The compact multi-planet system GJ 9827 revisited with ESPRESSO☆☆☆

被引：8

作者：

Passegger, V. M. ^{[1
,2
,3
]}

Mascareno, A. Suarez ^{[1
,2
]}

Allart, R. ^{[4
,5
,6
]}

Hernandez, J. I. Gonzalez ^{[1
,2
]}

Lovis, C. ^{[6
]}

Lavie, B. ^{[6
]}

Silva, A. M. ^{[7
,8
]}

Mueller, H. M. ^{[3
]}

Tabernero, H. M. ^{[9
,10
]}

Cristiani, S. ^{[11
]}

Pepe, F. ^{[12
]}

Rebolo, R. ^{[1
,2
,13
]}

Santos, N. C. ^{[7
,8
]}

Adibekyan, V. ^{[7
,8
]}

Alibert, Y. ^{[14
,15
]}

Prieto, C. Allende ^{[1
,2
]}

Barros, S. C. C. ^{[7
,8
]}

Bouchy, F. ^{[6
]}

Castro-Gonzalez, A. ^{[16
]}

D'Odorico, V. ^{[11
]}

Dumusque, X. ^{[6
]}

Di Marcantonio, P. ^{[11
]}

Ehrenreich, D. ^{[6
]}

Figueira, P. ^{[6
,7
]}

Santos, R. Genova ^{[1
,2
]}

Lo Curto, G. ^{[17
]}

Martins, C. J. A. P. ^{[7
,18
]}

Mehner, A. ^{[17
]}

Micela, G. ^{[19
]}

Molaro, P. ^{[11
]}

Nari, N. ^{[1
,2
,24
]}

Nunes, N. J. ^{[20
]}

Palle, E. ^{[1
,2
]}

Poretti, E. ^{[21
]}

Rodrigues, J. ^{[7
,8
,22
]}

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

Sozzetti, A. ^{[23
]}

Udry, S. ^{[6
]}

Osorio, M. R. Zapatero ^{[16
]}

机构：

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

[2] Univ La Laguna, Dept Astrofis, San Cristobal la Laguna 38206, Tenerife, Spain

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

[4] Univ Montreal, Dept Phys, Montreal, PQ H3T 1J4, Canada

[5] Univ Montreal, Trottier Inst Res Exoplanets, Montreal, PQ H3T 1J4, Canada

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

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

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

[9] Univ Complutense Madrid, Dept Fis Tierra & Astrofis, Madrid 28040, Spain

[10] Univ Complutense Madrid, Fac Ciencias Fis, IPARCOS UCM, Inst Fis Particulas & Cosmos UCM, Madrid 28040, Spain

[11] INAF Osservatorio Astron Trieste, Via Tiepolo 11, I-34143 Trieste, Italy

[12] Univ Geneva, Dept Astron, Chemin Pegasi 51, CH-1290 Versoix, Switzerland

[13] CSIC, Madrid 28006, Spain

[14] Univ Bern, Phys Inst, Gesellschaftsstr 6, CH-3012 Bern, Switzerland

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

[16] CSIC INTA, Ctr Astrobiol, Camino Bajo Castillo S N, Villanueva De La Canada 28692, Madrid, Spain

[17] European Southern Observ, Av Alonso Cordova 3107, Vitacura, Santiago De Chi, Chile

[18] Univ Porto, Ctr Astrofis, Rua Estrelas, P-4150762 Porto, Portugal

[19] INAF Osservatorio Astron Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy

[20] Fac Ciencias Univ Lisboa, Inst Astrofis & Ciencias Espaco, P-1749016 Campo Grande, Lisboa, Portugal

[21] INAF Osservatorio Astron Brera, Via Bianchi 46, I-23807 Merate, Italy

[22] Observ Francois Xavier Bagnoud OFXB, CH-3961 St Luc, Switzerland

[23] INAF Osservatorio Astrofisico Torino, Str Osservatorio 20, I-10025 Pino Torinese, TO, Italy

[24] Light Bridges SL, Avda Alcalde Ramirez Bethencourt 17, Las Palmas Gran Canaria 35004, Canarias, Spain

来源：

ASTRONOMY & ASTROPHYSICS | 2024年 / 684卷

基金：

欧洲研究理事会; 瑞士国家科学基金会;

关键词：

methods: data analysis; techniques: photometric; techniques: radial velocities; techniques: spectroscopic; stars: fundamental parameters; stars: individual: GJ 9827; LATE K-DWARF; SUPER-EARTHS; EXTENDED ATMOSPHERES; INTERIOR STRUCTURE; HARPS SEARCH; LOVE NUMBER; MASS; KEPLER; RADIUS; DETECTABILITY;

D O I：

10.1051/0004-6361/202348592

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

GJ 9827 is a bright, nearby K7V star orbited by two super-Earths and one mini-Neptune on close-in orbits. The system was first discovered using K2 data and then further characterized by other spectroscopic and photometric instruments. Previous literature studies provide several mass measurements for the three planets, however, with large variations and uncertainties. To better constrain the planetary masses, we added high-precision radial velocity measurements from ESPRESSO to published datasets from HARPS, HARPS-N, and HIRES and we performed a Gaussian process analysis combining radial velocity and photometric datasets from K2 and TESS. This method allowed us to model the stellar activity signal and derive precise planetary parameters. We determined planetary masses of M-b=4.28+0.35-0.33 M-circle plus, Mc=1.86(-0.39 )(+0.37)M(circle plus), and M-d=3.02+0.58-0.57 M-circle plus, and orbital periods of 1.208974 +/- 0.000001 days for planet b, 3.648103+0.000013-0.000010 days for planet c, and 6.201812 +/- 0.000009 days for planet d. We compared our results to literature values and found that our derived uncertainties for the planetary mass, period, and radial velocity amplitude are smaller than the previously determined uncertainties. We modeled the interior composition of the three planets using the machine-learning-based tool ExoMDN and conclude that GJ 9827 b and c have an Earth-like composition, whereas GJ 9827 d has an hydrogen envelope, which, together with its density, places it in the mini-Neptune regime.

引用

页数：28

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