The planetary system around HD 190622 (TOI-1054) Measuring the gas content of low-mass planets orbiting F-stars

被引：1

作者：

Cabrera, J. ^{[1
]}

Gandolfi, D. ^{[2
]}

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

Csizmadia, Sz. ^{[1
]}

Egger, J. A. ^{[3
]}

Baumeister, Ph. ^{[1
]}

Krenn, A. ^{[4
]}

Benz, W. ^{[3
,5
]}

Deline, A. ^{[6
]}

Floren, H. -G. ^{[7
]}

Cameron, A. Collier ^{[8
]}

Adibekyan, V. ^{[9
]}

Alibert, Y. ^{[3
]}

Bellomo, S. E. ^{[2
]}

Delrez, L. ^{[10
,11
]}

Fossati, L.

Fortier, A. ^{[3
,5
]}

Grziwa, S. ^{[12
]}

Hoyer, S. ^{[13
]}

Bonfanti, A. ^{[14
]}

Salmon, S. ^{[6
]}

Sousa, S. G. ^{[9
]}

Wilson, T. G. ^{[8
]}

Alarcon, J. ^{[14
]}

Alonso, R. ^{[15
,16
]}

Anglada Escude, G. ^{[17
,18
]}

Barczy, T. ^{[19
]}

Barragan, O. ^{[20
]}

Barrado, D. ^{[21
]}

Barros, S. C. C. ^{[22
]}

Baumjohann, W.

Beck, M. ^{[6
]}

Beck, T.

Bernabo, L. M.

Billot, N. ^{[6
]}

Bonfils, X. ^{[23
]}

Borsato, L. ^{[24
]}

Brandeker, A. ^{[7
]}

Broeg, C. ^{[5
]}

Carrion-Gonzalez, O. ^{[25
,26
]}

Charnoz, S. ^{[27
]}

Ciardi, D. R. ^{[28
]}

Cochran, W. D. ^{[29
]}

Collins, K. A. ^{[30
]}

Collins, K. I. ^{[31
]}

Conti, D. M. ^{[32
]}

Davies, M. B. ^{[33
]}

Deeg, H. J. ^{[15
,16
]}

Deleuil, M.

Demangeon, O. D. S. ^{[22
]}

机构：

[1] German Aerosp Ctr DLR, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany

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

[3] Univ Bern, Physikal Inst, Sidlerstr 5, CH-3012 Bern, Switzerland

[4] Austrian Acad Sci, Space Res Inst, Schmiedlstr 6, A-8042 Graz, Austria

[5] Univ Bern, Ctr Space & Habitabil, Gesellschaftsstr 6, CH-3012 Bern, Switzerland

[6] Univ Geneva, Observ Astronom, Chemin Pegasi 51, CH-1290 Versoix, Switzerland

[7] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden

[8] Univ St Andrews, Ctr Exoplanet Sci, SUPA Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland

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

[10] Univ Liege, Astrobiol Res Unit, Allee 6-Aout 19C, B-4000 Liege, Belgium

[11] Univ Liege, Space Sci Technol & Astrophys Res STAR, Allee 6-Aout 19C, B-4000 Liege, Belgium

[12] Univ Cologne, Rhein Inst Umweltforsch, Abt. Planetenforsch, D-50931 Cologne, Germany

[13] Aix Marseille Univ, CNRS, CNES, LAM, 38 rue Frederic Joliot Curie, F-13388 Marseille, France

[14] European Southern Observ, Alonso Cordova 3107, Santiago, Chile

[15] Inst Astrofis Canarias, C Via Lactea S-N, San Cristobal la Laguna 38205, Tenerife, Spain

[16] Univ La Laguna, Dept Astrofis, Secc Fis, Ave Astrofis Francisco Sanchez S-N,Apartado 456, San Cristobal De La Lagu, Tenerife, Spain

[17] CSIC, ICE, Campus UAB,Can Magrans S-N, Bellaterra 08193, Spain

[18] IEEC, 2-4 Edifici Nexus,Desp 201, Barcelona 08034, Spain

[19] Admatis, 5 Kando Kalman St, H-3534 Miskolc, Hungary

[20] Univ Oxford, Sub Dept Astrophys, Dept Phys, Clarendon Lab, Parks Rd, Oxford OX1 3PU, England

[21] CSIC, INTA, Depto Astrofis, ESAC campus, Villanueva De La Canada 28692, Madrid, Spain

[22] Univ Porto, Dept Fis & Astron, Fac Ciencias, P-4169007 Porto, Portugal

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

[24] INAF, Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy

[25] Tech Univ Berlin, Zentrum Astron & Astrophys, Hardenbergstr 36, D-10623 Berlin, Germany

[26] Univ Paris Cite, LESIA, Observatoire Paris, Univ PSL,CNRS,Sorbonne Univ, 5 Pl Jules Janssen, F-92195 Meudon, France

[27] Univ Paris, Inst Phys Globe Paris, CNRS, 1 Rue Jussieu, F-75005 Paris, France

[28] Caltech, NASA Exoplanet Sci Inst Pasadena, IPAC, Pasadena, CA USA

[29] Univ Texas Austin, Ctr Planetary Syst Habitabil & McDonald Observ, 2305 Speedway Stop C116, Austin, TX 78712 USA

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

[31] George Mason Univ, Dept Phys & Astron, 4400 Univ Dr, Fairfax, VA 22030 USA

[32] Amer Assoc Variable Star Observers, 185 Alewife Brook Pkwy,Suite 410, Cambridge, MA 02138 USA

[33] Lund Univ, Ctr Math Sci, Box 118, S-22100 Lund, Sweden

[34] Univ Geneva, Fac Sci, Ctr Vie Univ, Quai Ernest Ansermet 30, CH-1211 Geneva 4, Switzerland

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

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

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

[38] Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria

[39] Univ Warwick, Dept Phys, Gibbet Hill Rd, Coventry CV4 7AL, England

[40] Cavendish Lab, JJ Thomson Ave, Cambridge CB3 0HE, England

[41] European Space Agcy, Sci & Operat Dept, Div Sci, Directorate Sci,European Space Res & Technol Ctr, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands

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

[43] Konkoly Observ Budapest, Res Ctr Astron & Earth Sci, Konkoly Thege Miklos Ut 15-17, H-1121 Budapest, Hungary

[44] Eotvos Lorand Univ, Inst Phys, Pazmany Petersetany 1-A, H-1117 Budapest, Hungary

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

[46] Sorbonne Univ, IMCCE, UMR8028 CNRS, Observatoire Paris,PSL Univ, 77 Ave Denfert Rochereau, F-75014 Paris, France

[47] Univ Paris 06, Inst Astrophys Paris, UMR7095 CNRS, 98bis bld Arago, F-75014 Paris, France

[48] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA

[49] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England

[50] MIT, Dept Phys, 70 Vassar St, Cambridge, MA 02139 USA

来源：

ASTRONOMY & ASTROPHYSICS | 2023年 / 675卷

基金：

欧洲研究理事会; 瑞士国家科学基金会; 英国科学技术设施理事会;

关键词：

planetary systems; planets and satellites: detection; SUPER-EARTH; RADIAL-VELOCITY; ELEMENTAL ABUNDANCE; SUB-NEPTUNES; ATMOSPHERIC EVOLUTION; LARGE INTERFEROMETER; INTERIOR STRUCTURE; STELLAR ROTATION; ERROR-CORRECTION; I-ARCHITECTURE;

D O I：

10.1051/0004-6361/202245774

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Giant planets are known to dominate the long-term stability of planetary systems due to their prevailing gravitational interactions, but they are also thought to play an important role in planet formation. Observational constraints improve our understanding of planetary formation processes such as the delivery of volatile-rich planetesimals from beyond the ice line into the inner planetary system. Additional constraints may come from studies of the atmosphere, but almost all such studies of the atmosphere investigate the detection of certain species, and abundances are not routinely quantitatively measured. Aims. Accurate measurements of planetary bulk parameters - that is, mass and density - provide constraints on the inner structure and chemical composition of transiting planets. This information provides insight into properties such as the amounts of volatile species, which in turn can be related to formation and evolution processes. Methods. The Transiting Exoplanet Survey Satellite (TESS) reported a planetary candidate around HD190622 (TOI-1054), which was subsequently validated and found to merit further characterization with photometric and spectroscopic facilities. The KESPRINT collaboration used data from the High Accuracy Radial Velocity Planet Searcher (HARPS) to independently confirm the planetary candidate, securing its mass, and revealing the presence of an outer giant planet in the system. The CHEOPS consortium invested telescope time in the transiting target in order to reduce the uncertainty on the radius, improving the characterization of the planet. Results. We present the discovery and characterization of the planetary system around HD190622 (TOI-1054). This system hosts one transiting planet, which is smaller than Neptune (3.087(-0.053)(+0.058) R-Earth, 7.7 +/- 1.0 M-Earth) but has a similar bulk density (1.43 +/- 0.21 g cm(-3)) and an orbital period of 16 days; and a giant planet, not known to be transiting, with a minimum mass of 227.0 +/- 6.7 M-Earth in an orbit with a period of 315 days. Conclusions. Our measurements constrain the structure and composition of the transiting planet. HD190622b has singular properties among the known population of transiting planets, which we discuss in detail. Among the sub-Neptune-sized planets known today, this planet stands out because of its large gas content.

引用

页数：14

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