Modeling the orbital motion of Sgr A*'s near-infrared flares

被引：71

作者：

Bauboeck, M. ^{[1
]}

Dexter, J. ^{[1
,18
,19
]}

Abuter, R. ^{[10
]}

Amorim, A. ^{[6
,7
]}

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

Bonnet, H. ^{[10
]}

Brandner, W. ^{[3
]}

Clenet, Y. ^{[2
]}

du Foresto, V. Coude ^{[2
]}

de Zeeuw, P. T. ^{[1
,12
]}

Duvert, G. ^{[5
]}

Eckart, A. ^{[4
,16
]}

Eisenhauer, F. ^{[1
]}

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

Gao, F. ^{[1
]}

Garcia, P. ^{[8
,9
,11
]}

Gendron, E. ^{[2
]}

Genzel, R. ^{[1
,13
,14
]}

Gerhard, O. ^{[1
]}

Gillessen, S. ^{[1
]}

Habibi, M. ^{[1
]}

Haubois, X. ^{[11
]}

Henning, T. ^{[3
]}

Hippler, S. ^{[3
]}

Horrobin, M. ^{[4
]}

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

Jocou, L. ^{[5
]}

Kervella, P. ^{[2
]}

Lacour, S. ^{[1
,2
]}

Lapeyrere, V ^{[2
]}

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

Lena, P. ^{[2
]}

Ott, T. ^{[1
]}

Paumard, T. ^{[2
]}

Perraut, K. ^{[5
]}

Perrin, G. ^{[2
]}

Pfuhl, O. ^{[1
]}

Rabien, S. ^{[1
]}

Coira, G. Rodriguez ^{[2
]}

Rousset, G. ^{[2
]}

Scheithauer, S. ^{[3
]}

Stadler, J. ^{[1
]}

Sternberg, A. ^{[15
,17
]}

Straub, O. ^{[1
]}

Straubmeier, C. ^{[4
]}

Sturm, E. ^{[1
]}

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

Vincent, F. ^{[2
]}

von Fellenberg, S. ^{[1
]}

Waisberg, I ^{[20
]}

机构：

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

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

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

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

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

[6] CENTRA, Campo Grande, P-1749016 Lisbon, Portugal

[7] Univ Lisbon, Fac Ciencias, Campo Grande, P-1749016 Lisbon, Portugal

[8] CENTRA, P-4200465 Porto, Portugal

[9] Univ Porto, Fac Engn, P-4200465 Porto, Portugal

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

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

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

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

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

[15] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel

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

[17] Flatiron Inst, Ctr Computat Astrophys, 162 5th Ave, New York, NY 10010 USA

[18] Univ Colorado, JILA, Boulder, CO 80309 USA

[19] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA

[20] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-7610001 Rehovot, Israel

来源：

ASTRONOMY & ASTROPHYSICS | 2020年 / 635卷

基金：

美国国家卫生研究院;

关键词：

black hole physics; Galaxy: center; accretion; accretion disks; ACCRETION FLOW; BLACK-HOLE; CENTRAL PARSEC; DISKS; CODE;

D O I：

10.1051/0004-6361/201937233

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Infrared observations of Sgr A* probe the region close to the event horizon of the black hole at the Galactic center. These observations can constrain the properties of low-luminosity accretion as well as that of the black hole itself. The GRAVITY instrument at the ESO VLTI has recently detected continuous circular relativistic motion during infrared flares which has been interpreted as orbital motion near the event horizon. Here we analyze the astrometric data from these flares, taking into account the effects of out-of-plane motion and orbital shear of material near the event horizon of the black hole. We have developed a new code to predict astrometric motion and flux variability from compact emission regions following particle orbits. Our code combines semi-analytic calculations of timelike geodesics that allow for out-of-plane or elliptical motions with ray tracing of photon trajectories to compute time-dependent images and light curves. We apply our code to the three flares observed with GRAVITY in 2018. We show that all flares are consistent with a hotspot orbiting at R similar to 9 gravitational radii with an inclination of i similar to 140 degrees. The emitting region must be compact and less than similar to 5 gravitational radii in diameter. We place a further limit on the out-of-plane motion during the flare.

引用

页数：9

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