Direct confirmation of the radial-velocity planet β Pictoris c

被引：95

作者：

Nowak, M. ^{[1
,2
]}

Lacour, S. ^{[3
,7
]}

Lagrange, A. -M. ^{[4
]}

Rubini, P. ^{[24
]}

Wang, J. ^{[10
]}

Stolker, T. ^{[27
]}

Abuter, R. ^{[7
]}

Amorim, A. ^{[16
,17
]}

Asensio-Torres, R. ^{[6
]}

Bauboeck, M. ^{[5
]}

Benisty, M. ^{[4
]}

Berger, J. P. ^{[4
]}

Beust, H. ^{[4
]}

Blunt, S. ^{[10
]}

Boccaletti, A. ^{[3
]}

Bonnefoy, M. ^{[4
]}

Bonnet, H. ^{[7
]}

Brandner, W. ^{[6
]}

Cantalloube, F. ^{[6
]}

Charnay, B. ^{[3
]}

Choquet, E. ^{[9
]}

Christiaens, V. ^{[13
]}

Clenet, Y. ^{[3
]}

du Foresto, V. Coude ^{[3
]}

Cridland, A. ^{[18
]}

de Zeeuw, P. T. ^{[5
,18
]}

Dembet, R. ^{[7
]}

Dexter, J. ^{[5
]}

Drescher, A. ^{[5
]}

Duvert, G. ^{[4
]}

Eckart, A. ^{[15
,21
]}

Eisenhauer, F. ^{[5
]}

Gao, F. ^{[5
]}

Garcia, P. ^{[17
,28
]}

Lopez, R. Garcia ^{[6
,19
]}

Gardner, T. ^{[12
]}

Gendron, E. ^{[3
]}

Genzel, R. ^{[5
]}

Gillessen, S. ^{[5
]}

Girard, J. ^{[11
]}

Grandjean, A. ^{[4
]}

Haubois, X. ^{[8
]}

Heissel, G. ^{[3
]}

Henning, T. ^{[6
]}

Hinkley, S. ^{[26
]}

Hippler, S. ^{[6
]}

Horrobin, M. ^{[15
]}

Houlle, M. ^{[9
]}

Hubert, Z. ^{[4
]}

Jimenez-Rosales, A. ^{[5
]}

机构：

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

[2] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England

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

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

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

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

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

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

[9] Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France

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

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

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

[13] Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia

[14] Cornell Univ, Dept Astron, Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA

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

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

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

[18] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands

[19] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland

[20] Pasadena City Coll, Pasadena, CA 91106 USA

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

[22] Univ Liege, STAR Inst, Liege, Belgium

[23] Ctr Astrophys Harvard & Smithsonian, Cambridge, MA 02138 USA

[24] Pixyl, 5 Av Grand Sablon, F-38700 La Tronche, France

[25] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia

[26] Univ Exeter, Phys Bldg,Stocker Rd, Exeter EX4 4QL, Devon, England

[27] Swiss Fed Inst Technol, Inst Particle Phys & Astrophys, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland

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

[29] Amherst Coll, Coll 5, Astron Dept, Amherst, MA 01002 USA

来源：

ASTRONOMY & ASTROPHYSICS | 2020年 / 642卷

基金：

欧洲研究理事会;

关键词：

planets and satellites: detection; planets and satellites: formation; techniques: interferometric; GIANT PLANETS; BROWN DWARFS; DUST; ACCRETION;

D O I：

10.1051/0004-6361/202039039

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Methods used to detect giant exoplanets can be broadly divided into two categories: indirect and direct. Indirect methods are more sensitive to planets with a small orbital period, whereas direct detection is more sensitive to planets orbiting at a large distance from their host star. This dichotomy makes it difficult to combine the two techniques on a single target at once.Aims. Simultaneous measurements made by direct and indirect techniques offer the possibility of determining the mass and luminosity of planets and a method of testing formation models. Here, we aim to show how long-baseline interferometric observations guided by radial-velocity can be used in such a way.Methods. We observed the recently-discovered giant planet beta Pictoris c with GRAVITY, mounted on the Very Large Telescope Interferometer.Results. This study constitutes the first direct confirmation of a planet discovered through radial velocity. We find that the planet has a temperature of T=125050 K and a dynamical mass of M=8.2 +/- 0.8 M-Jup. At 18.5 +/- 2.5 Myr, this puts beta Pic c close to a 'hot start' track, which is usually associated with formation via disk instability. Conversely, the planet orbits at a distance of 2.7 au, which is too close for disk instability to occur. The low apparent magnitude (M-K=14.3 +/- 0.1) favours a core accretion scenario.Conclusions. We suggest that this apparent contradiction is a sign of hot core accretion, for example, due to the mass of the planetary core or the existence of a high-temperature accretion shock during formation.

引用

页数：8

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