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

被引：0

作者：

Abuter, R. ^{[8
]}

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

Bauböck, M. ^{[1
]}

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

Bonnet, H. ^{[8
]}

Brandner, W. ^{[3
]}

Cardoso, V. ^{[13
,15
]}

Clénet, Y. ^{[2
]}

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

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

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

Eisenhauer, F. ^{[1
]}

Förster Schreiber, N.M. ^{[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
]}

Jiménez-Rosales, A. ^{[1
]}

Jochum, L. ^{[9
]}

Jocou, L. ^{[5
]}

Kaufer, A. ^{[9
]}

Kervella, P. ^{[2
]}

Lacour, S. ^{[2
]}

Lapeyrère, V. ^{[2
]}

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

Léna, P. ^{[2
]}

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

Ott, T. ^{[1
]}

Paumard, T. ^{[2
]}

Perraut, K. ^{[5
]}

Perrin, G. ^{[2
]}

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

Rodríguez-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 Institute for Extraterrestrial Physics, Giessenbachstraße 1, Garching,85748, Germany

[2] LESIA Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, 5 Place Jules Janssen, Meudon,92195, France

[3] Max Planck Institute for Astronomy, Königstuhl 17, Heidelberg,69117, Germany

[4] 1st Institute of Physics, University of Cologne, Zülpicher Straße 77, Cologne,50937, Germany

[5] Univ. Grenoble Alpes, CNRS, IPAG, Grenoble,38000, France

[6] Universidade de Lisboa, Faculdade de Ciências Campo Grande, Lisboa,1749-016, Portugal

[7] Faculdade de Engenharia, Universidade Do Porto, Rua Dr. Roberto Frias, Porto,4200-465, Portugal

[8] European Southern Observatory, Karl-Schwarzschild-Straße 2, Garching,85748, Germany

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

[10] Max Planck Institute for Radio Astronomy, Auf dem Hügel 69, Bonn,53121, Germany

[11] Sterrewacht Leiden, Leiden University, Postbus 9513, Leiden,2300 RA, Netherlands

[12] Departments of Physics and Astronomy, University of California, Le Conte Hall, Berkeley,CA,94720, United States

[13] CENTRA - Centro de Astrofísica e Gravitação, IST, Universidade de Lisboa, Lisboa,1049-001, Portugal

[14] Department of Astrophysical and Planetary Sciences, JILA, University of Colorado, Duane Physics Bldg., 2000 Colorado Ave, Boulder,CO,80309, United States

[15] CERN, 1 Espl. des Particules, Genève 23, 1211, Switzerland

[16] Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot,76100, Israel

[17] Institute of Astronomy, Madingley Road, Cambridge,CB3 0HA, United Kingdom

来源：

Astronomy and Astrophysics | 2020年 / 636卷

关键词：

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 ≈±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 fSP for the SP (fSP = 0 for Newton and 1 for GR). From data up to the end of 2019 we robustly detect the SP of S2; δφ ≈ 12′ per orbital period. From posterior fitting and MCMC Bayesian analysis with different weighting schemes and bootstrapping we find fSP = 1.10 ± 0.19. The S2 data are fully consistent with GR. Any extended mass inside S2's orbit cannot exceed ≈0.1% of the central mass. Any compact third mass inside the central arcsecond must be less than about 1000 M. © GRAVITY Collaboration 2020;

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