Mass distribution in the Galactic Center based on interferometric astrometry of multiple stellar orbits

被引：184

作者：

Abuter, R. ^{[8
]}

Aimar, N. ^{[2
]}

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

Ball, J. ^{[18
]}

Bauboeck, M. ^{[1
,16
]}

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

Bonnet, H. ^{[8
]}

Bourdarot, G. ^{[1
,5
]}

Brandner, W. ^{[3
]}

Cardoso, V ^{[13
,15
]}

Clenet, Y. ^{[2
]}

Dallilar, Y. ^{[1
]}

Davies, R. ^{[1
]}

de Zeeuw, P. T. ^{[1
,10
]}

Dexter, J. ^{[14
]}

Drescher, A. ^{[1
]}

Eisenhauer, F. ^{[1
]}

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

Foschi, A. ^{[13
,15
]}

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

Gao, F. ^{[1
,17
]}

Gendron, E. ^{[2
]}

Genzel, R. ^{[1
,11
,12
]}

Gillessen, S. ^{[1
]}

Habibi, M. ^{[1
]}

Haubois, X. ^{[9
]}

Heissel, G. ^{[2
]}

Henning, T. ^{[3
]}

Hippler, S. ^{[3
]}

Horrobin, M. ^{[4
]}

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
]}

Lutz, D. ^{[1
]}

Ott, T. ^{[1
]}

Paumard, T. ^{[2
]}

Perraut, K. ^{[5
]}

Perrin, G. ^{[2
]}

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

Rabien, S. ^{[1
]}

Shangguan, J. ^{[1
]}

Shimizu, T. ^{[1
]}

Scheithauer, S. ^{[3
]}

Stadler, J. ^{[1
]}

Stephens, A. W. ^{[18
]}

机构：

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

[2] Sorbonne Univ, Univ PSL, Univ Paris, 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, CNRS, IPAG, 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] Leiden Univ, Sterrewacht Leiden, Postbus 9513, NL-2300 RA Leiden, Netherlands

[11] Univ Calif Berkeley, Dept Phys, Le Conte Hall, Berkeley, CA 94720 USA

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

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

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

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

[16] Univ Illinois, Dept Phys, 1110 West Green St, Urbana, IL 61801 USA

[17] Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany

[18] NSFs NOIRLab, Gemini Observ, 670 N Aohoku Pl, Hilo, HI 96720 USA

来源：

ASTRONOMY & ASTROPHYSICS | 2022年 / 657卷

基金：

欧洲研究理事会;

关键词：

black hole physics; instrumentation; interferometers; Galaxy; center; SUPERMASSIVE BLACK-HOLE; SGR A-ASTERISK; YOUNG STARS; DYNAMICS; DISTANCE; MILKY; CUSP; MOTION; GALAXY; DISKS;

D O I：

10.1051/0004-6361/202142465

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Stars orbiting the compact radio source Sgr A* in the Galactic Center serve as precision probes of the gravitational field around the closest massive black hole. In addition to adaptive optics-assisted astrometry (with NACO/VLT) and spectroscopy (with SINFONI/VLT, NIRC2/Keck and GNIRS/Gemini) over three decades, we have obtained 30-100 mu as astrometry since 2017 with the four-telescope interferometric beam combiner GRAVITY/VLTI, capable of reaching a sensitivity of m(K)=20 when combining data from one night. We present the simultaneous detection of several stars within the diffraction limit of a single telescope, illustrating the power of interferometry in the field. The new data for the stars S2, S29, S38, and S55 yield significant accelerations between March and July 2021, as these stars pass the pericenters of their orbits between 2018 and 2023. This allows for a high-precision determination of the gravitational potential around Sgr A*. Our data are in excellent agreement with general relativity orbits around a single central point mass, M-center dot=4.30 x 10(6)M(circle dot), with a precision of about +/- 0.25%. We improve the significance of our detection of the Schwarzschild precession in the S2 orbit to 7 sigma. Assuming plausible density profiles, the extended mass component inside the S2 apocenter (approximate to 0.23 '' or 2.4 x 10(4)R(S)) must be less than or similar to 3000M(circle dot)(1 sigma), or less than or similar to 0.1% of M-center dot. Adding the enclosed mass determinations from 13 stars orbiting Sgr A* at larger radii, the innermost radius at which the excess mass beyond Sgr A* is tentatively seen is r approximate to 2.5 ''>= 10x the apocenter of S2. This is in full harmony with the stellar mass distribution (including stellar-mass black holes) obtained from the spatially resolved luminosity function.

引用

页数：17

共 50 条

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