Astrometric detection of a Neptune-mass candidate planet in the nearest M-dwarf binary system GJ65 with VLTI/GRAVITY

被引：1

作者：

Abuter, R. ^{[4
]}

Amorim, A. ^{[7
,8
]}

Benisty, M. ^{[3
]}

Berger, J. P. ^{[3
]}

Bonnet, H. ^{[4
]}

Bourdarot, G. ^{[1
]}

Bourget, P. ^{[4
]}

Brandner, W. ^{[5
]}

Clenet, Y. ^{[2
]}

Davies, R. ^{[1
]}

Delplancke-Stroebele, F. ^{[4
]}

Dembet, R. ^{[2
]}

Drescher, A. ^{[1
]}

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

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

Feuchtgruber, H. ^{[1
]}

Finger, G. ^{[1
]}

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

Garcia, P. ^{[7
,10
]}

Garcia-Lopez, R. ^{[18
,19
]}

Gao, F. ^{[11
]}

Gendron, E. ^{[2
]}

Genzel, R. ^{[1
,12
,13
]}

Gillessen, S. ^{[1
]}

Hartl, M. ^{[1
]}

Haubois, X. ^{[9
]}

Haussmann, F. ^{[1
]}

Henning, T. ^{[5
]}

Hippler, S. ^{[5
]}

Horrobin, M. ^{[6
]}

Jochum, L. ^{[9
]}

Jocou, L. ^{[3
]}

Kaufer, A. ^{[9
]}

Kervella, P. ^{[2
]}

Lacour, S. ^{[2
]}

Lapeyrere, V ^{[2
]}

Le Bouquin, J. -B ^{[3
]}

Ledoux, C. ^{[9
]}

Lena, P. ^{[2
]}

Lutz, D. ^{[1
]}

Mang, F. ^{[1
]}

Merand, A. ^{[4
]}

More, N. ^{[1
]}

Nowak, M. ^{[20
]}

Ott, T. ^{[1
]}

Paumard, T. ^{[2
]}

Perraut, K. ^{[3
]}

Perrin, G. ^{[2
]}

Pfuhl, O. ^{[4
]}

Rabien, S. ^{[1
]}

机构：

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

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

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

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

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

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

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

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

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

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

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

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

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

[14] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany

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

[16] ORIGINS Excellence Cluster, Boltzmannstr 2, D-85748 Garching, Germany

[17] Tech Univ Munich, Dept Phys, D-85748 Garching, Germany

[18] Dublin Inst Adv Studies, 31 Fitzwilliam Pl, Dublin D02 XF86, Ireland

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

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

来源：

ASTRONOMY & ASTROPHYSICS | 2024年 / 685卷

基金：

欧盟地平线“2020”; 欧洲研究理事会;

关键词：

instrumentation: high angular resolution; instrumentation: interferometers; astrometry; planets and satellites: detection; planets and satellites: dynamical evolution and stability; stars: low-mass; LONG-TERM STABILITY; OPTICAL INTERFEROMETRY; SUBSTELLAR COMPANIONS; STELLAR MULTIPLICITY; NARROW-ANGLE; STARS; PERTURBATIONS; PARAMETERS; TELESCOPE; ASTROPY;

D O I：

10.1051/0004-6361/202449547

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The detection of low-mass planets orbiting the nearest stars is a central stake of exoplanetary science, as they can be directly characterized much more easily than their distant counterparts. Here, we present the results of our long-term astrometric observations of the nearest binary M-dwarf Gliese 65 AB (GJ65), located at a distance of only 2.67 pc. We monitored the relative astrometry of the two components from 2016 to 2023 with the VLTI/GRAVITY interferometric instrument. We derived highly accurate orbital parameters for the stellar system, along with the dynamical masses of the two red dwarfs. The GRAVITY measurements exhibit a mean accuracy per epoch of 50-60 ms in 1.5 h of observing time using the 1.8 m Auxiliary Telescopes. The residuals of the two-body orbital fit enable us to search for the presence of companions orbiting one of the two stars (S-type orbit) through the reflex motion they imprint on the differential A-B astrometry. We detected a Neptune-mass candidate companion with an orbital period of p = 156 +/- 1 d and a mass of mp = 36 +/- 7 M circle plus. The best-fit orbit is within the dynamical stability region of the stellar pair. It has a low eccentricity, e = 0.1 - 0.3, and the planetary orbit plane has a moderate-to-high inclination of i > 30 degrees with respect to the stellar pair, with further observations required to confirm these values. These observations demonstrate the capability of interferometric astrometry to reach microarcsecond accuracy in the narrow-angle regime for planet detection by reflex motion from the ground. This capability offers new perspectives and potential synergies with Gaia in the pursuit of low-mass exoplanets in the solar neighborhood.

引用

页数：10

共 59 条

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