Chemo-dynamical modelling with Schwarzschild's method  

作　　者：Richard John Long Shude Mao 

机构地区：[1]National Astronomical Observatories, Chinese Academy of Sciences [2]Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester [3]Physics Department and Tsinghua Centre for Astrophysics, Tsinghua University

出　　处：《Research in Astronomy and Astrophysics》2018年第12期1-8,共8页天文和天体物理学研究（英文版）

基　　金：partly supported by the National Key Basic Research and Development Program of China (No.2018YFA0404501 to SM);by the National Natural Science Foundation of China (Grant Nos.11333003, 11390372 and 11761131004 to SM)

摘　　要：We extend Schwarzschild’s dynamical modelling method to model absorption line strength data as well as the more usual luminosity and kinematic data.Our approach draws on earlier published work by the first author with the Syer & Tremaine made-to-measure(M2M) dynamical modelling method and uses similar ideas to create a chemo-Schwarzschild method.We apply our extended Schwarzschild method to the same four early type galaxies(NGC 1248, NGC 3838, NGC 4452,NGC 4551) as the chemo-M2M work, and are able to recover successfully the 2D absorption line strength for the three lines we model(Hβ, Fe5015, Mg b).We believe that this is the first time Schwarzschild’s method has been used in this way.The techniques developed can be applied to modelling other aspects of galaxies, for example age and metallicity data coming from stellar population modelling, and are not specific to absorption line strength data.We extend Schwarzschild's dynamical modelling method to model absorption line strength data as well as the more usual luminosity and kinematic data.Our approach draws on earlier published work by the first author with the Syer & Tremaine made-to-measure(M2M) dynamical modelling method and uses similar ideas to create a chemo-Schwarzschild method.We apply our extended Schwarzschild method to the same four early type galaxies(NGC 1248, NGC 3838, NGC 4452,NGC 4551) as the chemo-M2M work, and are able to recover successfully the 2D absorption line strength for the three lines we model(Hβ, Fe5015, Mg b).We believe that this is the first time Schwarzschild's method has been used in this way.The techniques developed can be applied to modelling other aspects of galaxies, for example age and metallicity data coming from stellar population modelling, and are not specific to absorption line strength data.

关 键 词：galaxies:abundances galaxies:formation galaxies:individual(NGC 1248 NGC 3838 NGC 4452 NGC 4551) galaxies:kinematics and dynamics galaxies:structure methods:numerical 

分 类 号：P[天文地球]