Pub Date : 2023-11-28DOI: 10.1134/S1063773723060038
I. M. Khamitov, I. F. Bikmaev, M. R. Gilfanov, R. A. Sunyaev, P. S. Medvedev, M. A. Gorbachev
This paper is an extension of the study by Khamitov et al. (2022) with regard to the catalog and the astrophysical interpretation of the imitation of significant proper motions in active galactic nuclei (AGNs) and quasars based on data from the Gaia space observatory. We present a sample of SRG/eROSITA X-ray sources in the eastern Galactic hemisphere (({0^{circ}<l<180^{circ}})) having significant proper motions in the Gaia EDR3 measurements with the confirmed extragalactic nature of the objects. The catalog consists of 248 extragalactic sources with spectroscopically measured redshifts. The catalog includes all of the objects available in the SIMBAD database and coincident with the identified optical counterpart within 0.5 arcsec. Eighteen sources with spectroscopically measured redshifts from observations with the Russian–Turkish 1.5-m telescope RTT-150 (Khamitov et al. 2022) have been additionally included in the catalog. The sources in the catalog are AGNs of various types (Sy1, Sy2, LINER), quasars, radio galaxies, and star-forming galaxies. The imitation of significant proper motions can be explained (by the VIM effect previously known in astrometry) by the presence of transient events on the line of sight in the vicinity of AGNs and quasars (within the Gaia optical resolution element). Among such astrophysical events are supernova outbursts, tidal disruption events in binary AGNs, the variability of high-mass supergiants, the presence of OB associations against the background of AGNs with a variable brightness, etc. The model of outbursts with a fast rise–exponential decay profile allows the variable positional parameters of most sources observed in Gaia to be described. This approach can be used as an independent way of detecting transient events in the vicinity of AGNs (on scales of several hundred parsecs in the plane of the sky) based on data from the SRG/eROSITA catalogs of X-ray sources and the optical Gaia catalog.
本文是Khamitov等人(2022)基于盖亚空间天文台数据对活动星系核(agn)和类星体中重要固有运动模拟的目录和天体物理学解释研究的延伸。我们在银河系东半球(({0^{circ}<l<180^{circ}}))提供了一个SRG/eROSITA x射线源样本,在盖亚EDR3测量中具有显著的固有运动,并证实了物体的河外性质。该目录包括248个星系外的源,光谱测量红移。该目录包括SIMBAD数据库中可用的所有对象,并且在0.5弧秒内与已识别的光学对应物一致。俄罗斯-土耳其1.5米望远镜RTT-150 (Khamitov et al. 2022)观测到的光谱测量红移的18个源已被额外列入目录。目录中的源是各种类型的agn (Sy1, Sy2, LINER),类星体,射电星系和恒星形成星系。重要的固有运动的模仿可以通过agn和类星体(在盖亚光学分辨率元件范围内)附近视线上的瞬态事件的存在来解释(通过天体测量中先前已知的VIM效应)。这些天体物理事件包括超新星爆发、双星agn中的潮汐破坏事件、高质量超巨星的可变性、在亮度可变的agn背景下OB关联的存在等。具有快速上升-指数衰减剖面的爆发模型允许描述在盖亚观测到的大多数源的可变位置参数。基于SRG/eROSITA x射线源目录和光学Gaia目录的数据,这种方法可以作为探测agn附近瞬变事件的一种独立方法(在天空平面上的数百秒差距范围内)。
{"title":"Transient Events in the Circumnuclear Regions of AGNs and Quasars As Sources of Imitations of Proper Motions","authors":"I. M. Khamitov, I. F. Bikmaev, M. R. Gilfanov, R. A. Sunyaev, P. S. Medvedev, M. A. Gorbachev","doi":"10.1134/S1063773723060038","DOIUrl":"10.1134/S1063773723060038","url":null,"abstract":"<p>This paper is an extension of the study by Khamitov et al. (2022) with regard to the catalog and the astrophysical interpretation of the imitation of significant proper motions in active galactic nuclei (AGNs) and quasars based on data from the Gaia space observatory. We present a sample of SRG/eROSITA X-ray sources in the eastern Galactic hemisphere (<span>({0^{circ}<l<180^{circ}})</span>) having significant proper motions in the Gaia EDR3 measurements with the confirmed extragalactic nature of the objects. The catalog consists of 248 extragalactic sources with spectroscopically measured redshifts. The catalog includes all of the objects available in the SIMBAD database and coincident with the identified optical counterpart within 0.5 arcsec. Eighteen sources with spectroscopically measured redshifts from observations with the Russian–Turkish 1.5-m telescope RTT-150 (Khamitov et al. 2022) have been additionally included in the catalog. The sources in the catalog are AGNs of various types (Sy1, Sy2, LINER), quasars, radio galaxies, and star-forming galaxies. The imitation of significant proper motions can be explained (by the VIM effect previously known in astrometry) by the presence of transient events on the line of sight in the vicinity of AGNs and quasars (within the Gaia optical resolution element). Among such astrophysical events are supernova outbursts, tidal disruption events in binary AGNs, the variability of high-mass supergiants, the presence of OB associations against the background of AGNs with a variable brightness, etc. The model of outbursts with a fast rise–exponential decay profile allows the variable positional parameters of most sources observed in Gaia to be described. This approach can be used as an independent way of detecting transient events in the vicinity of AGNs (on scales of several hundred parsecs in the plane of the sky) based on data from the SRG/eROSITA catalogs of X-ray sources and the optical Gaia catalog.</p>","PeriodicalId":55443,"journal":{"name":"Astronomy Letters-A Journal of Astronomy and Space Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.9,"publicationDate":"2023-11-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138454554","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-11-28DOI: 10.1134/S1063773723060014
V. V. Bobylev, A. T. Bajkova
We have estimated the spiral pattern speed in the Galaxy (Omega_{p}) from a large sample of young open star clusters (OSCs). For this purpose, we have used 2494 OSCs younger than 50 Myr. Their mean proper motions, line-of-sight velocities, and distances were calculated by Hunt and Reffert (2023) based on data from the Gaia DR3 catalogue. Three methods have been applied to estimate (Omega_{p}). They all are based on the linear Lin–Shu spiral density wave theory. We have obtained an estimate of (Omega_{p}=24.26pm 0.52) km s({}^{-1}) kpc({}^{-1}) by the first method, which is most reliable in our view, using the velocity perturbations (f_{R}) and (f_{theta}) found through a spectral analysis of the radial, (V_{R}), and residual rotation, (Delta V_{rm circ}), velocities. Using the second method, we have found the velocity perturbations (f_{R}) and (f_{theta}) by solving the basic kinematic equations together with the Galactic rotation parameters and obtained an estimate of (Omega_{p}=23.45pm 0.53) km s({}^{-1}) kpc({}^{-1}). We have found (Omega_{p}=28.9pm 2.8) km s({}^{-1}) kpc({}^{-1}) by the third method based on an analysis of the position angles of OSCs at their birth time (theta_{rm birth}).
我们从大量年轻的疏散星团(OSCs)样本中估计了银河系$Omega_p$的螺旋模式速度。为此,我们使用了2494个小于50 Myr的osc。它们的平均固有运动、视距速度和距离是由Hunt和refert(2023)根据盖亚DR3目录的数据计算出来的。我们采用了三种方法来估算$Omega_p$。它们都是基于线性林树螺旋密度波理论。我们已经通过第一种方法获得了$Omega_p=24.26pm0.52$ km s $^{-1}$ kpc $^{-1}$的估计值,在我们看来,这是最可靠的,使用通过对径向速度$V_R$和剩余旋转速度$Delta V_{rm circ},$的光谱分析发现的速度扰动$f_R$和$f_theta$。利用第二种方法,我们通过求解基本运动学方程和银河系旋转参数,得到了速度摄动$f_R$和$f_theta$,并得到了$Omega_p= 23.45pm0.53$ km s $^{-1}$ kpc $^{-1}$的估计值。通过对osc出生时体位角度的分析,我们找到了$Omega_p= 28.9pm2.8$ km s $^{-1}$ kpc $^{-1}$$theta_{rm birth}$。
{"title":"Determination of the Spiral Pattern Speed in the Milky Way from Young Open Star Clusters","authors":"V. V. Bobylev, A. T. Bajkova","doi":"10.1134/S1063773723060014","DOIUrl":"10.1134/S1063773723060014","url":null,"abstract":"<p>We have estimated the spiral pattern speed in the Galaxy <span>(Omega_{p})</span> from a large sample of young open star clusters (OSCs). For this purpose, we have used 2494 OSCs younger than 50 Myr. Their mean proper motions, line-of-sight velocities, and distances were calculated by Hunt and Reffert (2023) based on data from the Gaia DR3 catalogue. Three methods have been applied to estimate <span>(Omega_{p})</span>. They all are based on the linear Lin–Shu spiral density wave theory. We have obtained an estimate of <span>(Omega_{p}=24.26pm 0.52)</span> km s<span>({}^{-1})</span> kpc<span>({}^{-1})</span> by the first method, which is most reliable in our view, using the velocity perturbations <span>(f_{R})</span> and <span>(f_{theta})</span> found through a spectral analysis of the radial, <span>(V_{R})</span>, and residual rotation, <span>(Delta V_{rm circ})</span>, velocities. Using the second method, we have found the velocity perturbations <span>(f_{R})</span> and <span>(f_{theta})</span> by solving the basic kinematic equations together with the Galactic rotation parameters and obtained an estimate of <span>(Omega_{p}=23.45pm 0.53)</span> km s<span>({}^{-1})</span> kpc<span>({}^{-1})</span>. We have found <span>(Omega_{p}=28.9pm 2.8)</span> km s<span>({}^{-1})</span> kpc<span>({}^{-1})</span> by the third method based on an analysis of the position angles of OSCs at their birth time <span>(theta_{rm birth})</span>.</p>","PeriodicalId":55443,"journal":{"name":"Astronomy Letters-A Journal of Astronomy and Space Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.9,"publicationDate":"2023-11-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136236929","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-11-28DOI: 10.1134/S106377372306004X
F. Melazzini, S. Sazonov
We have developed a Monte Carlo code for simulation of X-ray spectra of active galactic nuclei (AGN) based on a model of a clumpy obscuring torus. Using this code, we investigate the diagnostic power of X-ray spectroscopy of obscured AGN with respect to the physical properties and orientation of the torus, namely: the average column density, (langle N_{textrm{H}}rangle), the line-of-sight column density, (N_{textrm{H}}), the abundance of iron, (A_{textrm{Fe}}), the clumpiness (i.e., the average number of gas clouds along the line of sight), (langle Nrangle), and the viewing angle, (alpha). In this first paper of a series, we consider the Compton-thin case, where both (langle N_{textrm{H}}rangle) and (N_{textrm{H}}) do not exceed (10^{24}) cm({}^{-2}). To enable quantitative comparison of the simulated spectra, we introduce five measurable spectral characteristics: the low-energy hardness ratio (ratio of the continuum fluxes in the 7–11 and 2–7 keV energy bands), the high-energy hardness ratio (ratio of the continuum fluxes in the 10–100 and 2–10 keV energy bands), the depth of the iron K absorption edge, the equivalent width of the Fe K(alpha) line, and the fraction of the Fe K(alpha) flux contained in the Compton shoulder. We demonstrate that by means of X-ray spectroscopy it is possible to tightly constrain (langle N_{textrm{H}}rangle), (N_{textrm{H}}), and (A_{textrm{Fe}}) in the Compton-thin regime, while there is degeneracy between clumpiness and viewing direction.
{"title":"What Can We Learn about Compton-Thin AGN Tori from Their X-ray Spectra? *","authors":"F. Melazzini, S. Sazonov","doi":"10.1134/S106377372306004X","DOIUrl":"10.1134/S106377372306004X","url":null,"abstract":"<p>We have developed a Monte Carlo code for simulation of X-ray spectra of active galactic nuclei (AGN) based on a model of a clumpy obscuring torus. Using this code, we investigate the diagnostic power of X-ray spectroscopy of obscured AGN with respect to the physical properties and orientation of the torus, namely: the average column density, <span>(langle N_{textrm{H}}rangle)</span>, the line-of-sight column density, <span>(N_{textrm{H}})</span>, the abundance of iron, <span>(A_{textrm{Fe}})</span>, the clumpiness (i.e., the average number of gas clouds along the line of sight), <span>(langle Nrangle)</span>, and the viewing angle, <span>(alpha)</span>. In this first paper of a series, we consider the Compton-thin case, where both <span>(langle N_{textrm{H}}rangle)</span> and <span>(N_{textrm{H}})</span> do not exceed <span>(10^{24})</span> cm<span>({}^{-2})</span>. To enable quantitative comparison of the simulated spectra, we introduce five measurable spectral characteristics: the low-energy hardness ratio (ratio of the continuum fluxes in the 7–11 and 2–7 keV energy bands), the high-energy hardness ratio (ratio of the continuum fluxes in the 10–100 and 2–10 keV energy bands), the depth of the iron K absorption edge, the equivalent width of the Fe K<span>(alpha)</span> line, and the fraction of the Fe K<span>(alpha)</span> flux contained in the Compton shoulder. We demonstrate that by means of X-ray spectroscopy it is possible to tightly constrain <span>(langle N_{textrm{H}}rangle)</span>, <span>(N_{textrm{H}})</span>, and <span>(A_{textrm{Fe}})</span> in the Compton-thin regime, while there is degeneracy between clumpiness and viewing direction.</p>","PeriodicalId":55443,"journal":{"name":"Astronomy Letters-A Journal of Astronomy and Space Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.9,"publicationDate":"2023-11-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138454535","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-11-28DOI: 10.1134/S1063773723060051
A. S. Tsvetkov, F. A. Amosov
We have solved the Ogorodnikov–Milne stellar-kinematics equations in the Galactic rectangular coordinate system based on the total velocities for a special sample of stars with radial velocities from the final Gaia Data Release 3 catalogue. We have found the region of applicability of the linear model and the regions that it describes poorly. We have constructed a second-order model that takes into account the peculiarities of stellar kinematics more accurately and showed its applicability for stars at distances up to 5 kpc.
{"title":"Determination of the Parameters of a Nonlinear Kinematic Galactic Rotation Model Based on the Proper Motions and Radial Velocities of Stars from the Gaia DR3 Catalogue","authors":"A. S. Tsvetkov, F. A. Amosov","doi":"10.1134/S1063773723060051","DOIUrl":"10.1134/S1063773723060051","url":null,"abstract":"<p>We have solved the Ogorodnikov–Milne stellar-kinematics equations in the Galactic rectangular coordinate system based on the total velocities for a special sample of stars with radial velocities from the final Gaia Data Release 3 catalogue. We have found the region of applicability of the linear model and the regions that it describes poorly. We have constructed a second-order model that takes into account the peculiarities of stellar kinematics more accurately and showed its applicability for stars at distances up to 5 kpc.</p>","PeriodicalId":55443,"journal":{"name":"Astronomy Letters-A Journal of Astronomy and Space Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.9,"publicationDate":"2023-11-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138454563","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-11-28DOI: 10.1134/S1063773723060026
T. V. Demidova, I. I. Shevchenko
Ways of formation of azimuthal resonant patterns in circumstellar planetesimal disks with planets are considered. Our analytical estimates and massive numerical experiments show that the disk particles that initially reside in zones of low-order mean-motion resonances with the planet may eventually concentrate into potentially observable azimuthal patterns. The structuring process is rapid, usually taking (sim)100 orbital periods of the planet. It is found that the relative number of particles that retain their resonant position increases with decreasing the mass parameter (mu) (the ratio of masses of the perturbing planet and the parent star), but a significant fraction of the particle population is always removed from the disk due to accretion of the particles onto the star and planet, as well as due to their transition to highly elongated and hyperbolic orbits. Expected radio images of azimuthally structured disks are constructed. In the considered models, azimuthal patterns associated with the (2:1) and (3:2) resonances are most clearly manifested; observational manifestations of the (1:2) and (2:3) resonances are also possible.
{"title":"Azimuthal Patterns in Planetesimal Circumstellar Disks","authors":"T. V. Demidova, I. I. Shevchenko","doi":"10.1134/S1063773723060026","DOIUrl":"10.1134/S1063773723060026","url":null,"abstract":"<p>Ways of formation of azimuthal resonant patterns in circumstellar planetesimal disks with planets are considered. Our analytical estimates and massive numerical experiments show that the disk particles that initially reside in zones of low-order mean-motion resonances with the planet may eventually concentrate into potentially observable azimuthal patterns. The structuring process is rapid, usually taking <span>(sim)</span>100 orbital periods of the planet. It is found that the relative number of particles that retain their resonant position increases with decreasing the mass parameter <span>(mu)</span> (the ratio of masses of the perturbing planet and the parent star), but a significant fraction of the particle population is always removed from the disk due to accretion of the particles onto the star and planet, as well as due to their transition to highly elongated and hyperbolic orbits. Expected radio images of azimuthally structured disks are constructed. In the considered models, azimuthal patterns associated with the <span>(2:1)</span> and <span>(3:2)</span> resonances are most clearly manifested; observational manifestations of the <span>(1:2)</span> and <span>(2:3)</span> resonances are also possible.</p>","PeriodicalId":55443,"journal":{"name":"Astronomy Letters-A Journal of Astronomy and Space Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.9,"publicationDate":"2023-11-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138454562","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-11-25DOI: 10.1134/S1063773723070022
A. V. Meshcheryakov, V. D. Borisov, G. A. Khorunzhev, P. A. Medvedev, M. R. Gilfanov, M. I. Belvedersky, S. Yu. Sazonov, R. A. Burenin, R. A. Krivonos, I. F. Bikmaev, I. M. Khamitov, S. V. Gerasimov, I. V. Mashechkin, R. A. Sunyaev
We describe the methods of the SRGz system for the physical identification of eROSITA point X-ray sources from photometric data in the DESI Legacy Imaging Surveys footprint. We consider the models included in the SRGz system (version 2.1) that have allowed us to obtain accurate measurements of the cosmological redshift and class of an X-ray object (quasar/galaxy/star) from multiwavelength photometric sky surveys (DESI LIS, SDSS, Pan-STARRS, WISE, eROSITA) for 87({%}) of the entire eastern extragalactic region ((0^{circ}<l<180^{circ}), (|b|>20^{circ})). An important feature of the SRGz system is that its data handling model (identification, classification, photo-z algorithms) is based entirely on heuristic machine learning approaches. For a standard choice of SRGz parameters the optical counterpart identification completeness (recall) in the DESI LIS footprint is (95{%}) (with an optical counterpart selection precision of (94{%})); the classification completeness (recall) of X-ray sources without optical counterparts in DESI LIS is (82{%}) ((85{%}) precision). A high quality of the photometric classification of X-ray source optical counterparts is achieved in SRGz: ({>}99{%}) photometric classification completeness (recall) for extragalactic objects (a quasar or a galaxy) and stars on a test sample of sources with SDSS spectra and GAIA astrometric stars. We present an analysis of the importance of various photometric features for the optical identification and classification of eROSITA X-ray sources. We have shown that the infrared (IR) magnitude (W_{2}), the X-ray/optical(IR) ratios, the optical colors (for example, ((g-r))), and the IR color ((W_{1}-W_{2})) as well as the color distances introduced by us play a significant role in separating the classes of X-ray objects. We use the most important photometric features to interpret the SRGz predictions in this paper. The accuracy of the SRGz photometric redshifts (from DESI LIS, SDSS, Pan-STARRS, and WISE photometric data) has been tested in the Stripe82X field on a sample of 3/4 of the optical counterparts of eROSITA point X-ray sources (for which spectroscopic measurements are available in Stripe82X): (sigma_{NMAD}=3.1{%}) (the normalized median absolute deviation of the prediction) and (n_{>0.15}=7.8{%}) (the fraction of catastrophic outliers). The presented photo-z results for eROSITA X-ray sources in the Stripe82X field are more than a factor of 2 better in both metrics ((sigma_{NMAD}) and (n_{>0.15})) than the photo-z results of other groups published in the Stripe82X catalog.
{"title":"SRGz: Machine Learning Methods and Properties of the Catalog of SRG/eROSITA Point X-ray Source Optical Counterparts in the DESI Legacy Imaging Surveys Footprint","authors":"A. V. Meshcheryakov, V. D. Borisov, G. A. Khorunzhev, P. A. Medvedev, M. R. Gilfanov, M. I. Belvedersky, S. Yu. Sazonov, R. A. Burenin, R. A. Krivonos, I. F. Bikmaev, I. M. Khamitov, S. V. Gerasimov, I. V. Mashechkin, R. A. Sunyaev","doi":"10.1134/S1063773723070022","DOIUrl":"10.1134/S1063773723070022","url":null,"abstract":"<p>We describe the methods of the SRGz system for the physical identification of eROSITA point X-ray sources from photometric data in the DESI Legacy Imaging Surveys footprint. We consider the models included in the SRGz system (version 2.1) that have allowed us to obtain accurate measurements of the cosmological redshift and class of an X-ray object (quasar/galaxy/star) from multiwavelength photometric sky surveys (DESI LIS, SDSS, Pan-STARRS, WISE, eROSITA) for 87<span>({%})</span> of the entire eastern extragalactic region (<span>(0^{circ}<l<180^{circ})</span>, <span>(|b|>20^{circ})</span>). An important feature of the SRGz system is that its data handling model (identification, classification, photo-z algorithms) is based entirely on heuristic machine learning approaches. For a standard choice of SRGz parameters the optical counterpart identification completeness (recall) in the DESI LIS footprint is <span>(95{%})</span> (with an optical counterpart selection precision of <span>(94{%})</span>); the classification completeness (recall) of X-ray sources without optical counterparts in DESI LIS is <span>(82{%})</span> (<span>(85{%})</span> precision). A high quality of the photometric classification of X-ray source optical counterparts is achieved in SRGz: <span>({>}99{%})</span> photometric classification completeness (recall) for extragalactic objects (a quasar or a galaxy) and stars on a test sample of sources with SDSS spectra and GAIA astrometric stars. We present an analysis of the importance of various photometric features for the optical identification and classification of eROSITA X-ray sources. We have shown that the infrared (IR) magnitude <span>(W_{2})</span>, the X-ray/optical(IR) ratios, the optical colors (for example, <span>((g-r))</span>), and the IR color (<span>(W_{1}-W_{2})</span>) as well as the color distances introduced by us play a significant role in separating the classes of X-ray objects. We use the most important photometric features to interpret the SRGz predictions in this paper. The accuracy of the SRGz photometric redshifts (from DESI LIS, SDSS, Pan-STARRS, and WISE photometric data) has been tested in the Stripe82X field on a sample of 3/4 of the optical counterparts of eROSITA point X-ray sources (for which spectroscopic measurements are available in Stripe82X): <span>(sigma_{NMAD}=3.1{%})</span> (the normalized median absolute deviation of the prediction) and <span>(n_{>0.15}=7.8{%})</span> (the fraction of catastrophic outliers). The presented photo-z results for eROSITA X-ray sources in the Stripe82X field are more than a factor of 2 better in both metrics (<span>(sigma_{NMAD})</span> and <span>(n_{>0.15})</span>) than the photo-z results of other groups published in the Stripe82X catalog.</p>","PeriodicalId":55443,"journal":{"name":"Astronomy Letters-A Journal of Astronomy and Space Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.9,"publicationDate":"2023-11-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138438414","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-11-25DOI: 10.1134/S1063773723070034
Yu. A. Nagovitsyn, A. A. Osipova
The extreme levels of solar activity on time scales of 300–400 and 9000 years are considered. The total sunspot area (AR), a physical index of solar activity, has been estimated using the sunspot number reconstruction from Wu et al. (2018). The main study has been carried out precisely in terms of this index. The variations in solar activity at the epoch of the last 300–400 years represent fairly well its variations on time scales of the order of nine millennia. The maximum level of solar activity for the yearly averages is (AR_{M}=2930pm 400) m.s.h. (millionths of the solar hemisphere). The upper limit for the daily values is (AR_{M}=7500pm 2200) m.s.h. for the traditional sunspot areas corrected for the perspective distortion and (AR_{OM}=11,400pm 3300) m.s.d. (millionths of the solar disk) for the so-called ‘‘observed’’ areas—the sunspot projections onto the visible solar disk. The maximum yearly averages of the sunspot number (SN_{M}=258pm 38) and the sunspot group number (GN_{M}=12.3pm 2.4) have also been estimated; 11.3({%}) of the time the solar activity is at an extremely high level; 8.5 and 4.5({%}) of the time its level corresponds to the Dalton minimum or lower and an extremely low one, respectively. Thus, extremely high levels are more likely for solar activity than extremely low ones.
{"title":"Extreme Values of Sunspot Activity on a Long Time Scale","authors":"Yu. A. Nagovitsyn, A. A. Osipova","doi":"10.1134/S1063773723070034","DOIUrl":"10.1134/S1063773723070034","url":null,"abstract":"<p>The extreme levels of solar activity on time scales of 300–400 and 9000 years are considered. The total sunspot area <span>(AR)</span>, a physical index of solar activity, has been estimated using the sunspot number reconstruction from Wu et al. (2018). The main study has been carried out precisely in terms of this index. The variations in solar activity at the epoch of the last 300–400 years represent fairly well its variations on time scales of the order of nine millennia. The maximum level of solar activity for the yearly averages is <span>(AR_{M}=2930pm 400)</span> m.s.h. (millionths of the solar hemisphere). The upper limit for the daily values is <span>(AR_{M}=7500pm 2200)</span> m.s.h. for the traditional sunspot areas corrected for the perspective distortion and <span>(AR_{OM}=11,400pm 3300)</span> m.s.d. (millionths of the solar disk) for the so-called ‘‘observed’’ areas—the sunspot projections onto the visible solar disk. The maximum yearly averages of the sunspot number <span>(SN_{M}=258pm 38)</span> and the sunspot group number <span>(GN_{M}=12.3pm 2.4)</span> have also been estimated; 11.3<span>({%})</span> of the time the solar activity is at an extremely high level; 8.5 and 4.5<span>({%})</span> of the time its level corresponds to the Dalton minimum or lower and an extremely low one, respectively. Thus, extremely high levels are more likely for solar activity than extremely low ones.</p>","PeriodicalId":55443,"journal":{"name":"Astronomy Letters-A Journal of Astronomy and Space Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.9,"publicationDate":"2023-11-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138438367","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-11-25DOI: 10.1134/S1063773723070010
V. V. Bobylev, A. T. Bajkova
We have studied the kinematics of a unique sample of young open star clusters (OSCs) with high vertical velocities, (15<W<40) km s({}^{-1}). The characteristics of these clusters were taken from the catalogue by Hunt and Reffert (2023), where their mean proper motions, line-of-sight velocities, and distances were calculated using Gaia DR3 data. These OSCs are located within 0.6 kpc of the Sun and form two clumps: one in the region of the Sco–Cen OB association and the other one in the region of the Per OB3–Per OB2 associations. The OSC group of 47 members in the region of the Sco–Cen association is shown to expand along the (y) axis, (partial V/partial y=51pm 12) km s({}^{-1}) kpc({}^{-1}). This group also has a positive rotation around the (z) axis with an angular velocity of (71pm 11) km s({}^{-1}) kpc({}^{-1}) and a negative rotation around the (x) axis with an angular velocity of (-35pm 5) km s({}^{-1}) kpc({}^{-1}). Based on the velocities of 27 OSCs from the region of the Per OB3–Per OB2 associations, we have found no gradients differing significantly from zero. We have studied the kinematics of more than 1700 stars selected by Luhman (2022) as probable members of the Sco–Cen OB association. These stars are shown to have no high vertical velocities. The expansion coefficient of the stellar system in the (xy) plane has been found from all stars to be (K_{xy}=43.2pm 2.2) km s({}^{-1}) kpc({}^{-1}). Based on stars from the three UCL, LCC, and V1062 Sco groups with a mean age ({sim}20) Myr, for the first time we have found a volume expansion coefficient of the stellar system differing significantly from zero, (K_{xyz}=43.2pm 3.4) km s({}^{-1}) kpc({}^{-1}).
我们研究了一个独特的年轻疏散星团(OSCs)样本的运动学,它具有高垂直速度,$15
{"title":"Peculiarities of Open Star Clusters with High Vertical Velocities from the Region of the Sco–Cen OB Association","authors":"V. V. Bobylev, A. T. Bajkova","doi":"10.1134/S1063773723070010","DOIUrl":"10.1134/S1063773723070010","url":null,"abstract":"<p>We have studied the kinematics of a unique sample of young open star clusters (OSCs) with high vertical velocities, <span>(15<W<40)</span> km s<span>({}^{-1})</span>. The characteristics of these clusters were taken from the catalogue by Hunt and Reffert (2023), where their mean proper motions, line-of-sight velocities, and distances were calculated using Gaia DR3 data. These OSCs are located within 0.6 kpc of the Sun and form two clumps: one in the region of the Sco–Cen OB association and the other one in the region of the Per OB3–Per OB2 associations. The OSC group of 47 members in the region of the Sco–Cen association is shown to expand along the <span>(y)</span> axis, <span>(partial V/partial y=51pm 12)</span> km s<span>({}^{-1})</span> kpc<span>({}^{-1})</span>. This group also has a positive rotation around the <span>(z)</span> axis with an angular velocity of <span>(71pm 11)</span> km s<span>({}^{-1})</span> kpc<span>({}^{-1})</span> and a negative rotation around the <span>(x)</span> axis with an angular velocity of <span>(-35pm 5)</span> km s<span>({}^{-1})</span> kpc<span>({}^{-1})</span>. Based on the velocities of 27 OSCs from the region of the Per OB3–Per OB2 associations, we have found no gradients differing significantly from zero. We have studied the kinematics of more than 1700 stars selected by Luhman (2022) as probable members of the Sco–Cen OB association. These stars are shown to have no high vertical velocities. The expansion coefficient of the stellar system in the <span>(xy)</span> plane has been found from all stars to be <span>(K_{xy}=43.2pm 2.2)</span> km s<span>({}^{-1})</span> kpc<span>({}^{-1})</span>. Based on stars from the three UCL, LCC, and V1062 Sco groups with a mean age <span>({sim}20)</span> Myr, for the first time we have found a volume expansion coefficient of the stellar system differing significantly from zero, <span>(K_{xyz}=43.2pm 3.4)</span> km s<span>({}^{-1})</span> kpc<span>({}^{-1})</span>.</p>","PeriodicalId":55443,"journal":{"name":"Astronomy Letters-A Journal of Astronomy and Space Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.9,"publicationDate":"2023-11-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136104888","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-10-03DOI: 10.1134/S1063773723050067
L. S. Ugol’kova, M. S. Pshirkov, V. P. Goranskij, N. P. Ikonnikova, B. S. Safonov, A. M. Tatarnikov, E. V. Shimanovskaya, M. A. Burlak, M. D. Afonina
The source BL Lac exhibited an enhanced activity from August 2020 to July 2022. This activity peaked in July–August 2021. In this period the source reached historic brightness maxima in various energy ranges. Observations of this nonstandard maximum were carried out by the SAI staff of the Crimean Station of SAI and with the telescopes of the Caucasus Mountain Observatory (CMO SAI MSU). Optical and near-infrared photometric data as well as optical polarimetric data were obtained. When investigating the correlation between the optical and gamma-ray fluxes and between the optical and infrared fluxes, its high degree with an almost zero lag was confirmed—this means that the emission regions spatially coincide or are very close together. The degree of linear polarization in the investigated period changed in a wide range, reaching 20({%}), with an anticorrelation between the degree of linear polarization and the brightness of the object having been observed. A similar pattern of variation was also observed in the preceding flares of this object. The changes in the electric vector position angle (EVPA) show a dependence on the rate of change of the object’s brightness. The EVPA changed greatly during flares and slowly at the times of a slow change in the intensity.
来源BL Lac在2020年8月至2022年7月期间表现出增强的活性。这一活动在2021年7月至8月达到峰值。在这一时期,光源在不同的能量范围内达到了历史亮度最大值。这一非标准最大值的观测是由SAI克里米亚站的SAI工作人员和高加索山天文台(CMO SAI MSU)的望远镜进行的。获得了光学和近红外光度数据以及光学偏振数据。在研究光学和伽马射线通量之间以及光学和红外通量之间的相关性时,证实了其几乎为零滞后的高度——这意味着发射区域在空间上重合或非常接近。在研究期间,线偏振度变化范围很广,达到20({%}),观察到线偏振度与物体亮度之间存在反相关性。在该天体之前的耀斑中也观察到了类似的变化模式。电矢量位置角(EVPA)的变化显示出对物体亮度变化率的依赖性。EVPA在耀斑期间变化很大,在强度缓慢变化时变化缓慢。
{"title":"Investigation of the Flaring Activity of BL Lac in July–November 2021","authors":"L. S. Ugol’kova, M. S. Pshirkov, V. P. Goranskij, N. P. Ikonnikova, B. S. Safonov, A. M. Tatarnikov, E. V. Shimanovskaya, M. A. Burlak, M. D. Afonina","doi":"10.1134/S1063773723050067","DOIUrl":"10.1134/S1063773723050067","url":null,"abstract":"<p>The source BL Lac exhibited an enhanced activity from August 2020 to July 2022. This activity peaked in July–August 2021. In this period the source reached historic brightness maxima in various energy ranges. Observations of this nonstandard maximum were carried out by the SAI staff of the Crimean Station of SAI and with the telescopes of the Caucasus Mountain Observatory (CMO SAI MSU). Optical and near-infrared photometric data as well as optical polarimetric data were obtained. When investigating the correlation between the optical and gamma-ray fluxes and between the optical and infrared fluxes, its high degree with an almost zero lag was confirmed—this means that the emission regions spatially coincide or are very close together. The degree of linear polarization in the investigated period changed in a wide range, reaching 20<span>({%})</span>, with an anticorrelation between the degree of linear polarization and the brightness of the object having been observed. A similar pattern of variation was also observed in the preceding flares of this object. The changes in the electric vector position angle (EVPA) show a dependence on the rate of change of the object’s brightness. The EVPA changed greatly during flares and slowly at the times of a slow change in the intensity.</p>","PeriodicalId":55443,"journal":{"name":"Astronomy Letters-A Journal of Astronomy and Space Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.9,"publicationDate":"2023-10-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"50447187","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-10-03DOI: 10.1134/S1063773723050043
O. K. Sil’chenko, A. V. Moiseev, D. V. Oparin, D. V. Zlydneva, D. V. Kozlova
Using long-slit and panoramic spectroscopy at the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences and by mapping emission lines in a narrow passband of 13 Å with the MaNGaL instrument at the 2.5-m telescope of the Caucasus Mountain Observatory of the Sternberg Astronomical Institute of the Lomonosov Moscow State University, we have investigated the gaseous component of the giant lenticular galaxy NGC 934. The gas kinematics in the galaxy has turned out to disagree completely with the stellar kinematics, suggesting recent accretion of a large amount of cold gas by the galaxy. Weak star formation proceeds in the accreted gas on the periphery of the galaxy, mainly in a ring of radius 26 kpc, which may promise the buildup of a giant low-surface-brightness stellar disk in this early-type galaxy. The gas metallicity in the star formation ring is nearly solar: the accretion source is most likely the swallowing of a massive gas-rich satellite.
{"title":"Counter-Rotating Gaseous Disk and Star Formation in the S0 Galaxy NGC 934","authors":"O. K. Sil’chenko, A. V. Moiseev, D. V. Oparin, D. V. Zlydneva, D. V. Kozlova","doi":"10.1134/S1063773723050043","DOIUrl":"10.1134/S1063773723050043","url":null,"abstract":"<p>Using long-slit and panoramic spectroscopy at the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences and by mapping emission lines in a narrow passband of 13 Å with the MaNGaL instrument at the 2.5-m telescope of the Caucasus Mountain Observatory of the Sternberg Astronomical Institute of the Lomonosov Moscow State University, we have investigated the gaseous component of the giant lenticular galaxy NGC 934. The gas kinematics in the galaxy has turned out to disagree completely with the stellar kinematics, suggesting recent accretion of a large amount of cold gas by the galaxy. Weak star formation proceeds in the accreted gas on the periphery of the galaxy, mainly in a ring of radius 26 kpc, which may promise the buildup of a giant low-surface-brightness stellar disk in this early-type galaxy. The gas metallicity in the star formation ring is nearly solar: the accretion source is most likely the swallowing of a massive gas-rich satellite.</p>","PeriodicalId":55443,"journal":{"name":"Astronomy Letters-A Journal of Astronomy and Space Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.9,"publicationDate":"2023-10-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"50447188","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}