology is effectively applied to the field of psychological crisis analysis, which can quickly screen the psychological status of college students and report abnormal data in a timely manner, so as to help college psychological teachers identify the state of college students’ psychological crisis and intervene in a timely manner to promote the physical and mental health of students. By applying machine learning technology for the establishment of a cloud computing data system and putting the system into the field of psychological crisis identification of Chinese college students, this study lays a theoretical and practical foundation for preventing students from the psychological crisis.
Constraining globular cluster formation through studies of young massive clusters - III. A lack of gas and dust in massive stellar clusters in the LMC and SMC

Scenarios that invoke multiple episodes of star formation within young globular clusters (GCs) to explain the observed chemical and photometric anomalies in GCs, require that clusters can retain the stellar ejecta of the stars within them and accrete large amounts of gas from their surroundings. Hence, it should be possible to find young massive clusters in the local Universe that contain significant amounts ($>10$\%) of the cluster mass of gas and/or dust within them. Recent theoretical studies have suggested that clusters in the Large Magellanic Cloud (LMC) with masses in excess of $10^4$\msun\, and ages between $30$ and $\sim300$~Myr, should contain such gas reservoirs. We have searched for \hi\ gas within 12 LMC (and 1 SMC) clusters and also for dust using {\em Spitzer} 70\micron\ and 160\micron\ images. No clusters were found to contain gas and/or dust. While two of the clusters have \hi\ at the same (projected) position and velocity, the gas does not appear to be centred on the clusters, but rather part of nearby clouds or filaments, suggesting that the gas and cluster are not directly related. This lack of gas ($<1$\% of the stellar mass) is in strong tension with model predictions, and may be due to higher stellar feedback than has been previously assumed or due to the assumptions used in the previous calculations.
Field O stars: formed in situ or as runaways?

A significant fraction of massive stars in the Milky Way and other galaxies are located far from star clusters and star-forming regions. It is known that some of these stars are runaways, i.e. possess high space velocities (determined through the proper motion and/or radial velocity measurements), and therefore most likely were formed in embedded clusters and then ejected into the field because of dynamical few-body interactions or binary-supernova explosions. However, there exists a group of field O stars whose runaway status is difficult to prove via direct proper motion measurements (e.g. in the Magellanic Clouds) or whose (measured) low space velocities and/or young ages appear to be incompatible with their large separation from known star clusters. The existence of this group led some authors to believe that field O stars can form in situ. Since the question of whether or not O stars can form in isolation is of crucial importance for star formation theory, it is important to thoroughly test candidates of such stars in order to improve the theory. In this paper, we examine the runaway status of the best candidates for isolated formation of massive stars in the Milky Way and the Magellanic Clouds by searching for bow shocks around them, by using the new reduction of the Hipparcos data, and by searching for stellar systems from which they could originate within their lifetimes. We show that most of the known O stars thought to have formed in isolation are instead very likely runaways. We show also that the field must contain a population of O stars whose low space velocities and/or young ages are in apparent contradiction to the large separation of these stars from their parent clusters and/or the ages of these clusters. These stars (the descendants of runaway massive binaries) cannot be traced back to their parent clusters and therefore can be mistakenly considered as having formed in situ. We argue also that some field O stars could be detected in optical wavelengths only because they are runaways, while their cousins residing in the deeply embedded parent clusters might still remain totally obscured. The main conclusion of our study is that there is no significant evidence whatsoever in support of the in situ proposal on the origin of massive stars.
The Syntax of Sentential Stress (2004)

This thesis explores the nature of sentential stress, how it is assigned and its interaction with information structure. The central thesis is that the position of sentential or nuclear stress, the element with the highest prominence in the sentence, is determined syntactically and that cross-linguistic differences in this respect follow from syntactic variations. In particular, it is proposed that the Sentential Stress Rule applies in a phase-based manner (Chomsky 2000, 2001 and subsequent work) and assigns stress to the highest element in the spelled out constituent. This proposal provides a systematic way of accounting for a wide range of cross-linguistic facts, with data taken from Persian, English, German, Eastern Armenian and some Romance languages. An additional rule, namely the Focus Stress Rule, is proposed to handle the interaction between sentential stress and information structure. The Focus Stress Rule, which is also proposed to apply in a phase-based manner, ensures that a focussed constituent receives the highest clausal prominence in languages which mark focus prosodically. It is shown that sentential stress is determined in an interplay between the default Sentential Stress Rule and the Focus Stress Rule. It is argued that the relationship between syntax and phonology is unidirectional, always from syntax to phonology, thereby arguing against syntactic phenomena being triggered by phonological or prosodic motivations (contra Zubizarreta 1998). It is also shown that, from a conceptual and empirical perspective, the proposed account of the interaction between focus and sentential stress is preferable to the theories based on the focus projection algorithm (Selkirk 1995).
Modified pulsar current analysis: probing magnetic field evolution

We use a modified pulsar current analysis to study magnetic fie ld decay in radio pulsars. In our approach we analyse the flow, not along the spin period axi s as has been performed in previous studies, but study the flow along the direction of gr owing characteristic age, τ = P/(2 u P). We perform extensive tests of the method and find that in most of the cases it is able to uncover non-negligible magnetic field decay (more th an a few tens of per cent during the studied range of ages) in normal radio pulsars for realis tic initial properties of neutron stars. However, precise determination of the magnetic field decay timescale is not possible at present. The estimated timescale may differ by a factor of few for different sets of initial distributions of neutron star parameters. In addition, som e combinations of initial distributions and/or selection effects can also mimic enhanced field decay . We apply our method to the observed sample of radio pulsars at distances < 10 kpc in the range of characteristic ages 8 × 10 4 < τ < 10 6 years where, according to our study, selection effects are minimized. By analysing pulsars in the Parkes Multibeam and Swinburne surveys we find that, in this range, the field decays roughly by a factor of two. With an expo nential fit this corresponds to the decay time scale � 4 × 10 5 yrs. With larger statistics and better knowledge of the init ial distribution of spin periods and magnetic field strength, th is method can be a powerful tool to probe magnetic field decay in neutron stars.
Non-Perturbative Yang-Mills Condensate as Dark Energy

Models based on Yang-Mills condensate (YMC) have been advocated in the literature and claimed to be successful candidates to explain dark energy. Several instantiations of this simple idea have been considered, the most promising of which are reviewed here. Nevertheless, results previously attained heavily relied on the perturbative approach to the analysis of the effective Yang-Mills action, which is only adequate in the asymptotically-free limit, and were extended into a regime, the infrared limit, in which confinement is expected. We show that if a minimum of the effective Lagrangian in θ=−F μν F /2 exists, a YMC forms that drives the Universe toward an accelerated de Sitter phase. The details of the models depend weakly on the specific form of the effective YangMills Lagrangian. Using non-perturbative techniques mutated from the functional renormalization group procedure, we finally show that the minimum in θ of the effective Lagrangian exists, thus YMC can actually take place. The non-perturbative model has properties similar to the ones of the perturbative model. In the early stage of the universe, the YMC equation of state has an evolution that resembles the radiation component, i.e. wy → 1/3. However, in the late stage, wy naturally runs to the critical state with wy = −1, and the universe transits from matter-dominated into dark energy dominated stage only recently, at a redshift the value of which depends on the initial conditions that are chosen while solving the dynamical system.