A sub-Earth-mass planet orbiting Barnard's star*

被引：5

作者：

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

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

Silva, A. M. ^{[5
,6
]}

Stefanov, A. K. ^{[1
,2
]}

Faria, J. P. ^{[4
,5
,6
]}

Tabernero, H. M. ^{[17
]}

Sozzetti, A. ^{[11
]}

Rebolo, R. ^{[1
,2
,3
]}

Pepe, F. ^{[4
]}

Santos, N. C. ^{[5
,6
]}

Cristiani, S. ^{[9
,10
]}

Lovis, C. ^{[4
]}

Dumusque, X. ^{[4
]}

Figueira, P. ^{[4
,5
]}

Lillo-Box, J. ^{[8
]}

Nari, N. ^{[1
,2
,16
]}

Benatti, S. ^{[14
]}

Hobson, M. J. ^{[4
]}

Castro-Gonzalez, A. ^{[8
]}

Allart, R. ^{[4
,13
]}

Passegger, V. M. ^{[1
,2
,20
,21
]}

Osorio, M. -r. Zapatero ^{[8
]}

Adibekyan, V. ^{[5
,6
]}

Alibert, Y. ^{[18
,19
]}

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

Bouchy, F. ^{[4
]}

Damasso, M. ^{[11
]}

D'Odorico, V. ^{[9
,10
]}

Di Marcantonio, P. ^{[9
]}

Ehrenreich, D. ^{[4
]}

Lo Curto, G. ^{[12
]}

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

Martins, C. J. A. P. ^{[5
,7
]}

Mehner, A. ^{[12
]}

Micela, G. ^{[14
]}

Molaro, P. ^{[9
]}

Nunes, N. ^{[15
]}

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

Sousa, S. G. ^{[5
,6
]}

Udry, S. ^{[4
]}

机构：

[1] Inst Astrofis Canarias, San Cristobal la Laguna 38205, Tenerife, Spain

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

[3] CSIC, Barcelona, Spain

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

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

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

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

[8] CSIC INTA, Ctr Astrobiol CAB, Camino Bajo Castillo S-N,ESAC campus, Villanueva De La Canada 28692, Madrid, Spain

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

[10] IFPU Inst Fundamental Phys Universe, Via Beirut 2, I-34151 Trieste, Italy

[11] INAF Osservatorio Astrofis Torino, Str Osservatorio 20, I-10025 Pino Torinese, TO, Italy

[12] ESO European Southern Observ, Alonso de Cordova 3107, Vitacura, Santiago, Chile

[13] Univ Montreal, Inst Trottier Rech Exoplanetes, Dept Phys, Montreal, PQ H3T 1J4, Canada

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

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

[16] Univ Palmas De Gran Canaria, Dept Educ, Las Palmas Gran Canaria 35004, Spain

[17] Univ Complutense Madrid, Fac Ciencias Fis, Dept Fis Tierra & Astrofis & IPARCOS UCM, Inst Fis Particulas & Cosmos UCM, Madrid 28040, Spain

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

[19] Univ Bern, Phys Inst, Weltraumforschung & Planetol, Gesellschaftsstr 6, CH-3012 Bern, Switzerland

[20] Natl Astron Observ Japan, Subaru Telescope, 650 N Aohoku Pl, Hilo, HI 96720 USA

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

来源：

ASTRONOMY & ASTROPHYSICS | 2024年 / 690卷

基金：

瑞士国家科学基金会;

关键词：

techniques: radial velocities; techniques: spectroscopic; planets and satellites: terrestrial planets; stars: activity; stars: low-mass; stars: individual: GJ 699; HIGH-RESOLUTION SPECTROSCOPY; M-DWARFS; STELLAR ACTIVITY; TERRESTRIAL PLANET; ROTATION PERIODS; MAGNETIC-FIELDS; NO PLANET; STABILITY; SYSTEM; SEARCH;

D O I：

10.1051/0004-6361/202451311

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. ESPRESSO guaranteed time observations (GTOs) at the 8.2m VLT telescope were performed to look for Earth-like exoplanets in the habitable zone of nearby stars. Barnard's star is a primary target within the ESPRESSO GTO as it is the second closest neighbour to our Sun after the alpha Centauri stellar system. Aims. We present here a large set of 156 ESPRESSO observations of Barnard's star carried out over four years with the goal of exploring periods of shorter than 50 days, thus including the habitable zone (HZ). Methods. Our analysis of ESPRESSO data using Gaussian process (GP) to model stellar activity suggests a long-term activity cycle at 3200 d and confirms stellar activity due to rotation at 140 d as the dominant source of radial velocity (RV) variations. These results are in agreement with findings based on publicly available HARPS, HARPS-N, and CARMENES data. ESPRESSO RVs do not support the existence of the previously reported candidate planet at 233 d. Results. After subtracting the GP model, ESPRESSO RVs reveal several short-period candidate planet signals at periods of 3.15 d, 4.12 d, 2.34 d, and 6.74 d. We confirm the 3.15 d signal as a sub-Earth mass planet, with a semi-amplitude of 55 +/- 7 cm s(-1), leading to a planet minimum mass mp sin i of 0.37 +/- 0.05 M circle plus, which is about three times the mass of Mars. ESPRESSO RVs suggest the possible existence of a candidate system with four sub-Earth mass planets in circular orbits with semi-amplitudes from 20 to 47 cm s(-1), thus corresponding to minimum masses in the range of 0.17-0.32 M circle plus. Conclusions. The sub-Earth mass planet at 3.1533 +/- 0.0006 d is in a close-to circular orbit with a semi-major axis of 0.0229 +/- 0.0003 AU, thus located inwards from the HZ of Barnard's star, with an equilibrium temperature of 400 K. Additional ESPRESSO observations would be required to confirm that the other three candidate signals originate from a compact short-period planet system orbiting Barnard's star inwards from its HZ.

引用

页数：36

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