GRAVITY K-band spectroscopy of HD 206893 B Brown dwarf or exoplanet

被引：8

作者：

Kammerer, J. ^{[1
,2
,22
]}

Lacour, S. ^{[1
,3
]}

Stolker, T. ^{[4
]}

Molliere, P. ^{[5
]}

Sing, D. K. ^{[27
,28
]}

Nasedkin, E. ^{[5
]}

Kervella, P. ^{[3
]}

Wang, J. J. ^{[6
]}

Ward-Duong, K. ^{[22
]}

Nowak, M. ^{[7
]}

Abuter, R. ^{[1
]}

Amorim, A. ^{[8
,9
]}

Asensio-Torres, R. ^{[5
]}

Baubock, M. ^{[10
]}

Benisty, M. ^{[11
]}

Berger, J-P ^{[11
]}

Beust, H. ^{[11
]}

Blunt, S. ^{[6
]}

Boccaletti, A. ^{[3
]}

Bohn, A. ^{[4
]}

Bolzer, M-L ^{[10
]}

Bonnefoy, M. ^{[11
]}

Bonnet, H. ^{[1
]}

Brandner, W. ^{[5
]}

Cantalloube, F. ^{[5
]}

Caselli, P. ^{[10
]}

Charnay, B. ^{[3
]}

Chauvin, G. ^{[11
]}

Choquet, E. ^{[12
]}

Christiaens, V ^{[13
]}

Clenet, Y. ^{[3
]}

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

Cridland, A. ^{[4
]}

Dembet, R. ^{[1
,3
]}

Dexter, J. ^{[14
,15
]}

de Zeeuw, P. T. ^{[4
,10
]}

Drescher, A. ^{[10
]}

Duvert, G. ^{[11
]}

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

Eisenhauer, F. ^{[10
]}

Gao, F. ^{[18
]}

Garcia, P. ^{[9
,19
]}

Lopez, R. Garcia ^{[5
,20
]}

Gendron, E. ^{[3
]}

Genzel, R. ^{[10
]}

Gillessen, S. ^{[10
]}

Girard, J. ^{[22
]}

Haubois, X. ^{[23
]}

Heissel, G. ^{[3
]}

Henning, T. ^{[5
]}

机构：

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

[27] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA

[28] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA

[29] Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,NTU AS Campus 1,Sect 4, Taipei 10617, Taiwan

来源：

ASTRONOMY & ASTROPHYSICS | 2021年 / 652卷

基金：

欧洲研究理事会;

关键词：

planets and satellites; atmospheres; planets and satellites: detection; planets and satellites: gaseous planets; techniques: interferometric; LOW-MASS STARS; SELF-CONSISTENT; GIANT PLANETS; RADIAL-VELOCITY; EXTREMELY RED; 1ST LIGHT; MU-M; YOUNG; COMPANION; DISCOVERY;

D O I：

10.1051/0004-6361/202140749

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Near-infrared interferometry has become a powerful tool for studying the orbital and atmospheric parameters of substellar companions. Aims. We aim to reveal the nature of the reddest known substellar companion HD 206893 B by studying its near-infrared colors and spectral morphology and by investigating its orbital motion. Methods. We fit atmospheric models for giant planets and brown dwarfs and perform spectral retrievals with petitRADTRANS and ATMO on the observed GRAVITY, SPHERE, and GPI spectra of HD 206893 B. To recover its unusual spectral features, first and foremost its extremely red near-infrared color, we include additional extinction by high-altitude dust clouds made of enstatite grains in the atmospheric model fits. However, forsterite, corundum, and iron grains predict similar extinction curves for the grain sizes considered here. We also infer the orbital parameters of HD 206893 B by combining the similar to 100 mu as precision astrometry from GRAVITY with data from the literature and constrain the mass and position of HD 206893 C based on the Gaia proper motion anomaly of the system. Results. The extremely red color and the very shallow 1.4 mu m water absorption feature of HD 206893 B can be fit well with the adapted atmospheric models and spectral retrievals. By comparison with AMES-Cond evolutionary tracks, we find that only some atmosphericmodels predict physically plausible objects. Altogether, our analysis suggests an age of similar to 3-300 Myr and a mass of similar to 5-30 M-Jup for HD 206893 B, which is consistent with previous estimates but extends the parameter space to younger and lower-mass objects. The GRAVITY astrometry points to an eccentric orbit (e = 0.29(-0.11)(+0.06)) with a mutual inclination of <34.4 deg with respect to the debris disk of the system. Conclusions. While HD 206893 B could in principle be a planetary-mass companion, this possibility hinges on the unknown influence of the inner companion on the mass estimate of 10(-4)(+5) M-Jup from radial velocity and Gaia as well as a relatively small but significant Argus moving group membership probability of similar to 61%. However, we find that if the mass of HD 206893 B is M-Jup, then the inner companion HD 206893 C should have a mass between similar to 8-15 M-Jup. Finally, further spectroscopic or photometric observations at higher signal-to-noise and longer wavelengths are required to learn more about the composition and dust cloud properties of HD 206893 B.

引用

页数：26

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