Miracle-dz/UniFAR-FTUs huggingface dataset:
Gender and Tobacco Consumption among University Students

In 2019, an estimated 155 million people aged between 15 and 24 were smokers. It is also known that 82.6% of current smokers started smoking between 14 and 25 years old. Tobacco uses in adolescents and young adults can lead to the development of serious and potentially life-threatening health problems. The aim of the present investigation is to identify and describe the practices related to the consumption of tobacco products and their distribution according to gender among students at the University of Algarve. This is an exploratory, cross-sectional study with a quantitative approach. For inferential statistics, a non-parametric analysis (χ2) was performed. The sample consisted of 326 university students, 75.5% female, with an average age of 26.03 years. In this sample, 45% of men and 57.7% of women reported never having smoked. In male students, the pattern of combined consumption is more frequent, with female students preferring conventional cigarettes. Statistically significant differences were found between genders for the pattern of tobacco consumption, the number of colleagues/peers who smoke, the opinion about tobacco-free outdoor spaces and the knowledge about new forms of tobacco/nicotine consumption. The university campus is identified by students as the second space where they most consume tobacco products and where they are most exposed to tobacco smoke. This fact forces a reflection on the strategies to be implemented to develop a healthier university.
Exciton valley dynamics probed by Kerr rotation in WSe2 monolayers

We have experimentally studied the pump-probe Kerr rotation dynamics in WSe2 monolayers. This yields a direct measurement of the exciton valley depolarization time tau(nu). At T = 4 K, we find tau(nu) approximate to 6 ps, a fast relaxation time resulting from the strong electron-hole Coulomb exchange interaction in bright excitons. The exciton valley depolarization time decreases significantly when the lattice temperature increases, with tau(nu) being as short as 1.5 ps at 125 K. The temperature dependence is well explained by the developed theory, taking into account the exchange interaction and fast exciton scattering time on the short-range potential.
COSMOLOGY OF CHAMELEONS WITH POWER-LAW COUPLINGS

In chameleon field theories, a scalar field can couple to matter with gravitational strength and still evade local gravity constraints due to a combination of self-interactions and the couplings to matter. Originally, these theories were proposed with a constant coupling to matter; however, the chameleon mechanism also extends to the case where the coupling becomes field dependent. We study the cosmology of chameleon models with power-law couplings and power-law potentials. It is found that these generalized chameleons, when viable, have a background expansion very close to ΛCDM, but can in some special cases enhance the growth of the linear perturbations at low redshifts. For the models we consider, it is found that this region of the parameter space is ruled out by local gravity constraints. Imposing a coupling to dark matter only, the local constraints are avoided, and it is possible to have observable signatures on the linear matter perturbations.
Scattering of massive W bosons into gravitinos and tree unitarity in broken supergravity

The WW scattering into gravitino and gaugino is here investigated in the broken phase, by using both gauge and mass eigenstates. Differently from what is obtained for unbroken gauge symmetry, we find in the scattering amplitudes new structures, which can lead to violation of unitarity above a certain scale. This happens because, in the annihilation diagram, the longitudinal degrees of freedom in the propagator of the gauge bosons disappear from the amplitude, by virtue of the SUGRA vertex. We show that the longitudinal polarizations of the on-shell W become strongly interacting in the high energy limit, and that the inclusion of diagrams with off-shell scalars of the MSSM does not cancel the divergences.
Evaluation of Resting Serum Bile Acid Concentrations in Dogs with Sepsis

Simple Summary There is paucity of information in the veterinary literature regarding bile acid concentrations in septic dogs. Nonetheless, in critically ill human patients, bile acids concentrations are suggested to be an early predictor of short-term survival. This study, therefore, aimed to assess resting bile acid concentrations in a population of septic dogs and ascertain if comparably to human medicine, septic dogs would have higher bile acid concentrations when compared to non-septic dogs. Medical records of dogs presenting to a single referral center over a twelve-year period were retrospectively reviewed. Twenty-six client-owned dogs with a diagnosis of sepsis were included. Two control groups of non-septic dogs (ill control and orthopedic control) were also included. Resting serum bile acid concentrations were significantly higher in the septic group compared to the non-septic group combined. However, no difference in resting serum bile acid concentrations was identified between the septic and the orthopedic control group alone. Abstract Recent studies in the human literature suggest that serum bile acid concentrations could be an early predictor of short-term survival in critically ill patients. However, there is no available information in the veterinary literature regarding serum bile acid concentrations in dogs with sepsis. We aimed to evaluate if resting serum bile acid concentrations differ between septic and non-septic dogs. This was a retrospective observational study, of medical records at a single referral center over a twelve-year period. Twenty-six client-owned dogs diagnosed with sepsis were identified. Twenty-one dogs presenting with a non-hepatobiliary systemic disease and twenty-nine dogs admitted for an elective orthopedic procedure, considered otherwise healthy, were selected as control groups. Resting serum bile acid concentrations were significantly higher in the septic compared to the non-septic groups (ill control and orthopedic control groups). However, when assessing bile acid concentrations between groups individually, no difference was identified between the septic and the orthopedic control group. These results should be interpreted cautiously.
A Jet Source of Event Horizon Telescope Correlated Flux in M87

Event Horizon Telescope (EHT) observations at 230 GHz are combined with Very Long Baseline Interferometry (VLBI) observations at 86 GHz and high-resolution Hubble Space Telescope optical observations in order to constrain the broadband spectrum of the emission from the base of the jet in M87. The recent VLBI observations of Hada et al. provide much stricter limits on the 86 GHz luminosity and component acceleration in the jet base than were available to previous modelers. They reveal an almost hollow jet on sub-mas scales. Thus, tubular models of the jet base emanating from the innermost accretion disk are considered within the region responsible for the EHT correlated flux. There is substantial synchrotron self-absorbed opacity at 86 GHz. A parametric analysis indicates that the jet dimensions and power depend strongly on the 86 GHz flux density and the black hole spin, but depend weakly on other parameters, such as jet speed, 230 GHz flux density, and optical flux. The entire power budget of the M87 jet, , can be accommodated by the tubular jet. No invisible, powerful spine is required. Even though this analysis never employs the resolution of the EHT, the spectral shape implies a dimension transverse to the jet direction of 12–21 ( ) for ( ), where M is the mass and a is the angular momentum per unit mass of the central black hole.
New Horizons in Gravity: The Trace Anomaly, Dark Energy and Condensate Stars

General Relativity receives quantum corrections relevant at macroscopic distance scales and near event horizons. These arise from the conformal scalar degrees of freedom in the extended effective field theory of gravity generated by the trace anomaly of massless quantum fields in curved space. The origin of these conformal scalar degrees of freedom as massless poles in two-particle intermediate states of anomalous amplitudes in flat space is exposed. At event horizons the conformal anomaly scalar degrees of freedom can have macroscopically large effects on the geometry, potentially removing the classical event horizon of black hole and cosmological spacetimes, replacing them with a quantum boundary layer where the effective value of the gravitational vacuum energy density can change. In the effective theory, the cosmological term becomes a dynamical condensate, whose value depends upon boundary conditions near the horizon. In the conformal phase where the anomaly induced fluctutations dominate, and the condensate dissolves, the effective cosmological "constant" is a running coupling which has an infrared stable fixed point at zero. By taking a positive value in the interior of a fully collapsed star, the effective cosmological term removes any singularity, replacing it with a smooth dark energy interior. The resulting gravitational condensate star configuration resolves all black hole paradoxes, and provides a testable alternative to black holes as the final state of complete gravitational collapse. The observed dark energy of our universe likewise may be a macroscopic finite size effect whose value depends not on microphysics but on the cosmological horizon scale.
Exact analytical solution of the linear structure growth rate in {Lambda}CDM cosmology and its cosmological applications

We derive the exact analytical solution of the linear structure growth rate in {Lambda}CDM cosmology with flat or curved geometry, under the Newtonian gauge. Unlike the well known solution under the Newtonian limit [D. J. Heath, Mon. Not. R. Astron. Soc. 179, 351 (1977)], our solution takes all general relativistic corrections into account and is hence valid at both the sub- and superhorizon scales. With this exact solution, we evaluate cosmological impacts induced by these relativistic corrections. (1) General relativistic corrections alter the density growth from z=100 to z=0 by 10% at k=0.01 h/Mpc and the impact becomes stronger toward larger scales. We caution the readers that the overdensity is not gauge invariant and the above statement is restrained to the Newtonian gauge. (2) Relativistic corrections introduce a k{sup -2} scale dependence in the density fluctuation. It mimics a primordial non-Gaussianity of the local type with f{sub NL}{sup local{approx}}1. This systematical error may become non-negligible for future all sky deep galaxy surveys. (3) Cosmological simulations with box size greater than 1 Gpc are also affected by these relativistic corrections. We provide a postprocessing recipe to correct for these effects. (4) These relativistic corrections affect the redshift distortion. However, at redshiftsmore » and scales relevant to redshift distortion measurements, such effect is negligible. « less
A morphosyntactic and semantic analysis of toponyms among the Luhya: A case of Bungoma County

Onomastics,the study of names has remained an area of marginal significance in research despite its importance in language studies. This paper conducts a morphosyntactic and semantic analysis of toponymns (place names) among the Luhya group of speakers in Western Kenya, Bungoma County. A structural and functional approach is used to analyse the naming patterns with the idea that African names, as signs of language, can be divided into two morpho-syntactic categories:nominal that is, they constitute single words, or syntagmatic, meaning they are made up of sentences or phrases. Purposively sampled thirty place names are selected from the IEBC inventory and nine key respondents from the nine sub counties. The 30 names are subjected to morpho-syntactic analysis whereas the semi-structured interviews are used to elicit data on etimology and meaning of names from the nine respondents within the framework of the Frame Semantic theory by Fillmore, (Fillmore, 1982). The theory is used to ascertain whether the meaning-making elements in the respective toponymns reflect the historical functions and meanings embedded within the names.The findings reveal that Luhya place names are generated through grammatical rules as a result of word transformations. Such names are generated from nominals and their resulting phrases through derivational morphology.Three word formation processes namely, pre-fixation, compounding and borrowing are exhibited in the naming process. Semantically, the study reveals that Luhya place names are transparent and descriptive in terms of their function. Places are named after topographical features, historical events, climatic conditions and prominent people.
Disc formation in turbulent massive cores: circumventing the magnetic braking catastrophe

We present collapse simulations of strongly magnetised, 100 M⊙, turbulent cloud cores. Around the protostars formed during the collapse Keplerian discs with typical sizes of up to 100 AU build up in contrast to previous simulations neglecting turbulence. Analysing the condensations in which the discs form, we show that the magnetic flux loss is not sufficient to explain the build-up of Keplerian discs. The average magnetic field is strongly inclined to the disc which might reduce the magnetic braking efficiency. However, the main reason for the reduced magnetic braking efficiency is the highly disordered magnetic field in the surroundings of the discs. Furthermore, due to the lack of a coherently rotating structure in the turbulent environment of the disc no toroidal magnetic field necessary for angular momentum extraction can build up. Simultaneously the angular momentum inflow remains high due to local shear flows created by the turbulent motions. We suggest that the “magnetic braking catastrophe” is an artefact of the idealised non-turbulent initial conditions and that turbulence provides a natural mechanism to circumvent this problem.
Effect of nutrient and weed management on crop productivity and soil microbial properties in aerobic rice (Oryza sativa)

A field experiment was conducted during rainy (kharif) seasons of 2020 and 2021 at the research farm of ICAR-Indian Agricultural Research Institute, New Delhi to study the effect of nutrient and weed management on crop productivity and soil microbial properties in aerobic rice (Oryza sativa L.). Experiment was conducted in factorial randomized complete block design and replicated thrice. Nutrient management factor comprised 3 levels, viz. Control, 100% and 75% RDF + Biofertilizer (BF) consortia; and weed management factor comprised 5 levels, viz. Weedy check, Pyrazosulfuran + Bispyribac + Almix, Bispyribac + mulch, Sesbania + hand weeding (HW) and weed free check. Significantly higher plant growth and grain yield (4.2 and 4.4 t/ha) and biological yield (11.6 and 11.6 t/ha) of rice were recorded with 100% RDF but these parameters were at par with 75% RDF+ BF consortia. However, soil microbial biomass carbon, nitrogen as well as soil microbial biomass phosphorus were recorded significantly higher with 75% RDF + BF. In weed management treatments significantly higher plant height, no. of tillers, grain yield and biological yield were recorded under weed free check over weedy check and Sesbania + HW but these were recorded at par with Pyrazosulfuran + Bispyribac + almix and Bispyribac + mulch. Soil microbial biomass was significantly higher with Sesbania + HW over weedy check, Pyrazosulfuran + Bispyribac + Almix and weed free check but were at par with Bispyribac + mulch. Hence, 75 % RDF + Biofertilizer consortia along with weed management through Bispyribac at 25 DAS + organic mulch (3 t/ha) may be recommended for enhancing crop productivity and soil microbial properties in aerobic rice.
MAGNIFICENT MAGNIFICATION: EXPLOITING THE OTHER HALF OF THE LENSING SIGNAL

We describe a new method for measuring galaxy magnification due to weak gravitational lensing. Our method makes use of a tight scaling relation between galaxy properties that are modified by gravitational lensing, such as apparent size, and other properties that are not, such as surface brightness. In particular, we use a version of the well-known fundamental plane relation for early-type galaxies. This modified “photometric fundamental plane” uses only photometric galaxy properties, eliminating the need for spectroscopic data. We present the first detection of magnification using this method by applying it to photometric catalogs from the Sloan Digital Sky Survey. This analysis shows that the derived magnification signal is within a factor of three of that available from conventional methods using gravitational shear. We suppress the dominant sources of systematic error and discuss modest improvements that may further enhance the lensing signal-to-noise available with this method. Moreover, some of the dominant sources of systematic error are substantially different from those of shear-based techniques. With this new technique, magnification becomes a useful measurement tool for the coming era of large ground-based surveys intending to measure gravitational lensing.
A 100ks XMM-Newton view of the Seyfert 1.8 ESO113-G010. I. Discovery of large X-ray variability and study of the FeKalpha line complex.

(Abridged) We present here a long (100ks) XMM-Newton follow-up of the Seyfert 1.8 galaxy ESO113-G010 performed in November 2005, in order to study over a longer time-scale its main X-ray properties. The source was found in a higher/softer time-averaged flux state, and timing analysis of this source reveals strong, rapid variability. The Power Spectral Density (PSD) analysis indicates (at 95% c.l.) a break at 3.7 x 10^-4 Hz. This cut-off frequency is comparable to those measured in some other rapidly-variable Seyferts, such as MCG-6-30-15 and NGC4051. From the mass-luminosity-time-scale, we infer that M_BH ranges from 4 x 10^6 - 10^7 M_odot and the source is accreting at or close to the Eddington rate (or even higher). The existing data cannot distinguish between spectral pivoting of the continuum and a two-component origin for the spectral softening, primarily because the data do not span a broad enough flux range. In the case of the two-component model, the fractional offsets measured in the flux-flux plots increase significantly toward higher energies (similar to what is observed in MCG-6-30-15) as expected if there exists a constant reflection component. Contrary to May 2001, no significant highly redshifted emission line is observed (which might be related to the source flux level), while two narrow emission lines at about 6.5keV and 7keV are observed. The S/N is not high enough to establish if the lines are variable or constant. As already suggested by the 2001 observation, no significant constant narrow 6.4keV FeK line (EW~32eV) is observed, hence excluding any dominant emission from distant cold matter such as a torus in this Seyfert type 1.8 galaxy.
Clustering, percolation and directionally convex ordering of point processes

Heuristics indicate that point processes exhibiting clustering of points have larger critical radius $r_c$ for the percolation of their continuum percolation models than spatially homogeneous point processes. It has already been shown, and we reaffirm it in this paper, that the $dcx$ ordering of point processes is suitable to compare their clustering tendencies. Hence, it was tempting to conjecture that $r_c$ is increasing in $dcx$ order. Some numerical evidences support this conjecture for a special class of point processes, called perturbed lattices, which are "toy models" for determinantal and permanental point processes. However, the conjecture is not true in full generality, since one can construct a Cox point process with degenerate critical radius $r_c=0$, that is $dcx$ larger than a given homogeneous Poisson point process. Nevertheless, we are able to compare some nonstandard critical radii related, respectively, to the finiteness of the expected number of void circuits around the origin and asymptotic of the expected number of long occupied paths from the origin in suitable discrete approximations of the continuum model. These new critical radii sandwich the "true" one. Surprisingly, the inequalities for them go in opposite directions, which gives uniform lower and upper bounds on $r_c$ for all processes $dcx$ smaller than some given process. In fact, the above results hold under weaker assumptions on the ordering of void probabilities or factorial moment measures only. Examples of point processes comparable to Poisson processes in this weaker sense include determinantal and permanental processes. More generally, we show that point processes $dcx$ smaller than homogeneous Poisson processes exhibit phase transitions in certain percolation models based on the level-sets of additive shot-noise fields, as e.g. $k$-percolation and SINR-percolation.
THE BOLOCAM GALACTIC PLANE SURVEY: SURVEY DESCRIPTION AND DATA REDUCTION

We present the Bolocam Galactic Plane Survey (BGPS), a 1.1 mm continuum survey at 33″ effective resolution of 170 deg2 of the Galactic Plane visible from the northern hemisphere. The BGPS is one of the first large area, systematic surveys of the Galactic Plane in the millimeter continuum without pre-selected targets. The survey is contiguous over the range −10.5 ⩽ l ⩽ 90.5, |b| ⩽ 0.5. Toward the Cygnus X spiral arm, the coverage was flared to |b| ⩽ 1.5 for 75.5 ⩽ l ⩽ 87.5. In addition, cross-cuts to |b| ⩽ 1.5 were made at l= 3, 15, 30, and 31. The total area of this section is 133 deg2. With the exception of the increase in latitude, no pre-selection criteria were applied to the coverage in this region. In addition to the contiguous region, four targeted regions in the outer Galaxy were observed: IC1396 (9 deg2, 97.5 ⩽ l ⩽ 100.5, 2.25 ⩽ b ⩽ 5.25), a region toward the Perseus Arm (4 deg2 centered on l = 111, b = 0 near NGC 7538), W3/4/5 (18 deg2, 132.5 ⩽ l ⩽ 138.5), and Gem OB1 (6 deg2, 187.5 ⩽ l ⩽ 193.5). The survey has detected approximately 8400 clumps over the entire area to a limiting non-uniform 1σ noise level in the range 11–53 mJy beam−1 in the inner Galaxy. The BGPS source catalog is presented in a previously published companion paper. This paper details the survey observations and data reduction methods for the images. We discuss in detail the determination of astrometric and flux density calibration uncertainties and compare our results to the literature. Data processing algorithms that separate astronomical signals from time-variable atmospheric fluctuations in the data timestream are presented. These algorithms reproduce the structure of the astronomical sky over a limited range of angular scales and produce artifacts in the vicinity of bright sources. Based on simulations, we find that extended emission on scales larger than about 5. ′9 is nearly completely attenuated (>90%) and the linear scale at which the attenuation reaches 50% is 3. ′8. Comparison with other millimeter-wave data sets implies a possible systematic offset in flux calibration, for which no cause has been discovered. This presentation serves as a companion and guide to the public data release (http://irsa.ipac.caltech.edu/Missions/bolocam.html) through NASA's Infrared Processing and Analysis Center (IPAC) Infrared Science Archive (IRSA). New data releases will be provided through IPAC-IRSA with any future improvements in the reduction. The BGPS provides a complementary long-wavelength spectral band for the ongoing ATLASGAL and Herschel-SPIRE surveys, and an important database and context for imminent observations with SCUBA-2 and ALMA.