The CARMENES search for exoplanets around M dwarfs Wolf 1069 b: Earth-mass planet in the habitable zone of a nearby, very low-mass star

被引：10

作者：

Kossakowski, D. ^{[1
]}

Kuerster, M. ^{[1
]}

Trifonov, T. ^{[1
,2
]}

Henning, Th. ^{[1
]}

Kemmer, J. ^{[3
]}

Caballero, J. A. ^{[4
]}

Burn, R. ^{[1
]}

Sabotta, S. ^{[3
]}

Crouse, J. S. ^{[5
,6
,7
]}

Fauchez, T. J. ^{[5
,8
]}

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

Kaminski, A. ^{[3
]}

Herrero, E. ^{[11
,12
]}

Rodriguez, E. ^{[13
]}

Gonzalez-Alvarez, E. ^{[14
]}

Quirrenbach, A. ^{[3
]}

Amado, P. J. ^{[13
]}

Ribas, I. ^{[11
,12
]}

Reiners, A. ^{[15
]}

Aceituno, J. ^{[13
,16
]}

Bejar, V. J. S. ^{[17
,18
]}

Baroch, D. ^{[11
,12
]}

Bastelberger, S. T. ^{[5
,6
,7
]}

Chaturvedi, P. ^{[10
]}

Cifuentes, C. ^{[4
]}

Dreizler, S. ^{[15
]}

Jeffers, S. V. ^{[19
]}

Kopparapu, R. ^{[5
]}

Lafarga, M. ^{[11
,12
,20
]}

Lopez-Gonzalez, M. J. ^{[13
]}

Martin-Ruiz, S. ^{[13
]}

Montes, D. ^{[21
,22
]}

Morales, J. C. ^{[11
,12
]}

Palle, E. ^{[17
,18
]}

Pavlov, A. ^{[1
]}

Pedraz, S. ^{[16
]}

Perdelwitz, V. ^{[9
,23
]}

Perez-Torres, M. ^{[13
,24
]}

Perger, M. ^{[11
,12
]}

Reffert, S. ^{[3
]}

Rodriguez Lopez, C. ^{[13
]}

Schlecker, M. ^{[1
,25
]}

Schoefer, P. ^{[13
,15
]}

Schweitzer, A. ^{[9
]}

Shan, Y. ^{[15
,26
]}

Shields, A. ^{[27
]}

Stock, S. ^{[3
]}

Wolf, E. ^{[5
,28
,29
]}

Zapatero Osorio, M. R. ^{[14
]}

Zechmeister, M. ^{[15
]}

机构：

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

[2] Sofia Univ St Kliment Ohridski, Dept Astron, 5 James Bourchier Blvd, Sofia 1164, Bulgaria

[3] Heidelberg Univ, Zentrum Astronomie, Landessternwarte, Konigstuhl 12, D-69117 Heidelberg, Germany

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

[5] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA

[6] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[7] NASA, Ctr Res & Explorat Space Sci & Technol, GSFC, Greenbelt, MD 20771 USA

[8] Amer Univ, Coll Arts & Sci, Washington, DC USA

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

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

[11] CSIC, Inst Ciencies Espai ICE, C de Can Magrans S-N, Cerdanyola Del Valles 08193, Spain

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

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

[14] Ctr Astrobiol CSIC INTA, Carretera Ajalvir Km 4, Madrid 28850, Spain

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

[16] Observ Calar Alto, Ctr Astron Hispano Andalucia, Gergal 04550, Spain

[17] Inst Astrofis Canarias IAC, Tenerife 38200, Spain

[18] Univ La Laguna, Dept Astrofis, Tenerife 38206, Spain

[19] Max Planck Inst Sonnensyst Forsch, Justus von Liebig Weg 3, D-37077 Gottingen, Germany

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

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

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

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

[24] European Univ Cyprus, Sch Sci, Diogenes St, CY-1516 Nicosia, Cyprus

[25] Univ Arizona, Steward Observ, Dept Astron, 933 North Cherry Ave, Tucson, AZ 85721 USA

[26] Univ Oslo, Dept Geosci, Ctr Earth Evolut & Dynam, Sem Saelands Vei 2b, N-0315 Oslo, Norway

[27] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA

[28] Univ Colorado, Boulder Lab Atmospher & Space Phys, Dept Atmospher & Ocean Sci, Boulder, CO 80303 USA

[29] NASA, NExSS Virtual Planetary Lab, Seattle, WA USA

来源：

ASTRONOMY & ASTROPHYSICS | 2023年 / 670卷

基金：

欧洲研究理事会; 美国国家科学基金会; 瑞士国家科学基金会;

关键词：

methods: data analysis; planetary systems; stars: individual: Wolf 1069; stars: low-mass; techniques: radial velocities; MAIN-SEQUENCE STARS; SPECTROSCOPIC SURVEY; TRANSITING PLANET; ERROR-CORRECTION; GIANT PLANETS; SIZED PLANET; TARGET LIST; SOLAR; TEMPERATE; EMISSION;

D O I：

10.1051/0004-6361/202245322

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the discovery of an Earth-mass planet (M-b sin i = 1.26 +/- 0.21 M-circle plus) on a 15.6 d orbit of a relatively nearby (d similar to 9.6 pc) and low-mass (0.167 +/- 0.011 M-circle dot) M5.0 V star, Wolf 1069. Sitting at a separation of 0.0672 +/- 0.0014 au away from the host star puts Wolf 1069 b in the habitable zone (HZ), receiving an incident flux of S = 0.652 +/- 0.029 S-circle plus. The planetary signal was detected using telluric-corrected radial-velocity (RV) data from the CARMENES spectrograph, amounting to a total of 262 spectroscopic observations covering almost four years. There are additional long-period signals in the RVs, one of which we attribute to the stellar rotation period. This is possible thanks to our photometric analysis including new, well-sampled monitoring campaigns undergone with the OSN and TJO facilities that supplement archival photometry (i.e., from MEarth and SuperWASP), and this yielded an updated rotational period range of P-rot = 150-170 d, with a likely value at 169.3(-3.6)(+3.7)d. The stellar activity indicators provided by the CARMENES spectra likewise demonstrate evidence for the slow rotation period, though not as accurately due to possible factors such as signal aliasing or spot evolution. Our detectability limits indicate that additional planets more massive than one Earth mass with orbital periods of less than 10 days can be ruled out, suggesting that perhaps Wolf 1069 b had a violent formation history. This planet is also the sixth closest Earth-mass planet situated in the conservative HZ, after Proxima Centauri b, GJ 1061 d, Teegarden's Star c, and GJ 1002 b and c. Despite not transiting, Wolf 1069 b is nonetheless a very promising target for future three-dimensional climate models to investigate various habitability cases as well as for sub-m s(-1) RV campaigns to search for potential inner sub-Earth-mass planets in order to test planet formation theories.

引用

页数：25

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