The distribution of stars around the Milky Way's central black hole III. Comparison with simulations

doi:10.1051/0004-6361/201730462

	The distribution of stars around the Milky Way's central black hole III. Comparison with simulations
	Baumgardt, H.1; Amaro-Seoane, P.2,3,4,5,6; Schodel, R.7
刊名	ASTRONOMY & ASTROPHYSICS
	2018
卷号	609 页码:6
关键词	methods: numerical Hertzsprung-Russell and C-M diagrams stars: kinematics and dynamics Galaxy: centre Galaxy: nucleus
ISSN号	1432-0746
DOI	10.1051/0004-6361/201730462
英文摘要	Context. The distribution of stars around a massive black hole (MBH) has been addressed in stellar dynamics for the last four decades by a number of authors. Because of its proximity, the centre of the Milky Way is the only observational test case where the stellar distribution can be accurately tested. Past observational work indicated that the brightest giants in the Galactic centre (GC) may show a density deficit around the central black hole, not a cusp-like distribution, while we theoretically expect the presence of a stellar cusp. Aims. We here present a solution to this long-standing problem. Methods. We performed direct-summation N-body simulations of star clusters around massive black holes and compared the results of our simulations with new observational data of the GC's nuclear cluster. Results. We find that after a Hubble time, the distribution of bright stars as well as the diffuse light follow power-law distributions in projection with slopes of approximate to 0.3 in our simulations. This is in excellent agreement with what is seen in star counts and in the distribution of the diffuse stellar light extracted from adaptive-optics (AO) assisted near-infrared observations of the GC. Conclusions. Our simulations also confirm that there exists a missing giant star population within a projected radius of a few arcsec around Sgr A*. Such a depletion of giant stars in the innermost 0.1 pc could be explained by a previously present gaseous disc and collisions, which means that a stellar cusp would also be present at the innermost radii, but in the form of degenerate compact cores.
资助项目	European Research Council under the European Union's Seventh Framework Programme/ERC[614922] ; Ramon y Cajal Programme of the Ministry of Economy, Industry and Competitiveness of Spain ; CAS President's International Fellowship Initiative
WOS研究方向	Astronomy & Astrophysics
语种	英语
出版者	EDP SCIENCES S A
WOS记录号	WOS:000418963900028
内容类型	期刊论文
源URL	[http://ir.amss.ac.cn/handle/2S8OKBNM/26974]
专题	中国科学院数学与系统科学研究院
通讯作者	Baumgardt, H.
作者单位	1.Univ Queensland, Sch Math & Phys, St Lucia, Qld 4072, Australia 2.CSIC, ICE, Inst Space Sci, Campus UAB,Carrer Can Magrans S-N, Barcelona 08193, Spain 3.IEEC, Campus UAB,Carrer Can Magrans S-N, Barcelona 08193, Spain 4.Chinese Acad Sci, Acad Math & Syst Sci, Inst Appl Math, Beijing 100190, Peoples R China 5.Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China 6.TU Berlin, Zentrum Astron & Astrophys, Hardenbergstr 36, D-10623 Berlin, Germany 7.Inst Astrofis Andalucia, Glorieta Astron S-N, E-18080 Granada, Spain
推荐引用方式 GB/T 7714	Baumgardt, H.,Amaro-Seoane, P.,Schodel, R.. The distribution of stars around the Milky Way's central black hole III. Comparison with simulations[J]. ASTRONOMY & ASTROPHYSICS,2018,609:6.
APA	Baumgardt, H.,Amaro-Seoane, P.,&Schodel, R..(2018).The distribution of stars around the Milky Way's central black hole III. Comparison with simulations.ASTRONOMY & ASTROPHYSICS,609,6.
MLA	Baumgardt, H.,et al."The distribution of stars around the Milky Way's central black hole III. Comparison with simulations".ASTRONOMY & ASTROPHYSICS 609(2018):6.