TOI-220b: a warm sub-Neptune discovered by TESS

被引：6

作者：

Hoyer, S. ^{[1
]}

Gandolfi, D. ^{[2
]}

Armstrong, D. J. ^{[3
,4
]}

Deleuil, M. ^{[1
]}

Acuna, L. ^{[1
]}

de Medeiros, J. R. ^{[5
]}

Goffo, E. ^{[2
]}

Lillo-Box, J. ^{[6
]}

Delgado Mena, E. ^{[7
,8
]}

Lopez, T. A. ^{[1
]}

Santerne, A. ^{[1
]}

Sousa, S. ^{[7
,8
]}

Fridlund, M. ^{[9
,10
]}

Adibekyan, V ^{[7
,8
]}

Collins, K. A. ^{[11
]}

Serrano, L. M. ^{[2
]}

Cortes-Zuleta, P. ^{[1
]}

Howell, S. B. ^{[12
]}

Deeg, H. ^{[13
,14
]}

Aguichine, A. ^{[1
]}

Barragan, O. ^{[15
]}

Bryant, E. M. ^{[3
,4
]}

Canto Martins, B. L. ^{[5
]}

Collins, K., I ^{[16
]}

Cooke, B. F. ^{[3
,4
]}

Diaz, R. F. ^{[17
,18
]}

Esposito, M. ^{[19
]}

Furlan, E. ^{[20
]}

Hojjatpanah, S. ^{[7
,8
]}

Jackman, J. ^{[3
,4
]}

Jenkins, J. M. ^{[12
]}

Jensen, E. L. N. ^{[21
]}

Latham, D. W. ^{[9
]}

Leao, I. C. ^{[5
]}

Matson, R. A. ^{[22
]}

Nielsen, L. D. ^{[23
]}

Osborn, A. ^{[3
,4
]}

Otegi, J. F. ^{[23
,24
]}

Rodler, F. ^{[25
]}

Sabotta, S. ^{[19
]}

Scott, N. J. ^{[12
]}

Seager, S. ^{[26
,27
,28
,29
]}

Stockdale, C. ^{[30
]}

Strom, P. A. ^{[3
,4
]}

Vanderspek, R. ^{[26
,27
]}

Van Eylen, V. ^{[31
]}

Wheatley, P. J. ^{[3
,4
]}

Winn, J. N. ^{[32
]}

Almenara, J. M. ^{[33
]}

Barrado, D. ^{[6
]}

机构：

[1] Aix Marseille Univ, LAM, CNES, CNRS, F-13388 Marseille, France

[2] Univ Torino, Dipartimento Fis, Via Pietro Giuria 1, I-10125 Turin, Italy

[3] Univ Warwick, Ctr Exoplanets & Habitabil, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England

[4] Univ Warwick, Dept Phys, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England

[5] Univ Fed Rio Grande do Norte, Dept Fis Teor & Expt, Campus Univ, BR-59072970 Natal, RN, Brazil

[6] CSIC INTA, Dept Astrofis, Ctr Astrobiol CAB, ESAC Campus, E-28692 Villanueva De La Canada, Madrid, Spain

[7] Univ Porto, Inst Astrofis & Ciencias Espaco, CAUP, Rua Estrelas, P-4150762 Porto, Portugal

[8] Univ Porto, Fac Ciencias, Dept Fis & Astron, Rua Campo Alegre, P-4169007 Porto, Portugal

[9] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands

[10] Chalmers Univ Technol, Dept Space Earth & Environm, Onsala Space Observ, SE-43992 Onsala, Sweden

[11] Ctr Astrophys Harvard & Smithsonian, 60 Garden St, Cambridge, MA 02138 USA

[12] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA

[13] Inst Astrofis Canarias, E-38205 Tenerife, Spain

[14] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain

[15] Univ Oxford, Subdept Astrophys, Dept Phys, Oxford, England

[16] George Mason Univ, 4400 Univ Dr, Fairfax, VA 22030 USA

[17] ECyT UNSAM, Int Ctr Adv Studies ICAS, Campus Miguelete,25 Mayo & Francia, RA-1650 Buenos Aires, DF, Argentina

[18] ECyT UNSAM, ICIFI CONICET, Campus Miguelete,25 Mayo & Francia, RA-1650 Buenos Aires, DF, Argentina

[19] Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany

[20] CALTECH, IPAC, NASA Exoplanet Sci Inst, Mail Code 100-22,1200 E Calif Blvd, Pasadena, CA 91125 USA

[21] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA

[22] US Naval Observ, 3450 Massachusetts Ave NW, Washington, DC 20392 USA

[23] Observ Univ Geneve, Chemin Maillettes 51, CH-1290 Versoix, Switzerland

[24] Univ Zurich, Inst Computat Sci, Winterthurerstr 190, CH-8057 Zurich, Switzerland

[25] European Southern Observ, Alonso de Cordova 3107, Santiago, Chile

[26] MIT, Dept Phys, Cambridge, MA 02139 USA

[27] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA

[28] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA

[29] MIT, Dept Aeronaut & Astronaut, 77 Massachusetts Ave, Cambridge, MA 02139 USA

[30] Hazelwood Observ, Churchill, Vic 3842, Australia

[31] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England

[32] Princeton Univ, Dept Astrophys Sci, 4 Ivy Lane, Princeton, NJ 08544 USA

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

[34] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[35] Inst Planetenforsch, Deutsch Zentrum Luft & Raumfahrt, Rutherfordstr 2, D-12489 Berlin, Germany

[36] Univ Texas Austin, Ctr Planetary Syst Habitabil, Austin, TX 78730 USA

[37] Univ Texas Austin, McDonald Observ, Austin, TX 78730 USA

[38] Noqsi Aerosp Ltd, 15 Blanchard Ave, Billerica, MA 01821 USA

[39] Univ Cologne, Rhein Inst Umweltforsch, Aachener Str 209, D-50931 Cologne, Germany

[40] Czech Acad Sci, Astron Inst, Fricova 298, CZ-25168 Ondrejov, Czech Republic

[41] Aarhus Univ, Stellar Astrophys Ctr, Dept Phys & Astron, Ny Munkegade 120, DK-8000 Aarhus C, Denmark

[42] Univ Tokyo, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan

[43] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA

[44] Univ Bern, Ctr Space & Habitabil, NCCR PlanetS, Gesell Str 6 G6, CH-3012 Bern, Switzerland

[45] Wesleyan Univ, Astron Dept, Middletown, CT 06459 USA

[46] Wesleyan Univ, Van Vleck Observ, Middletown, CT 06459 USA

[47] SETI Inst, Mountain View, CA 94043 USA

[48] Columbia Univ, Dept Astron, 550 W 120th St, New York, NY 10027 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2021年 / 505卷 / 03期

关键词：

techniques: photometric; techniques: radial velocities; planets and satellites: fundamental parameters; planets and satellites: individual: TYC 8897-01263-1; stars: fundamental parameters; EXTRASOLAR PLANET VALIDATION; POWERED MASS-LOSS; RADIUS DISTRIBUTION; ERROR-CORRECTION; STARS; CORE; EXOPLANETS; VARIABILITY; PARAMETERS; VELOCITIES;

D O I：

10.1093/mnras/stab1427

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

In this paper, we report the discovery of TOI-220b, a new sub-Neptune detected by the Transiting Exoplanet Survey Satellite (TESS) and confirmed by radial velocity follow-up observations with the HARPS spectrograph. Based on the combined analysis of TESS transit photometry and high precision radial velocity measurements, we estimate a planetary mass of 13.8 +/- 1.0M(circle plus) and radius of 3.03 +/- 0.15R(circle plus), implying a bulk density of 2.73 +/- 0.47. TOI-220b orbits a relative bright (V=10.4) and old (10.1 +/- 1.4Gyr) K dwarf star with a period of similar to 10.69d. Thus, TOI-220b is a new warm sub-Neptune with very precise mass and radius determinations. A Bayesian analysis of the TOI-220b internal structure indicates that due to the strong irradiation it receives, the low density of this planet could be explained with a steam atmosphere in radiative-convective equilibrium and a supercritical water layer on top of a differentiated interior made of a silicate mantle and a small iron core.

引用

页码：3361 / 3379

页数：19

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