Metal-THINGS: On the Metallicity and Ionization of ULX Sources in NGC 925

Galaxie

Construction of annual cycle of preparation of sportsmen, specialized in cheerleading. [Postroenie godovogo cikla podgotovki sportsmenov, specializiruiushchikhsia v cherlidinge]

The plan-chart of distributing of educational material is rotined in the annual loop of preparation of sportsmen. In an experiment took part 42 sportsmen in age 18-19 years. It is marked that duration of setup time is occupied by to 6 months of preparation. The following correlation of elements is recommended in the structure of competition period: 10% is a body-conditioning, 20% is the special physical preparation, 70% is technical preparation. It is marked that it is necessary to concentrate basic attention on working off competition composition, elements and synchronousness at implementation of compositions. It becomes firmly established that the transitional period of sportsmen is directed on renewal of physical and psychological potential. In this period it is recommended to bring in adjustments in competition compositions or make new

Two types of distribution of the gas velocity dispersion of MaNGA galaxies

The distribution of the gas velocity dispersion σ across the images of 1146 MaNGA galaxies is analyzed. We find that there are two types of distribution of the gas velocity dispersion across the images of galaxies: (i) the distributions of 909 galaxies show a radial symmetry with or without the σ enhancement at the center ("R distribution", radial symmetry in the σ distribution) and (ii) distributions with a band of enhanced σ along the minor axis in the images of 159 galaxies with or without the σ enhancement at the center ("B distribution", band in the σ distribution). The σ distribution across the images of 78 galaxies cannot be reliable classified. We select 806 galaxies with the best defined characteristics (this sample includes 687 galaxies with R distribution and 119 galaxies with B distribution) and compare the properties of galaxies with R and B distributions. We find that the median value of the gas velocity dispersion σm in galaxies with B distribution is higher by around 5 km s-1, on average, than that of galaxies with R distribution. The optical radius R25 of galaxies with B distribution is lower by around 0.1 dex, on average, than that of galaxies with similar masses with R distribution. Thus the properties of a galaxy are related to the type of distribution of the gas velocity dispersion σ across its image. This suggests that the presence of the band of the enhanced gas velocity dispersion can be an indicator of a specific evolution (or a specific stage in the evolution) of a galaxy

Breaks in surface brightness profiles and radial abundance gradients in the discs of spiral galaxies

We examine the relation between breaks in the surface brightness profiles and radial abundance gradients within the optical radius in the discs of 134 spiral galaxies from the CALIFA survey. The distribution of the radial abundance (in logarithmic scale) in each galaxy was fitted by simple and broken linear relations. The surface brightness profile was fitted assuming pure and broken exponents for the disc. We find that the maximum absolute difference between the abundances in a disc given by broken and pure linear relations is less than 0.05 dex in the majority of our galaxies and exceeds the scatter in abundances for 26 out of 134 galaxies considered. The scatter in abundances around the broken linear relation is close (within a few percent) to that around the pure linear relation. The breaks in the surface brightness profiles are more prominent. The scatter around the broken exponent in a number of galaxies is lower by a factor of two or more than that around the pure exponent. The shapes of the abundance gradients and surface brightness profiles within the optical radius in a galaxy may be different. A pure exponential surface brightness profile may be accompanied by a broken abundance gradient and vise versa. There is no correlation between the break radii of the abundance gradients and surface brightness profiles. Thus, a break in the surface brightness profile does not need to be accompanied by a break in the abundance gradient.© ESO, 2017.Peer Reviewe

Circumnuclear regions of different BPT types in star-forming MaNGA galaxies: AGN detectability

© ESO 2020. We consider the circumnuclear regions of star-forming MaNGA galaxies. The spaxels spectra are classified as active-galactic-nucleus-like (AGN-like), H» II-region-like (or SF-like), and intermediate (INT) spectra according to their positions on the Baldwin-Phillips-Terlevich (BPT) diagram. There are the following four configurations of the radiation distributions in the circumnuclear regions in (massive) galaxies: (1) AGN+INT, the innermost region of the AGN-like radiation is surrounded by a ring of radiation of the intermediate type; (2) INT, the central area of radiation of the intermediate type; (3) SF+INT, the inner region of the H» II-region-like radiation is surrounded by a ring of radiation of the intermediate type; and (4) SF, the central area of the H» II-region-like radiation only. The low ionization nuclear emission line regions (LINERs) of configurations 1 and 2 are examined. The spaxel spectra of the LINERs form a sequences on the BPT diagram, that is, they lie along the known AGN-SF mixing line trajectories. The diagnostic line ratios of the spaxels spectra change smoothly with radius, from AGN-like (or INT) line ratios at the galactic center to H» II-region-like at larger galactocentric distances. This is in agreement with the paradigm that the LINERs are excited by AGN activity. We found that the AGN and INT radiation in the circumnuclear region is accompanied by an enhanced gas velocity dispersion σgas. The radius of the area of the AGN and INT radiation is similar to the radius of the area with enhanced σgas, and the central σgas, c correlates with the luminosity of the AGN+INT area. We assume that the gas velocity dispersion can serve as an indicator of the AGN activity. An appreciable enhancement of σgas, c was also measured in the SF-type centers of massive galaxies. The values of σgas, c for the SF-type centers partly overlap with those of the AGN-type centers. This suggests that the manifestation of the circumnuclear region as AGN or as SF on the BPT diagram depends not only on the value of σgas, c (the level of the AGN activity) but it is also governed by an additional parameter(s). We find that there is a demarcation line between the positions of the AGN-type and SF-type objects on the central gas velocity dispersion - central Hα surface brightness diagram, in the sense that an object with a given value of σgas, c is an AGN-type only if the central Hα surface brightness is lower than some value

Properties of galaxies with an offset between the position angles of the major kinematic and photometric axes

© ESO 2020. We derive the photometric, kinematic, and abundance characteristics of 18 star-forming MaNGA galaxies with fairly regular velocity fields and surface brightness distributions and with a large offset between the measured position angles of the major kinematic and photometric axes, ΔPA ≳ 20°. The aim is to examine if there is any other distinctive characteristic common to these galaxies. We found morphological signs of interaction in some (in 11 out of 18) but not in all galaxies. The observed velocity fields show a large variety; the maps of the isovelocities vary from an hourglass-like appearance to a set of straight lines. The position angles of the major kinematic axes of the stellar and gas rotations are close to each other. The values of the central oxygen abundance, radial abundance gradient, and star formation rate are distributed within the intervals defined by galaxies with small (no) ΔPA of similar mass. Thus, we do not find any specific characteristic common to all galaxies with large ΔPA. Instead, the properties of these galaxies are similar to those of galaxies with small (no) ΔPA. This suggests that either the reason responsible for the large ΔPA does not influence other characteristics or the galaxies with large ΔPA do not share a common origin, they can, instead, originate through different channels

The prevalence and diagnosis of rare (orphan) diseases in pediatric population of the Russian Federation

Objective of the research: to determine the prevalence of various nosological forms of rare (orphan) diseases in pediatric population of the Russian Federation (RF) to expand and improve diagnostic resources. Materials and methods: the prevalence of individual nosological forms of life-threatening and chronic progressive rare diseases in pediatric populationwas calculated according to the regional segments of the Federal Register. The results of fetus ultrasound screening, samples for biochemical screening and coverage of children with neonatal screening in the Russian Federation are evaluated. Results: the study revealed an increase in the prevalence of rare diseases due to the majority of nosological forms without changing their structure. For many nosological forms, an increase in their prevalence was accompanied by a decrease in the proportion of children among all patients. A high coverage of pregnant women with ultrasound screening was revealed. The number of fetuses with identified congenital malformations did not exceed 2%. Disorders during biochemical screening tests were recorded in 3-5% of cases. Neonatal screening coverage was not more than 95%. In 2013-2018, 49, 9 million screening tests were performed and 7, 7 thousand newborns with congenital and hereditary diseases were identified. The necessity of including in the neonatal screening of orphan diseases in which the use of pathogenetic therapy is possible is substantiated. Conclusion: determining the prevalence of various nosological forms of orphan diseases is extremely important and necessary to expand and improve their diagnosis, which will increase the detection of this pathology. © 2020, Pediatria Ltd.. All rights reserved