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A study of stellar orbit fractions: simulated IllustrisTNG galaxies compared to CALIFA observations
Xu, Dandan1,2; Zhu, Ling3; Grand, Robert4; Springel, Volker4; Mao, Shude2,5,6; van de Ven, Glenn7; Lu, Shengdong6; Wang, Yougang6; Pillepich, Annalisa8; Genel, Shy9,10; Nelson, Dylan4; Rodriguez-Gomez, Vicente11; Pakmor, Ruediger4; Weinberger, Rainer12; Marinacci, Federico13; Vogelsberger, Mark14; Torrey, Paul15; Naiman, Jill12,16; Hernquist, Lars12
2019-10-01
Source PublicationMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
ISSN0035-8711
Volume489Issue:1Pages:842-854
AbstractMotivated by the recently discovered kinematic 'Hubble sequence' shown by the stellar orbit-circularity distribution of 260 CALIFA galaxies, we make use of a comparable galaxy sample at z = 0 with a stellar mass range of M-*/M-circle dot is an element of [10(9.7), 10(11.4)] selected from the IllustrisTNG simulation and study their stellar orbit compositions in relation to a number of other fundamental galaxy properties. We find that the TNG100 simulation broadly reproduces the observed fractions of different orbital components and their stellar mass dependences. In particular, the mean mass dependences of the luminosity fractions for the kinematically warm and hot orbits are well reproduced within model uncertainties of the observed galaxies. The simulation also largely reproduces the observed peak and trough features at M-* approximate to 1-2 x 10(10) M-circle dot in the mean distributions of the cold- and hot-orbit fractions, respectively, indicating fewer cooler orbits and more hotter orbits in both more- and less-massive galaxies beyond such a mass range. Several marginal disagreements are seen between the simulation and observations: the average cold-orbit (counter-rotating) fractions of the simulated galaxies below (above) M-* approximate to 6 x 10(10) M-circle dot are systematically higher than the observational data by less than or similar to 10 per cent (absolute orbital fraction); the simulation also seems to produce more scatter for the cold-orbit fraction and less so for the non-cold orbits at any given galaxy mass. Possible causes that stem from the adopted heating mechanisms are discussed.
Keywordgalaxies: elliptical and lenticular, cD galaxies: kinematics and dynamics galaxies: spiral galaxies: stellar content galaxies: structure
Funding OrganizationDFG ; DFG ; NSFC ; NSFC ; National Key Basic Research and Development Program of China ; National Key Basic Research and Development Program of China ; Shanghai Astronomical Observatory, Chinese Academy of Sciences ; Shanghai Astronomical Observatory, Chinese Academy of Sciences ; European Research Council (ERC) under the European Union ; European Research Council (ERC) under the European Union ; Program 'Rita Levi Montalcini' of the Italian MIUR ; Program 'Rita Levi Montalcini' of the Italian MIUR ; DFG ; DFG ; NSFC ; NSFC ; National Key Basic Research and Development Program of China ; National Key Basic Research and Development Program of China ; Shanghai Astronomical Observatory, Chinese Academy of Sciences ; Shanghai Astronomical Observatory, Chinese Academy of Sciences ; European Research Council (ERC) under the European Union ; European Research Council (ERC) under the European Union ; Program 'Rita Levi Montalcini' of the Italian MIUR ; Program 'Rita Levi Montalcini' of the Italian MIUR ; DFG ; DFG ; NSFC ; NSFC ; National Key Basic Research and Development Program of China ; National Key Basic Research and Development Program of China ; Shanghai Astronomical Observatory, Chinese Academy of Sciences ; Shanghai Astronomical Observatory, Chinese Academy of Sciences ; European Research Council (ERC) under the European Union ; European Research Council (ERC) under the European Union ; Program 'Rita Levi Montalcini' of the Italian MIUR ; Program 'Rita Levi Montalcini' of the Italian MIUR ; DFG ; DFG ; NSFC ; NSFC ; National Key Basic Research and Development Program of China ; National Key Basic Research and Development Program of China ; Shanghai Astronomical Observatory, Chinese Academy of Sciences ; Shanghai Astronomical Observatory, Chinese Academy of Sciences ; European Research Council (ERC) under the European Union ; European Research Council (ERC) under the European Union ; Program 'Rita Levi Montalcini' of the Italian MIUR ; Program 'Rita Levi Montalcini' of the Italian MIUR
DOI10.1093/mnras/stz2164
WOS KeywordSTAR-FORMATION HISTORIES ; COSMOLOGICAL SIMULATIONS ; MASSIVE GALAXIES ; SPIN SWINGS ; EVOLUTION ; MODEL ; DISK ; PROJECT ; MERGERS ; MATTER
Language英语
Funding ProjectDFG[11761131004] ; NSFC[11761131004] ; NSFC[11773034] ; NSFC[11390372] ; National Key Basic Research and Development Program of China[2018YFA0404501] ; Shanghai Astronomical Observatory, Chinese Academy of Sciences[Y895201009] ; European Research Council (ERC) under the European Union[724857] ; Program 'Rita Levi Montalcini' of the Italian MIUR
Funding OrganizationDFG ; DFG ; NSFC ; NSFC ; National Key Basic Research and Development Program of China ; National Key Basic Research and Development Program of China ; Shanghai Astronomical Observatory, Chinese Academy of Sciences ; Shanghai Astronomical Observatory, Chinese Academy of Sciences ; European Research Council (ERC) under the European Union ; European Research Council (ERC) under the European Union ; Program 'Rita Levi Montalcini' of the Italian MIUR ; Program 'Rita Levi Montalcini' of the Italian MIUR ; DFG ; DFG ; NSFC ; NSFC ; National Key Basic Research and Development Program of China ; National Key Basic Research and Development Program of China ; Shanghai Astronomical Observatory, Chinese Academy of Sciences ; Shanghai Astronomical Observatory, Chinese Academy of Sciences ; European Research Council (ERC) under the European Union ; European Research Council (ERC) under the European Union ; Program 'Rita Levi Montalcini' of the Italian MIUR ; Program 'Rita Levi Montalcini' of the Italian MIUR ; DFG ; DFG ; NSFC ; NSFC ; National Key Basic Research and Development Program of China ; National Key Basic Research and Development Program of China ; Shanghai Astronomical Observatory, Chinese Academy of Sciences ; Shanghai Astronomical Observatory, Chinese Academy of Sciences ; European Research Council (ERC) under the European Union ; European Research Council (ERC) under the European Union ; Program 'Rita Levi Montalcini' of the Italian MIUR ; Program 'Rita Levi Montalcini' of the Italian MIUR ; DFG ; DFG ; NSFC ; NSFC ; National Key Basic Research and Development Program of China ; National Key Basic Research and Development Program of China ; Shanghai Astronomical Observatory, Chinese Academy of Sciences ; Shanghai Astronomical Observatory, Chinese Academy of Sciences ; European Research Council (ERC) under the European Union ; European Research Council (ERC) under the European Union ; Program 'Rita Levi Montalcini' of the Italian MIUR ; Program 'Rita Levi Montalcini' of the Italian MIUR
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000489292800062
PublisherOXFORD UNIV PRESS
Citation statistics
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/28052
Collection中国科学院国家天文台
Corresponding AuthorXu, Dandan; Zhu, Ling
Affiliation1.Tsinghua Univ, Inst Adv Studies, Beijing 100084, Peoples R China
2.Tsinghua Univ, Tsinghua Ctr Astrophys, Beijing 100084, Peoples R China
3.Chinese Acad Sci, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China
4.Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany
5.Tsinghua Univ, Dept Astron, Beijing 100084, Peoples R China
6.Chinese Acad Sci, Natl Astron Observ, 20A Datun Rd, Beijing 100101, Peoples R China
7.Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria
8.Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany
9.Flatiron Inst, Ctr Computat Astrophys, 162 Fifth Ave, New York, NY 10010 USA
10.Columbia Univ, Columbia Astrophys Lab, 550 West 120th St, New York, NY 10027 USA
11.Univ Nacl Autonoma Mexico, Inst Radioastron & Astrofis, AP 72-3, Morelia 58089, Michoacan, Mexico
12.Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA
13.Univ Bologna, Dept Phys & Astron, Via Gobetti 93-2, I-40129 Bologna, Italy
14.MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA
15.Univ Florida, Dept Phys, 2001 Museum Rd, Gainesville, FL 32611 USA
16.Univ Illinois, Sch Informat Sci, 501 E Daniel Str, Champaign, IL 61820 USA
Recommended Citation
GB/T 7714
Xu, Dandan,Zhu, Ling,Grand, Robert,et al. A study of stellar orbit fractions: simulated IllustrisTNG galaxies compared to CALIFA observations[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2019,489(1):842-854.
APA Xu, Dandan.,Zhu, Ling.,Grand, Robert.,Springel, Volker.,Mao, Shude.,...&Hernquist, Lars.(2019).A study of stellar orbit fractions: simulated IllustrisTNG galaxies compared to CALIFA observations.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,489(1),842-854.
MLA Xu, Dandan,et al."A study of stellar orbit fractions: simulated IllustrisTNG galaxies compared to CALIFA observations".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 489.1(2019):842-854.
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