arXiv subjects

George Gontcharov

Publications and source records attributed to George Gontcharov.

At least 19 recordsLinked to original sources

arXiv2023

The problem of dust attenuation in photometric decomposition of edge-on galaxies and possible solutions

The presence of dust in spiral galaxies affects the ability of photometric decompositions to retrieve the parameters of their main structural components. For galaxies in an edge-on orientation, the optical depth integrated over the line-of-sight is significantly higher than for those with intermediate or face-on inclinations, so it is only natural to expect that for edge-on galaxies, dust attenuation should severely influence measured structural parameters. In this paper, we use radiative transfer simulations to generate a set of synthetic images of edge-on galaxies which are then analysed via decomposition. Our results demonstrate that for edge-on galaxies, the observed systematic errors of the fit parameters are significantly higher than for moderately inclined galaxies. Even for models with a relatively low dust content, all structural parameters suffer offsets that are far from negligible. In our search for ways to reduce the impact of dust on retrieved structural parameters, we test several approaches, including various masking methods and an analytical model that incorporates dust absorption. We show that using such techniques greatly improves the reliability of decompositions for edge-on galaxies.

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arXiv2020

Gaia DR2 giants in the Galactic dust -- II. Application of the reddening maps and models

We exploit a complete sample of 101\,810 {\it Gaia} DR2 giants, selected in Paper I in the space cylinder with a radius of 700 pc around the Sun and a height of $|Z|=1800$ pc, using the {\it Gaia} DR2 parallaxes, $G_\mathrm{BP}$ and $G_\mathrm{RP}$ photometry, and {\it WISE} $W3$ photometry. We explain the spatial variations of the modes of the observables $G_\mathrm{BP}-G_\mathrm{RP}$ and $G_\mathrm{RP}-W3$ by the spatial variations of the corresponding reddenings described in the GM20 3D dust distribution model. Presented in this paper, GM20 is an advanced version of the model introduced by Gontcharov in 2009. GM20 proposes two intersecting dust layers, along the Galactic mid-plane and in the Gould Belt, with exponential vertical and sinusoidal longitudinal variations of the dust spatial density in each layer. The Belt layer is an ellipse, oriented nearly between the centre and anticentre of the Galaxy, and with a semi-major and semi-minor axes of 600 and 146~pc, respectively. $G_\mathrm{BP}-G_\mathrm{RP}$ and $G_\mathrm{RP}-W3$ give similar solutions, but different equatorial layer scale heights of $150\pm15$ and $180\pm15$~pc, respectively, and $(G_\mathrm{BP}-G_\mathrm{RP})_0=(1.14\pm0.01)-(0.022\pm0.010)\,|Z|$, $(G_\mathrm{RP}-W3)_0=(1.44\pm0.01)-(0.015\pm0.010)\,|Z|$, where $Z$ is in kpc. We compare GM20 with several 3D reddening models and maps in their ability to predict the observed colour modes. GM20 and the 3D map by Gontcharov appear to be the best among the models and maps, respectively. However, the most reliable models and maps mainly disagree only in their estimates of low reddening, including the reddening across the whole dust layer.

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arXiv2018

Kinematics of B-F Stars as a Function of Their Dereddened Color from Gaia and PCRV Data

Parallaxes with an accuracy better than 10% and proper motions from the Gaia DR1 TGAS catalogue, radial velocities from the PCRV, Tycho-2 photometry, PARSEC, MIST, YaPSI, BaSTI isochrones, and the most accurate reddening and extinction estimates have been used to analyze the kinematics of 9543 thin-disk B-F stars as a function of their dereddened color. These stars are located on the Hertzsprung-Russell diagram relative to the isochrones with a high accuracy. This has allowed me to conclude that the reddening and extinction were significantly underestimated in some kinematic studies of other authors. The median accuracy of the velocity components U, V, W in this study is 1.7 km/s, although outside the range $-0.1<(B_T-V_T)_0<0.5$ the kinematic characteristics are noticeably biased due to the incompleteness of the sample. We have confirmed the variations in the mean velocity of stars relative to the Sun and the stellar velocity dispersion as a function of their dereddened color known from the Hipparcos data. Given the age estimates for the stars under consideration from the TRILEGAL model and the Geneva-Copenhagen survey, these variations may be considered as variations as a function of the age. A comparison of our results with the results of other studies of the stellar kinematics near the Sun has shown that selection and reddening underestimation explain almost completely the discrepancies between the results. The dispersions and mean velocities from the results of reliable studies fit into a $\pm2$ km/s corridor, while the ratios $σ_V/σ_U$ and $σ_W/σ_U$ fit into $\pm0.05$. Based on all reliable studies in the range $-0.1<(B_T-V_T)_0<0.5$, i.e., for an age from 0.23 to 2.4 Gyr, we have found that the stellar velocity dispersions in km/s are proportional to the age in Gyr raised to the power $β_U=0.33$, $β_V=0.285$, and $β_W=0.37$.

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arXiv2017

Verifying reddening and extinction for Gaia DR1 TGAS main sequence stars

We compare eight sources of reddening and extinction estimates for approximately 60,000 {\it Gaia} DR1 Tycho--Gaia Astrometric Solution (TGAS) main sequence stars younger than 3~Gyr with a relative error of the {\it Gaia} parallax less than 0.1. For the majority of the stars, the best 2D dust emission-based reddening maps show considerable differences between the reddening to infinity and the one calculated to the stellar distance using the barometric law of the dust distribution. This proves that the majority of the TGAS stars are embedded in to the Galactic dust layer and a proper 3D treatment of the reddening/extinction is required to reliably calculate their de-reddened colors and absolute magnitudes. The sources with the 3D estimates of reddening are tested in their ability to put the stars among the PARSEC and MIST theoretical isochrones in the Hertzsprung--Russell diagram based on the precise {\it Gaia}, {\it Tycho-2}, 2MASS and {\it WISE} photometry. Only the reddening/extinction estimates by Arenou et al. (1992), Gontcharov (2012), and Gontcharov (2017), being appropriate for nearby stars within 280~pc, provide both the minimal number of outliers bluer than any reasonable isochrone and the correct number of stars younger than 3~Gyr in agreement with the Besançon Galaxy model.

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arXiv2017

Production, Processing and Consumption of the Dust in the Galaxy

The recent results obtained by the modern telescopes and spacecrafts allow us for the first time to compare directly the mass, spatial density and size distribution of the dust grains in the regions of their production, processing and consumption in our Galaxy. The ALMA and VLT/SPHERE telescopes allow us to estimate the production of the dust by supergiants and collapsing core supernovae. The 2MASS, WISE, SDSS, Planck and other telescopes allow us to estimate the processing of the dust in the interstellar medium. After renewed Besançon Galaxy model the medium appears to contain about half the local mass of matter (both baryonic and dark) in the Galactic neighborhood of the Sun. The Helios, Ulysses, Galileo, Cassini and New Horizons spacecrafts allow us to estimate the consumption of the dust into large solid bodies. The results are consistent each other assuming the local mean spatial density of the dust is about of $3.5\times10^{-26}$ g/cm$^3$, mean density of the grain is about 1 g/cm$^3$, and the dust production rate is about of 0.015 Solar mass per year for whole the Galaxy.

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arXiv2017

Spatial Variations of the Interstellar Polarization and Interstellar Extinction

For more than 5000 stars with accurate parallaxes from the Hipparcos and Gaia DR1 Tycho-Gaia astrometric solution (TGAS), Tycho-2 photometry, interstellar polarization from eight catalogues and interstellar extinction from eight 3D maps the largest up to date comparison of the polarization and extinction is provided. The extinction maps give different estimations of the extinction and of the polarization efficiency as the polarization divided into extinction $P/A_V$ as well as of the percentage of the stars with the polarization efficiency higher than the limit of Serkowski $P/A_V>0.03$. Using the Hipparcos parallaxes we found about 200 stars (4\%, mainly OB stars) drop higher than the limit when we use any extinction map. However, the usage of more accurate TGAS parallaxes decreases them to only 17 stars (0.3\%). The polarization and extinction are negligible inside the Local Bubble within 80 pc from the Sun. In the vast Bubble's shell at the distances 80--118 pc from the Sun the polarization and extinction rapidly grow with the distance whereas the position angle of the polarization is oriented predominantly along the shell of the Bubble. Outside the Bubble the polarization and extinction grow with the distance slowly. In addition, within a radius of 80--300 pc of the Sun a disc of some filamentary dust clouds (including well-known Markkanen cloud) is observed as in the polarization map as in the reddening one by Schlegel et al. In this disc the position angle of polarization is preferably oriented along the plane of the disk. For the regions further than 300 pc the position angle of polarization is preferably oriented along the Local spiral arm, i.e. Y coordinate axis. The polarization and its efficiency is lower in the dust layer in the Gould belt than in the equatorial dust layer. It may means different properties of dust in these two layers.

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arXiv2017

3D Reddening and Extinction Maps at the Beginning of the Gaia Era

The vast majority of Gaia DR1 Tycho-Gaia astrometric solution (TGAS) stars are located within a distance of 1200 pc from the Sun and up to 600 pc within the Galactic plane. Complete usage of their parallaxes is possible only if their reddening and interstellar extinction are known. We obtained those from a comparison of the eight most accurate and complete 3D maps of reddening and extinction in the considered space. We analyzed the statistics of the maps and their differences in the cells of $20\times20\times20$ pc in the whole considered space. The comparison of the maps in the cells outside the dust layer allows us to obtain a formula of the correction for both overestimated and minimal reddenings of the SFD map through the dust half-layer. We point out the need for a further study of the minimal reddening through the dust half-layer and the overestimation of higher reddenings by use of the most precise data. Based on the data of all the maps under consideration we compile two catalogues of the reddenings: for 630,109 cells of $20\times20\times20$ pc in the considered space and for 1,758,723 TGAS stars with the most accurate distances.

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arXiv2017

Systematic Error of the Gaia DR1 TGAS Parallaxes from Data for the Red Giant Clump

Based on the Gaia DR1 TGAS parallaxes and photometry from the Tycho-2, Gaia, 2MASS, and WISE catalogues, we have produced a sample of about 100 000 clump red giants within about 800 pc of the Sun. The systematic variations of the mode of their absolute magnitude as a function of the distance, magnitude, and other parameters have been analyzed. We show that these variations reach 0.7 mag and cannot be explained by variations in the interstellar extinction or intrinsic properties of stars and by selection. The only explanation seems to be a systematic error of the Gaia DR1 TGAS parallax dependent on the square of the observed distance in kpc: $0.18R^2$ mas. Allowance for this error reduces significantly the systematic dependences of the absolute magnitude mode on all parameters. This error reaches 0.1 mas within 800 pc of the Sun and allows an upper limit for the accuracy of the TGAS parallaxes to be estimated as 0.2 mas. A careful allowance for such errors is needed to use clump red giants as "standard candles". This eliminates all discrepancies between the theoretical and empirical estimates of the characteristics of these stars and allows us to obtain the first estimates of the modes of their absolute magnitudes from the Gaia parallaxes: $mode(M_H)=-1.49^m\pm0.04^m$, $mode(M_{K_s})=-1.63^m\pm0.03^m$, $mode(M_{W1})=-1.67^m\pm0.05^m$, $mode(M_{W2})=-1.67^m\pm0.05^m$, $mode(M_{W3})=-1.66^m\pm0.02^m$, $mode(M_{W4})=-1.73^m\pm0.03^m$, as well as the corresponding estimates of their de-reddened colors.

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arXiv2017

Using the reduced proper motions of Tycho-2 stars with B-V from 0.75 to 1.25: Monte Carlo simulations

The stellar composition of the Tycho-2 Catalogue in the range $0.75<B-V<1.25$ has been reproduced through Monte Carlo simulations. For young and old stars of the red giant clump (RGC), the red giant branch, subgiants, red dwarfs, and thick-disk giants, we have specified the distributions in coordinates, velocities, $B-V$, and $M_V$ as a function of $B-V$ and calculated their reduced proper motions, photometric distances from the $(B-V)-M_V$ calibration, and photoastrometric distances from the reduced proper motion -- $M_V$ calibration. Our simulations have shown the following: (1) a sample of thin-disk giants within 500 pc with an admixture of less than 10\% of other stars can be produced; (2) a sample of dwarfs within 100 pc almost without any admixture of other stars can be produced; (3) the Local Spiral Arm affects the RGC composition of any magnitude-limited catalog in favor of giants younger than 2 Gyr; (4) the samples produced using reduced proper motions can be used for kinematic studies, provided that the biases of the quantities being determined are simulated and taken into account; (5) the photometric distances correlate with the photoastrometric ones because of the correlation between the proper motion and magnitude; (6) the photometric distances are closer to the true ones for the red giant branch and red dwarfs as the categories of stars with a clear $(B-V)-M_V$ relation, while the photoastrometric distances are closer to the true ones for the RGC, subgiants, and thick-disk giants; (7) the calculated distances differ systematically from the true ones, but they can be used to analyze the three-dimensional distribution of stars. Our simulations confirm the validity of our previous selection of RGC stars from Tycho-2.

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arXiv2017

3D Stellar Reddening Map from 2MASS Photometry: An Improved Version

An improved version of the 3D stellar reddening map in a space with a radius of 1200 pc around the Sun and within 600 pc of the Galactic midplane is presented. As in the previous 2010 and 2012 versions of the map, photometry with an accuracy better than $0.05^m$ in the $J$ and $K_s$ bands for more than 70 million stars from the 2MASS catalogue is used in the new version. However, the data reduction technique is considerably more complicated. As before, an analysis of the distribution of stars near the main-sequence turnoff on the $(J-K_s)$ - $K_s$ diagram, where they form a distribution maximum, provides a basis for the method. The shift of this maximum, i.e., the $mode(J-K_s)$, along $(J-K_s)$ and $K_s$, given the spatial variations of the mean de-reddened color $(J-K_s)_0$ of these stars, is interpreted as a growth of the reddening with increasing distance. The main distinction of the new method is that instead of the fixed mean absolute magnitude, de-reddened color, distance, and reddening for each cell, the individual values of these quantities are calculated for each star by iterations when solving the system of equations relating them. This has allowed one to increase the random accuracy of the map to $0.01^m$ and its spatial resolution to 20 pc in coordinates and distance and to $1^{\circ}$ in longitude and latitude. Comparison with other reddening estimates for the same spatial cells and Gaia DR1 TGAS stars shows that the constructed map is one of the best maps for the space under consideration. Its systematic errors have been estimated to be $σ(E(J-K_s))=0.025^m$, or $σ(E(B-V))=0.04^m$. The main purpose of the map is to analyze the characteristics of Galactic structures, clouds, and cloud complexes. For this purpose, the reddening map within each spatial cell has also been computed by analyzing the reddening along each line of sight.

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arXiv2017

Interstellar Extinction

This review describes our current understanding of interstellar extinction. This differ substantially from the ideas of the 20th century. With infrared surveys of hundreds of millions of stars over the entire sky, such as 2MASS, SPITZER-IRAC, and WISE, we have looked at the densest and most rarefied regions of the interstellar medium at distances of a few kpc from the sun. Observations at infrared and microwave wavelengths, where the bulk of the interstellar dust absorbs and radiates, have brought us closer to an understanding of the distribution of the dust particles on scales of the Galaxy and the Universe. We are in the midst of a scientific revolution in our understanding of the interstellar medium and dust. Progress in, and the key results of, this revolution are still difficult to predict. Nevertheless, (a) a physically justified model has been developed for the spatial distribution of absorbing material over the nearest few kiloparsecs, including the Gould belt as a dust container, which gives an accurate estimate of the extinction for any object just in terms of its galactic coordinates. It is also clear that (b) the interstellar medium makes up roughly half the mass of matter in the galactic vicinity of the solar system (the other half is made up of stars, their remnants, and dark matter) and (c) the interstellar medium and, especially, dust, differ substantially in different regions of space, and deep space cannot be understood by only studying nearby space.

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arXiv2017

On the discrepancy between asteroseismic and Gaia DR1 TGAS parallaxes

Recently, a deviation of the Gaia TGAS parallaxes from the asteroseismic ones for giants was found. We show that for parallaxes $\varpi<1.5$ mas it can be explained by a selection effect in favour of bright and luminous giants in the Tycho-2 and TGAS catalogues. Another explanation of this deviation seems to be valid for $\varpi>1.5$ mas based on the best extinction estimates: the deviation may be caused not by a bias of parallax, but by an underestimation of the extinction (and, consequently, an overestimation of the calculated absolute magnitude) in the asteroseismic results. We demonstrate that the reliable estimates of the reddening and extinction (about 0.22 mag of the visual extinction for the Kepler field) better fit both the giants and main sequence stars to the PARSEC, MIST and YaPSI isochrones.

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arXiv2016

Red Giant Clump in the Tycho-2 Catalogue

The Tycho-2 proper motions and Tycho-2 and 2MASS photometry are used to select 97348 red giant clump (RGC) stars. The interstellar extinction and photometric distance are calculated for each of the stars. The selected stars are shown to form a selection-unbiased sample of RGC stars within about 350 pc of the Sun with the addition of more distant stars. The distribution of the selected stars in space and their motion are consistent with the assumption that the RGC contains Galactic disk stars with various ages and metallicities, including a significant fraction of stars younger than 1 Gyr with masses of more than 2 $M_{\odot}$. These young stars show differences of their statistical characteristics from those of older RGC stars, including differences in the variations of their distribution density with distance from the Galactic plane and in the dispersion of their velocities found using radial velocities and proper motions. The Sun has been found to rise above the Galactic plane by $13\pm1$ pc. The distribution density of the stars under consideration in space is probably determined by the Local Spiral Arm and the distribution of absorbing matter in the plane of the Gould Belt.

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arXiv2016

Three-Dimensional Reddening Map for Stars from 2MASS Photometry: The Method and the First Results

The first results of the construction of a 3D reddening map for stars within 1600 pc of the Sun are presented. Analysis of the distribution of 70 million stars from the 2MASS catalog with the most accurate photometry on the (J-Ks) - Ks diagram supplemented with Monte Carlo simulations has shown that one of the maxima of this distribution corresponds to F-type dwarfs and subgiants with a mean absolute magnitude MKs=2.5m. The shift of this maximum toward large (J-Ks) with increasing $Ks$ reflects the reddening of these stars with increasing heliocentric distance. The distribution of the sample of stars over Ks, l, and b cells with corresponds to their distribution over 3D spatial cells. As a result, the reddening E(J-Ks) has been determined with an accuracy of 0.03m for spatial cells with a side of 100 pc. All of the known large absorbing clouds within 1600 pc of the Sun have manifested themselves in the results obtained. The distances to the near and far edges of the clouds have been determined with a relative accuracy of 15\%. The cases where unknown clouds are hidden behind known ones on the same line of sight have been found. The distance dependence of reddening is considered for various Galactic latitudes and longitudes. The absorbing matter of the Gould Belt is shown to manifest itself at latitudes up to 40 deg and within 600 pc of the Sun. The size and influence of the Gould Belt may have been underestimated thus far. The absorbing matter at latitudes up to 60 deg and within 1600 pc of the Sun has been found to be distributed predominantly in the first and second quadrants in S hemisphere and in the third and fourth quadrants in N hemisphere. A nonrandom orientation of the clouds relative to the Sun is possible. The mass of the baryonic dark matter in solar neighborhoods can then be considerably larger than is generally believed.

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arXiv2016

The Red Giant Branch in the Tycho-2 Catalogue

Based on multicolor photometry from the 2MASS and Tycho-2 catalogues, we have produced a sample of 38 368 branch red giants that has less than 1\% of admixtures and is complete within 500 pc of the Sun. The sample includes 30 671 K giants, 7544 M giants, 49 C giants, and 104 suspected supergiants or S stars. The photometric distances have been calculated for K, M, and C stars with an accuracy of 40\%. Tycho-2 proper motions and PCRV radial velocities are used to analyze the stellar kinematics. The decrease in the stellar distribution density with distance from the Galactic equator approximated by the barometric law, contrary to the Besancon model of the Galaxy, and the kinematic parameters calculated using the Ogorodnikov--Milne model characterize the overwhelming majority of the selected K and M giants as disk stars with ages of more than 3 Gyr. A small number of K and M giants are extremely young or, conversely, thick-disk ones. The latter show a nonuniform distribution in the phase space of coordinates and velocities, arguing against isothermality and full relaxation of the disk and for the theory of dynamical streams or superclusters. The spatial distribution and kinematics of the selected C stars force us to consider them as asymptotic branch giants with masses of more than 2 $M_{\odot}$ and ages of less than 2 Gyr probably associated with the Gould Belt. The offset of the Sun above the Galactic equator has been found from the distribution of stars to be $13\pm2$ pc, which coincides with the previously obtained value for the clump red giants.

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arXiv2016

Influence of the Gould Belt on Interstellar Extinction

A new analytical 3D model of interstellar extinction within 500 pc of the Sun as a function of the Galactic spherical coordinates is suggested. This model is physically more justified than the widely used Arenou model, since it takes into account the presence of absorbing matter both in the layer along the equatorial Galactic plane and in the Gould Belt. The extinction in the equatorial layer varies as the sine of the Galactic longitude and in the Gould Belt as the sine of twice the longitude in the Belt plane. The extinction across the layers varies according to a barometric law. It has been found that the absorbing layers intersect at an angle of 17 deg and that the Sun is located near the axial plane of the absorbing layer of the Gould Belt and is probably several parsecs below the axial plane of the equatorial absorbing layer but above the Galactic plane. The model has been tested using the extinction of real stars from three catalogs.

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arXiv2016

Variations of the Interstellar Extinction Law within the Nearest Kiloparsec

Multicolor photometry from the Tycho-2 and 2MASS catalogues for 11 990 OB and 30 671 K-type red giant branch stars is used to detect systematic large-scale variations of the interstellar extinction law within the nearest kiloparsec. The characteristic of the extinction law, the total-to-selective extinction ratio $R_V$, which also characterizes the size and other properties of interstellar dust grains, has been calculated for various regions of space by the extinction law extrapolation method. The results for the two classes of stars agree: the standard deviation of the "red giants minus OB" $R_V$ differences within 500 pc of the Sun is 0.2. The detected $R_V$ variations between 2.2 and 4.4 not only manifest themselves in individual clouds but also span the entire space near the Sun, following Galactic structures. In the Local Bubble within about 100 pc of the Sun, $R_V$ has a minimum. In the inner part of the Gould Belt and at high Galactic latitudes, at a distance of about 150 pc from the Sun, $R_V$ reaches a maximum and then decreases to its minimum in the outer part of the Belt and other directions at a distance of about 500 pc from the Sun, returning to its mean values far from the Sun. The detected maximum of $R_V$ at high Galactic latitudes is important when allowance is made for the interstellar extinction toward extragalactic objects. In addition, a monotonic increase in $R_V$ by 0.3 per kpc toward the Galactic center has been found near the Galactic equator. It is consistent with the result obtained by Zasowski et al. (2009) for much of the Galaxy. Ignoring the $R_V$ variations and traditionally using a single value for the entire space must lead to systematic errors in the calculated distances reaching 10\%.

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arXiv2016

3D Interstellar Extinction Map within the Nearest Kiloparsec

The product of the previously constructed 3D maps of stellar reddening (Gontcharov 2010) and $R_V$ variations (Gontcharov 2012) has allowed us to produce a 3D interstellar extinction map within the nearest kiloparsec from the Sun with a spatial resolution of 50 pc and an accuracy of $0.2^m$. This map is compared with the 2D reddening map by Schlegel et al. (1998), the 3D extinction map at high latitudes by Jones et al. (2011), and the analytical extinction models by Arenou et al. (1992) and Gontcharov (2009). In all cases, we have found good agreement and show that there are no systematic errors in the new map everywhere except the direction toward the Galactic center. We have found that the map by Schlegel et al. (1998) reaches saturation near the Galactic equator at $E_{(B-V)}>0.8^m$, has a zero-point error and systematic errors gradually increasing with reddening, and among the analytical models those that take into account the extinction in the Gould Belt are more accurate. Our extinction map shows that it is determined by reddening variations at low latitudes and $R_V$ variations at high ones. This naturally explains the contradictory data on the correlation or anticorrelation between reddening and $R_V$ available in the literature. There is a correlation in a thin layer near the Galactic equator, because both reddening and $R_V$ here increase toward the Galactic center. There is an anticorrelation outside this layer, because higher values of $R_V$ correspond to lower reddening at high and middle latitudes. Systematic differences in sizes and other properties of the dust grains in different parts of the Galaxy manifest themselves in this way. The largest structures within the nearest kiloparsec, including the Local Bubble, the Gould Belt, the Great Tunnel, the Scorpius, Perseus, Orion, and other complexes, have manifested themselves in the constructed map.

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