Figure 7 - uploaded by Alexander Khoperskov
Content may be subject to copyright.
![Distribution of inclinations i of spiral galaxies: (a) for NGC and IC galaxies with "rows" (276 objects of our catalog-the shaded bars, 406 objects including NGC objects from the catalog of Chernin et al. [3]-заштрихованные столбцы); the dashed bars); (b) for all spiral galaxies of the NGC/IC catalogs (according to HyperLeda data); the stripped barfir those with i ≥ 90 •](profile/Alexander-Khoperskov-2/publication/319627560/figure/fig5/AS:601022225453058@1520306273058/Distribution-of-inclinations-i-of-spiral-galaxies-a-for-NGC-and-IC-galaxies-with.png)
Distribution of inclinations i of spiral galaxies: (a) for NGC and IC galaxies with "rows" (276 objects of our catalog-the shaded bars, 406 objects including NGC objects from the catalog of Chernin et al. [3]-заштрихованные столбцы); the dashed bars); (b) for all spiral galaxies of the NGC/IC catalogs (according to HyperLeda data); the stripped barfir those with i ≥ 90 •
Source publication
Galaxies with “rows” in Vorontsov-Velyaminov’s terminology stand out among the variety of spiral galactic patterns. A characteristic feature of such objects is the sequence of straight-line segments that forms the spiral arm. In 2001 A. Chernin and co-authors published a catalog of such galaxies which includes 204 objects from the Palomar Atlas. In...
Contexts in source publication
Context 1
... pattern, and we exclude these objects from consideration. Figure 7 demonstrates the qualitative similar- ity of galaxies with "rows" and all S-type NGC and IC galaxies as far as the distribution of in- clinations iis concerned. In both cases we have a bell-shaped distribution with a maximum near 40 • for galaxies with "rows" and 50 • for all S-type galaxies. The nonuniformity of the distribution Straight-line segments are difficult to identify in galaxies with large inclination and that us why, given the incompleteness of our sample, hereafter for inclinations i 55 • (see Fig. 7), we show the distributions for both the combined sample of galaxies with "rows", and separately for galax- ies with i < 55 • . The angle between the adjacent "rows" is usually close to α = 120 • (Fig. 8). The average angle is equal to 126 • , both for our en- tire sample and for barred galaxies, in agreement with the result of Chernin et al. [3]. According to HyperLeda, UBV photometry with color indices corrected for selective Galactic extinction and galaxy disk inclination is available for 34% of the galaxies with "rows" from our cat- alog. Figure 11 shows the results of our numerical N-body mod- els where straight-line arm segments and even almost kink points can be seen. Let us point out 20 Figure 8. Histogram of the distribution of angles α between the adjacent "rows": (a) for all galaxies of sample [3]; (b) for our sample of galaxies. The light-shaded bars show the distribution for galaxies with i < 55 • Figure 9. Distribution of the −MHI /LB ratio (in solar units) for galaxies with "rows": (a) for the full -Polygonal structure consists of one to three "rows", unlike what we have in gas- dynamic models, where a global system of "rows" ...
Context 2
... pattern, and we exclude these objects from consideration. Figure 7 demonstrates the qualitative similar- ity of galaxies with "rows" and all S-type NGC and IC galaxies as far as the distribution of in- clinations iis concerned. In both cases we have a bell-shaped distribution with a maximum near 40 • for galaxies with "rows" and 50 • for all S-type galaxies. The nonuniformity of the distribution Straight-line segments are difficult to identify in galaxies with large inclination and that us why, given the incompleteness of our sample, hereafter for inclinations i 55 • (see Fig. 7), we show the distributions for both the combined sample of galaxies with "rows", and separately for galax- ies with i < 55 • . The angle between the adjacent "rows" is usually close to α = 120 • (Fig. 8). The average angle is equal to 126 • , both for our en- tire sample and for barred galaxies, in agreement with the result of Chernin et al. [3]. According to HyperLeda, UBV photometry with color indices corrected for selective Galactic extinction and galaxy disk inclination is available for 34% of the galaxies with "rows" from our cat- alog. Figure 11 shows the results of our numerical N-body mod- els where straight-line arm segments and even almost kink points can be seen. Let us point out 20 Figure 8. Histogram of the distribution of angles α between the adjacent "rows": (a) for all galaxies of sample [3]; (b) for our sample of galaxies. The light-shaded bars show the distribution for galaxies with i < 55 • Figure 9. Distribution of the −MHI /LB ratio (in solar units) for galaxies with "rows": (a) for the full -Polygonal structure consists of one to three "rows", unlike what we have in gas- dynamic models, where a global system of "rows" ...
Similar publications
In this work, I present an optimization problem which consists of assigning entries of a stellar catalog to multiple entries of another stellar catalog such that the probability of such assignment is maximum. I prove that the problem is NP-Hard and show a way of modeling this problem as a maximum weighted stable set problem. A real application is s...
The procedure for compilation of a new proton catalog is presented here. The focus is on the SOHO/ERNE instrument for the period 1996 to 2016 (entire solar cycle 23 and the ongoing solar cycle 24). The main steps of the data analysis are outlined. Namely, as a first approach it is selected that 5-min averaged data will be used to identify the peak...
Peixos de la subconca del riu Tomo, Orinòquia colombiana: actualització de la llista d’espècies
El riu Tomo recorre longitudinalment la plana alta de l’orient de Colòmbia, coneguda com a “altillanura”, i desemboca directament al riu Orinoco. La llista ictiològica actualitzada d’aquest riu es va elaborar a partir de la revisió i depuració de cinc f...
We address the problem of disambiguating large scale catalogs through the definition of an unknown artist clustering task. We explore the use of metric learning techniques to learn artist embeddings directly from audio, and using a dedicated homonym artists dataset, we compare our method with a recent approach that learn similar embeddings using ar...
Citations
... Remarkably, this arm contains two or three straight sections ('rows'). Such features often observed in galaxies with the ordered spiral arms may be considered as a sign of strong large-scale shock waves linked with spiral arms (see Chernin et al. 2001;Butenko & Khoperskov 2017, and the references therein). In contrast, the opposite (northern) spiral arm looks rather smoothed and badly defined, although the extended emission regions are observed along the whole arm. ...
We study three Arp’ systems of peculiar galaxies, Arp 42 (NGC 5829), Arp 82 (NGC 2535/36), and Arp 58 (UGC 4457), using the long-slit spectral observations carried out at the 6m telescope BTA of Special Astrophysical Observatory. Arp 82 and Arp 58 are the M51-type systems. In the third system, Arp 42, there are two extremely luminous kpc-sized clumps observed at the end of the bifurcated spiral arm, however the source of perturbations remains unknown. From the emission line measurements we analyzed the distribution of gas line-of-sight velocity, velocity dispersion, and gas-phase metallicity along the slits estimated by different methods. A special attention is paid to the young regions of star formation at the peripheries of the galaxies and in tidal debris, their connection with gas kinematics and abundance. All three systems show the signs of velocity disturbances and the presence of regions of locally enhanced gas velocity dispersion, as well as the regions of diffuse ionized gas. A distribution of oxygen reveals shallow radial abundance gradients, typical for interacting systems. A faint spiral-like branches of tidal bridges that are observed in NGC 2535 and UGC 4457 may represent the remnants of pre-existing ‘old’ mode of spiral waves.
... The southern spiral arm contains bright clumps of H . Remarkably, this arm contains two or three straight sections ('rows'). Such features often observed in galaxies with the ordered spiral arms may be considered as a sign of strong large-scale shock waves linked with spiral arms (see Chernin et al. 2001;Butenko & Khoperskov 2017, and the references therein). In contrast, the opposite (northern) spiral arm looks rather smoothed and badly defined, although the extended emission regions are observed along the whole arm. ...
We study three Arp' systems of peculiar galaxies: Arp 42 (NGC 5829), Arp 82 (NGC 2535/36) and Arp 58 (UGC 4457), using the long-slit spectral observations carried out at the 6m telescope BTA of Special Astrophysical Observatory. Arp 82 and Arp 58 are the M51-type systems. In the third system - Arp 42, there are two extremely luminous kpc-sized clumps observed at the ends of the bifurcated spiral arm, however the source of perturbations remains unknown. From the emission line measurements we analyzed the distribution of gas line-of-sight (LOS) velocity, velocity dispersion and gas-phase metallicity along the slits estimated by different methods. A special attention is paid to the young regions of star formation at the peripheries of the galaxies and in tidal debris, their connection with gas kinematics and abundance. All three systems show the signs of velocity disturbances and the presence of regions of locally enhanced gas velocity dispersion, as well as the regions of diffuse ionized gas. A distribution of oxygen reveals shallow radial abundance gradients, typical for interacting systems. A faint spiral-like branches of tidal bridges which are observed in NGC 2535 and UGC 4457 may represent the remnants of pre-existing "old" mode of spiral waves.
... In this work, we study the phenomenon of so-called "rows" (straight segments), which are one of the characteristic details of spiral arms, and they are observed in approximately 5-10% S-galaxies [8,9]. B. A. Vorontsov-Vel'yaminov was the first to detect the straightened segments in the arms of some galaxies [10], highlighting them in extragalactic nebulae images. ...
... The sequences of such straightened segments are also called polygonal structures [11]. Two catalogs of galaxies with rows contain 480 objects [8,9]. Statistical analysis of the properties of galaxies with rows indicates that such objects are typical spiral galaxies [9]. Figure 1 shows examples of images of galaxies with rows in different spectral bands. ...
... Two catalogs of galaxies with rows contain 480 objects [8,9]. Statistical analysis of the properties of galaxies with rows indicates that such objects are typical spiral galaxies [9]. Figure 1 shows examples of images of galaxies with rows in different spectral bands. ...
The work is aimed at studying the formation mechanisms of straightened segments (rows) in spiral galactic arms, which are found in approximately 5% of S-galaxies. We use the Smoothed Particles Hydrodynamics (SPH) numerical algorithm, which is adapted for parallel computing on the GPUs to simulate the gas component. N-body model is used to simulate the dynamics of collisionless stellar disk. Graphic processors allow you to apply the “Particle-Particle” algorithm (each particle interacts with every other particle), which is the most accurate method to account for self-gravity. Our numerical model demonstrates the formation of a rows system with a pronounced transient character.
