Detection of the Schwarzschild precession in the orbit of the star S2 near the Galactic centre massive black hole

被引：435

作者：

Abuter, R. ^{[8
]}

Amorim, A. ^{[6
,13
]}

Bauboeck, M. ^{[1
]}

Berger, J. P. ^{[5
,8
]}

Bonnet, H. ^{[8
]}

Brandner, W. ^{[3
]}

Cardoso, V ^{[13
,15
]}

Clenet, Y. ^{[2
]}

de Zeeuw, P. T. ^{[1
,11
]}

Dexter, J. ^{[1
,14
]}

Eckart, A. ^{[4
,10
]}

Eisenhauer, F. ^{[1
]}

Schreiber, N. M. Foerster ^{[1
]}

Garcia, P. ^{[7
,13
]}

Gao, F. ^{[1
]}

Gendron, E. ^{[2
]}

Genzel, R. ^{[1
,12
]}

Gillessen, S. ^{[1
]}

Habibi, M. ^{[1
]}

Haubois, X. ^{[9
]}

Henning, T. ^{[3
]}

Hippler, S. ^{[3
]}

Horrobin, M. ^{[4
]}

Jimenez-Rosales, A. ^{[1
]}

Jochum, L. ^{[9
]}

Jocou, L. ^{[5
]}

Kaufer, A. ^{[9
]}

Kervella, P. ^{[2
]}

Lacour, S. ^{[2
]}

Lapeyrere, V ^{[2
]}

Le Bouquin, J-B ^{[5
]}

Lena, P. ^{[2
]}

Nowak, M. ^{[2
,17
]}

Ott, T. ^{[1
]}

Paumard, T. ^{[2
]}

Perraut, K. ^{[5
]}

Perrin, G. ^{[2
]}

Pfuhl, O. ^{[1
,8
]}

Rodriguez-Coira, G. ^{[2
]}

Shangguan, J. ^{[1
]}

Scheithauer, S. ^{[3
]}

Stadler, J. ^{[1
]}

Straub, O. ^{[1
]}

Straubmeier, C. ^{[4
]}

Sturm, E. ^{[1
]}

Tacconi, L. J. ^{[1
]}

Vincent, F. ^{[2
]}

von Fellenberg, S. ^{[1
]}

Waisberg, I ^{[1
,16
]}

Widmann, F. ^{[1
]}

机构：

[1] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany

[2] Univ Paris, Sorbonne Univ, Univ PSL, LESIA,Observ Paris,CNRS, 5 Pl Jules Janssen, F-92195 Meudon, France

[3] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[4] Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany

[5] Univ Grenoble Alpes, IPAG, CNRS, F-38000 Grenoble, France

[6] Univ Lisbon, Fac Ciencias, P-1749016 Lisbon, Portugal

[7] Univ Porto, Fac Engn, Rua Dr Roberto Frias, P-4200465 Porto, Portugal

[8] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany

[9] European Southern Observ, Casilla 19001, Santiago 19, Chile

[10] Max Planck Inst Radio Astron, Hugel 69, D-53121 Bonn, Germany

[11] Leiden Univ, Sterrewacht Leiden, Postbus 9513, NL-2300 RA Leiden, Netherlands

[12] Univ Calif Berkeley, Dept Phys & Astron, Le Conte Hall, Berkeley, CA 94720 USA

[13] Univ Lisbon, IST, CENTRA Ctr Astrofis & Gravitacao, P-1049001 Lisbon, Portugal

[14] Univ Colorado, JILA, Dept Astrophys & Planetary Sci, Duane Phys Bldg,2000 Colorado Ave, Boulder, CO 80309 USA

[15] CERN, 1 Espl Particules, CH-1211 Geneva 23, Switzerland

[16] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel

[17] Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

来源：

ASTRONOMY & ASTROPHYSICS | 2020年 / 636卷

基金：

欧洲研究理事会;

关键词：

black hole physics; Galaxy: nucleus; gravitation; relativistic processes; SGR A-ASTERISK; STELLAR ORBITS; YOUNG STARS; GALAXY; RESOLUTION; SINFONI; FIELD; MILKY; DYNAMICS; TESTS;

D O I：

10.1051/0004-6361/202037813

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The star S2 orbiting the compact radio source Sgr A* is a precision probe of the gravitational field around the closest massive black hole (candidate). Over the last 2.7 decades we have monitored the star's radial velocity and motion on the sky, mainly with the SINFONI and NACO adaptive optics (AO) instruments on the ESO VLT, and since 2017, with the four-telescope interferometric beam combiner instrument GRAVITY. In this Letter we report the first detection of the General Relativity (GR) Schwarzschild Precession (SP) in S2's orbit. Owing to its highly elliptical orbit (e=0.88), S2's SP is mainly a kink between the pre-and post-pericentre directions of motion approximate to +/- 1 year around pericentre passage, relative to the corresponding Kepler orbit. The superb 2017-2019 astrometry of GRAVITY defines the pericentre passage and outgoing direction. The incoming direction is anchored by 118 NACO-AO measurements of S2's position in the infrared reference frame, with an additional 75 direct measurements of the S2-Sgr A* separation during bright states ("flares") of Sgr A*. Our 14-parameter model fits for the distance, central mass, the position and motion of the reference frame of the AO astrometry relative to the mass, the six parameters of the orbit, as well as a dimensionless parameter f(SP) for the SP (f(SP)=0 for Newton and 1 for GR). From data up to the end of 2019 we robustly detect the SP of S2, delta phi approximate to 12 ' per orbital period. From posterior fitting and MCMC Bayesian analysis with different weighting schemes and bootstrapping we find f(SP)=1.10 +/- 0.19. The S2 data are fully consistent with GR. Any extended mass inside S2's orbit cannot exceed approximate to 0.1% of the central mass. Any compact third mass inside the central arcsecond must be less than about 1000 M-circle dot.

引用

页数：14

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