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Abstract <p>Using integral field spectroscopic data from the Mapping Nearby Galaxies at Apache Point Observatory survey for three galaxies: SDSS J074834.64<InlineEquation ID="IEq1"> <EquationSource Format="TEX">\(+\)</EquationSource> <!--BPhysMGU2570112Goradzhanov-m1--> </InlineEquation>444117.8, SDSS J113356.96<InlineEquation ID="IEq2"> <EquationSource Format="TEX">\(+\)</EquationSource> <!--BPhysMGU2570112Goradzhanov-m2--> </InlineEquation>511459.2, and SDSS J105252.58<InlineEquation ID="IEq3"> <EquationSource Format="TEX">\(+\)</EquationSource> <!--BPhysMGU2570112Goradzhanov-m3--> </InlineEquation>432542.2, we studied the kinematics of three galaxies with inconsistent kinematics. By dividing the results of dynamical modeling into subsystems by the circularity parameter <InlineEquation ID="IEq4"> <EquationSource Format="TEX">\(\lambda_{z}\)</EquationSource> <!--BPhysMGU2570112Goradzhanov-m4--> </InlineEquation>, which we performed using two methods—the Jeans and Schwarzschild orbit-based methods, we confirmed the presence of inconsistent kinematics in all three galaxies. All of them have a counter-rotating stellar disk comparable in mass to the main disk. In the future, we will perform a population-dynamical analysis of the populations of each of the dynamical subsystems.</p>

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Dynamical Modeling of Galaxies with Inconsistent Kinematics

  • 期刊论文

  • 发表日期：

    2025年12月1日

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  • V. S. Goradzhanov,
  • D. D. Mishurin

摘要

Abstract

Using integral field spectroscopic data from the Mapping Nearby Galaxies at Apache Point Observatory survey for three galaxies: SDSS J074834.64 \(+\) 444117.8, SDSS J113356.96 \(+\) 511459.2, and SDSS J105252.58 \(+\) 432542.2, we studied the kinematics of three galaxies with inconsistent kinematics. By dividing the results of dynamical modeling into subsystems by the circularity parameter \(\lambda_{z}\) , which we performed using two methods—the Jeans and Schwarzschild orbit-based methods, we confirmed the presence of inconsistent kinematics in all three galaxies. All of them have a counter-rotating stellar disk comparable in mass to the main disk. In the future, we will perform a population-dynamical analysis of the populations of each of the dynamical subsystems.