The CARMENES search for exoplanets around M dwarfs Three temperate-to-warm super-Earths

被引：39

作者：

Stock, S. ^{[1
,18
]}

Nagel, E. ^{[2
,3
]}

Kemmer, J. ^{[1
]}

Passegger, V. M. ^{[2
,4
]}

Reffert, S. ^{[1
]}

Quirrenbach, A. ^{[1
]}

Caballero, J. A. ^{[6
]}

Czesla, S. ^{[2
]}

Bejar, V. J. S. ^{[11
,12
]}

Cardona, C. ^{[11
]}

Diez-Alonso, E. ^{[13
,14
,15
]}

Herrero, E. ^{[8
]}

Lalitha, S. ^{[7
]}

Schlecker, M. ^{[5
]}

Tal-Or, L. ^{[7
,16
]}

Rodriguez, E. ^{[10
]}

Rodriguez-Lopez, C. ^{[10
]}

Ribas, I ^{[8
,9
]}

Reiners, A. ^{[7
]}

Amado, P. J. ^{[10
]}

Bauer, F. F. ^{[10
]}

Bluhm, P. ^{[1
,18
]}

Cortes-Contreras, M. ^{[6
]}

Gonzalez-Cuesta, L. ^{[11
,12
]}

Dreizler, S. ^{[7
]}

Hatzes, A. P. ^{[3
]}

Henning, Th ^{[5
]}

Jeffers, S., V ^{[7
]}

Kaminski, A. ^{[1
]}

Kuerster, M. ^{[5
]}

Lafarga, M. ^{[8
,9
]}

Lopez-Gonzalez, M. J. ^{[10
]}

Montes, D. ^{[13
,14
]}

Morales, J. C. ^{[8
,9
]}

Pedraz, S. ^{[17
]}

Schoefer, P. ^{[7
]}

Schweitzer, A. ^{[2
]}

Trifonov, T. ^{[5
]}

Zapatero Osorio, M. R. ^{[6
]}

Zechmeister, M. ^{[7
]}

机构：

[1] Zentrum Astron Univ Heidelberg, Landessternwarte, Konigstuhl 12, D-69117 Heidelberg, Germany

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

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

[4] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 West Brooks St, Norman, OK 73019 USA

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

[6] ESAC, Ctr Astrobiol CSIC INTA, Camino Bajo Castillo S-N, Madrid 28692, Spain

[7] Georg August Univ, Inst Astrophys, Friedrich Hund Pl 1, D-37077 Gottingen, Germany

[8] CSIC, Inst Ciencies Espai ICE, Campus UAB,C Can Magrans S-N, Bellaterra, Spain

[9] Inst Estudis Espacials Catalunya IEEC, Barcelona 08034, Spain

[10] CSIC, Inst Astrofis Andalucia IAA, Glorieta Astron S-N, Granada 18008, Spain

[11] Inst Astrofis Canarias IAC, Tenerife 38205, Spain

[12] Univ La Laguna ULL, Dept Astrofis, Tenerife 38206, Spain

[13] Univ Complutense Madrid, Dept Fis Tierra & Astrofis, Fac Ciencias Fis, Madrid 28040, Spain

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

[15] Univ Oviedo, Dept Exploitat & Explorat Mines, Oviedo, Spain

[16] Ariel Univ, Dept Phys, IL-40700 Ariel, Israel

[17] Observatorio Calar Alto, Gergal 04550, Almeria, Spain

[18] Heidelberg Univ, IMPRS HD, Int Max Planck Res Sch Astron & Cosm Phys, Heidelberg, Germany

来源：

ASTRONOMY & ASTROPHYSICS | 2020年 / 643卷

关键词：

planetary systems; techniques: radial velocities; stars: individual: GJ 251; stars: individual: HD 238090; stars: individual: Lalande 21185; stars: late-type; PARSEC EVOLUTIONARY TRACKS; NEARBY STAR; STELLAR EVOLUTION; MASSIVE STARS; PLANET; ROTATION; MEMBERS; MODELS; SKY;

D O I：

10.1051/0004-6361/202038820

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We announce the discovery of two planets orbiting the M dwarfs GJ 251 (0.360 +/- 0.015M(circle dot)) and HD 238090 (0.578 +/- 0.021M(circle dot)) based on CARMENES radial velocity (RV) data. In addition, we independently confirm with CARMENES data the existence of Lalande 21185 b, a planet that has recently been discovered with the SOPHIE spectrograph. All three planets belong to the class of warm or temperate super-Earths and share similar properties. The orbital periods are 14.24 d, 13.67 d, and 12.95 d and the minimum masses are 4.0 +/- 0.4 M-circle plus, 6.9 +/- 0.9 M-circle plus, and 2.7 +/- 0.3 M-circle plus for GJ 251 b, HD 238090 b, and Lalande 21185 b, respectively. Based on the orbital and stellar properties, we estimate equilibrium temperatures of 351.0 +/- 1.4 K for GJ 251 b, 469.6 +/- 2.6 K for HD 238090 b, and 370.1 +/- 6.8 K for Lalande 21185 b. For the latter we resolve the daily aliases that were present in the SOPHIE data and that hindered an unambiguous determination of the orbital period. We find no significant signals in any of our spectral activity indicators at the planetary periods. The RV observations were accompanied by contemporaneous photometric observations. We derive stellar rotation periods of 122.1 +/- 2.2 d and 96.7 +/- 3.7 d for GJ 251 and HD 238090, respectively. The RV data of all three stars exhibit significant signals at the rotational period or its first harmonic. For GJ 251 and Lalande 21185, we also find long-period signals around 600 d, and 2900 d, respectively, which we tentatively attribute to long-term magnetic cycles. We apply a Bayesian approach to carefully model the Keplerian signals simultaneously with the stellar activity using Gaussian process regression models and extensively search for additional significant planetary signals hidden behind the stellar activity. Current planet formation theories suggest that the three systems represent a common architecture, consistent with formation following the core accretion paradigm.

引用

页数：35

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