The CARMENES search for exoplanets around M dwarfs Planet occurrence rates from a subsample of 71 stars

被引：99

作者：

Sabotta, S. ^{[1
,2
]}

Schlecker, M. ^{[3
]}

Chaturvedi, P. ^{[1
]}

Guenther, E. W. ^{[1
]}

Munoz Rodriguez, I. ^{[4
]}

Munoz Sanchez, J. C. ^{[5
,6
]}

Caballero, J. A. ^{[7
]}

Shan, Y. ^{[8
]}

Reffert, S. ^{[2
]}

Ribas, I. ^{[5
,6
]}

Reiners, A. ^{[8
]}

Hatzes, A. P. ^{[1
]}

Amado, P. J. ^{[4
]}

Klahr, H. ^{[3
]}

Morales, J. C. ^{[5
,6
]}

Quirrenbach, A. ^{[2
]}

Henning, Th. ^{[3
]}

Dreizler, S. ^{[8
]}

Palle, E. ^{[9
,10
]}

Perger, M. ^{[5
,6
]}

Azzaro, M. ^{[11
]}

Jeffers, S. V. ^{[12
]}

Kaminski, A. ^{[2
]}

Kurster, M. ^{[3
]}

Lafarga, M. ^{[5
,6
,13
]}

Montes, D. ^{[14
,15
]}

Passegger, V. M. ^{[16
,17
]}

Zechmeister, M. ^{[8
]}

机构：

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

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

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

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

[5] CSIC, Inst Ciencies Espai ICE, Campus UAB,C Can Magrans S-N, Barcelona 08193, Spain

[6] Inst Estudis Espacials Catalunya IEEC, C Gran Capita 2-4, Barcelona 08034, Spain

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

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

[9] Inst Astrofis Canarias, Via Lactea S-N, Tenerife 38205, Spain

[10] Univ La Laguna, Dept Astrofis, Tenerife 38026, Spain

[11] Max Planck Inst Solar Syst Res, Justus von Liebig Weg 3, D-37077 Gottingen, Germany

[12] Ctr Astron Hispano Aleman CSIC Junta Andalucia, Observatorio Astron Calar Alto, Almeria 04550, Spain

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

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

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

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

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

来源：

ASTRONOMY & ASTROPHYSICS | 2021年 / 653卷 / 653期

关键词：

planetary systems; techniques: radial velocities; methods: data analysis; stars: low-mass; SUPER-EARTH; SOLAR NEIGHBORHOOD; HABITABLE ZONE; MASS; NEPTUNE; HOT; DETECTABILITY; TEMPERATE; SYSTEMS; PAIR;

D O I：

10.1051/0004-6361/202140968

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. The CARMENES exoplanet survey of M dwarfs has obtained more than 18 000 spectra of 329 nearby M dwarfs over the past five years as part of its guaranteed time observations (GTO) program. Aims. We determine planet occurrence rates with the 71 stars from the GTO program for which we have more than 50 observations. Methods. We use injection -and-retrieval experiments on the radial -velocity time series to measure detection probabilities. We include 27 planets in 21 planetary systems in our analysis. Results. We find 0.06(-0.03)(+0.04) giant planets (100 M-circle plus < M-p1 sin i < 1000 M-circle plus) per star in periods of up to 1000 d, but due to a selection bias this number could be up to a factor of five lower in the whole 329 -star sample. The upper limit for hot Jupiters (orbital period of less than 10 d) is 0.03 planets per star, while the occurrence rate of planets with intermediate masses (10 M-circle plus < M-pl sin i < 100 M-circle plus) is 0.18(-0.05)(+0.07) planets per star. Less massive planets with 1 M-circle plus < M-pl sin i < 10 M-circle plus are very abundant, with an estimated rate of 1.3213331 planets per star for periods of up to 100 d. When considering only late M dwarfs with masses M-star < 0.34 M-circle dot, planets more massive than 10 M become rare. Instead, low-mass planets with periods shorter than 10 d are significantly overabundant. Conclusions. For orbital periods shorter than 100 d, our results confirm the known stellar mass dependences from the Kepler survey: M dwarfs host fewer giant planets and at least two times more planets with M-p1 sin i < 10 M-circle plus than G-type stars. In contrast to previous results, planets around our sample of very low-mass stars have a higher occurrence rate in short-period orbits of less than 10 d. Our results demonstrate the need to take into account host star masses in planet formation models.

引用

页数：15

共 98 条

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