First direct detection of an exoplanet by optical interferometry Astrometry and K-band spectroscopy of HR 8799 e

被引：117

作者：

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

Nowak, M. ^{[1
]}

Wang, J. ^{[21
]}

Pfuhl, O. ^{[2
]}

Eisenhauer, F. ^{[2
]}

Abuter, R. ^{[8
]}

Amorim, A. ^{[6
,15
]}

Anugu, N. ^{[7
,23
]}

Benisty, M. ^{[5
]}

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

Beust, H. ^{[5
]}

Blind, N. ^{[10
]}

Bonnefoy, M. ^{[5
]}

Bonnet, H. ^{[8
]}

Bourget, P. ^{[9
]}

Brandner, W. ^{[3
]}

Buron, A. ^{[2
]}

Collin, C. ^{[1
]}

Charnay, B. ^{[1
]}

Chapron, F. ^{[1
]}

Clenet, Y. ^{[1
]}

Coude du Foresto, V ^{[1
]}

de Zeeuw, P. T. ^{[2
,12
]}

Deen, C. ^{[2
]}

Dembet, R. ^{[1
]}

Dexter, J. ^{[2
]}

Duvert, G. ^{[5
]}

Eckart, A. ^{[4
,11
]}

Forster Schreiber, N. M. ^{[2
]}

Fedou, P. ^{[1
]}

Garcia, P. ^{[7
,9
,15
]}

Garcia Lopez, R. ^{[3
,16
]}

Gao, F. ^{[2
]}

Gendron, E. ^{[1
]}

Genzel, R. ^{[2
,13
,14
]}

Gillessen, S. ^{[2
]}

Gordo, P. ^{[6
,15
]}

Greenbaum, A. ^{[17
]}

Habibi, M. ^{[2
]}

Haubois, X. ^{[9
]}

Haussmann, F. ^{[2
]}

Henning, Th ^{[3
]}

Hippler, S. ^{[3
]}

Horrobin, M. ^{[4
]}

Hubert, Z. ^{[1
]}

Jimenez Rosales, A. ^{[2
]}

Jocou, L. ^{[5
]}

Kendrew, S. ^{[3
,18
]}

Kervella, P. ^{[1
]}

Kolb, J. ^{[9
]}

机构：

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

[2] Max Planck Inst Extraterr Phys, Giessenbach Str 1, D-85748 Garching, Germany

[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, Santiago 19001 19, Chile

[10] Univ Geneva, Observ Geneve, 51 Ch Maillettes, CH-1290 Versoix, Switzerland

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

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

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

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

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

[16] Dublin Inst Adv Studies, 31 Fitzwilliam Pl, Dublin 2, Ireland

[17] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

[18] Space Telescope Sci Inst, European Space Agcy, 3700 San Martin Dr, Baltimore, MD 21218 USA

[19] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[20] Univ Liege, STAR Inst, Allee Six Aout 19c, B-4000 Liege, Belgium

[21] CALTECH, Dept Astron, Pasadena, CA 91125 USA

[22] Univ Nacl Autonoma Mexico, Inst Astron, Apdo Postal 70264, Ciudad De Mexico 04510, Mexico

[23] Univ Exeter, Sch Phys, Astrophys Grp, Stocker Rd, Exeter EX4 4QL, Devon, England

来源：

ASTRONOMY & ASTROPHYSICS | 2019年 / 623卷

基金：

欧盟地平线“2020”;

关键词：

stars: individual: HR 8799; planets and satellites: atmospheres; planet-star interactions; techniques: interferometric; EFFECTIVE TEMPERATURES; ATMOSPHERES; STARS;

D O I：

10.1051/0004-6361/201935253

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Aims. To date, infrared interferometry at best achieved contrast ratios of a few times 10(-4) on bright targets. GRAVITY, with its dual-field mode, is now capable of high contrast observations, enabling the direct observation of exoplanets. We demonstrate the technique on HR 8799, a young planetary system composed of four known giant exoplanets. Methods. We used the GRAVITY fringe tracker to lock the fringes on the central star, and integrated off-axis on the HR 8799 e planet situated at 390 mas from the star. Data reduction included post-processing to remove the flux leaking from the central star and to extract the coherent flux of the planet. The inferred K band spectrum of the planet has a spectral resolution of 500. We also derive the astrometric position of the planet relative to the star with a precision on the order of 100 mu as. Results. The GRAVITY astrometric measurement disfavors perfectly coplanar stable orbital solutions. A small adjustment of a few degrees to the orbital inclination of HR 8799 e can resolve the tension, implying that the orbits are close to, but not strictly coplanar. The spectrum, with a signal-to-noise ratio of approximate to 5 per spectral channel, is compatible with a late- type L brown dwarf. Using Exo-REM synthetic spectra, we derive a temperature of 1150 +/- 50 K and a surface gravity of 10(4.3 +/- 0.3) cm s(2). This corresponds to a radius of 1.17(-0.11)(+0.13) R-Jup and a mass of 10(-4)(+7) M-Jup, which is an independent confirmation of mass estimates from evolutionary models. Our results demonstrate the power of interferometry for the direct detection and spectroscopic study of exoplanets at close angular separations from their stars.

引用

页数：6

共 8 条

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