A sub-Neptune and a non-transiting Neptune-mass companion unveiled by ESPRESSO around the bright late-F dwarf HD 5278 (TOI-130)

被引：26

作者：

Sozzetti, A. ^{[1
]}

Damasso, M. ^{[1
]}

Bonomo, A. S. ^{[1
]}

Alibert, Y. ^{[2
]}

Sousa, S. G. ^{[3
]}

Adibekyan, V. ^{[3
,4
]}

Zapatero Osorio, M. R. ^{[5
]}

Gonzalez Hernandez, J. I. ^{[6
,7
]}

Barros, S. C. C. ^{[3
,4
]}

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

Stassun, K. G. ^{[9
]}

Winn, J. ^{[10
]}

Cristiani, S. ^{[11
,12
]}

Pepe, F. ^{[13
]}

Rebolo, R. ^{[6
,7
,14
]}

Santos, N. C. ^{[3
,4
]}

Allart, R. ^{[13
,15
,16
]}

Barclay, T. ^{[17
,18
]}

Bouchy, F. ^{[13
]}

Cabral, A. ^{[19
,20
]}

Ciardi, D. ^{[21
]}

Di Marcantonio, P. ^{[11
]}

D'Odorico, V. ^{[11
,12
]}

Ehrenreich, D. ^{[13
]}

Fasnaugh, M. ^{[22
,23
]}

Figueira, P. ^{[3
,24
]}

Haldemann, J. ^{[2
]}

Jenkins, J. M. ^{[25
]}

Latham, D. W. ^{[26
]}

Lavie, B. ^{[13
]}

Lo Curto, G. ^{[24
]}

Lovis, C. ^{[13
]}

Martins, C. J. A. P. ^{[3
,27
]}

Megevand, D. ^{[13
]}

Mehner, A. ^{[24
]}

Micela, G. ^{[28
]}

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

Nunes, N. J. ^{[19
,20
]}

Oshagh, M. ^{[6
,7
]}

Otegi, J. ^{[13
,29
]}

Palle, E. ^{[6
,7
]}

Poretti, E. ^{[30
]}

Ricker, G. ^{[23
]}

Rodriguez, D. ^{[31
]}

Seager, S. ^{[22
,23
,32
,33
]}

Suarez Mascareno, A. ^{[6
,7
]}

Twicken, J. D. ^{[34
]}

Udry, S. ^{[13
]}

机构：

[1] Osserv Astron Torino, INAF, Via Osservatorio 20, I-10025 Pino Torinese, Italy

[2] Univ Bern, Inst Phys, Gesell Str 6, CH-3012 Bern, Switzerland

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

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

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

[6] Inst Astrofis Canarias, Via Lactea, Tenerife 38200, Spain

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

[8] Ctr Astrobiol CSIC INTA, ESAC Campus, Madrid 28692, Spain

[9] Vanderbilt Univ, Dept Phys & Astron, 6301 Stevenson Ctr Lane, Nashville, TN 37235 USA

[10] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA

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

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

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

[14] CSIC, Madrid 28006, Spain

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

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

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

[18] Univ Maryland, 1000 Hilltop Circle, Baltimore, MD 21250 USA

[19] Univ Lisbon, Fac Ciencias, Inst Astrofis & Ciencias Espaco, P-1749016 Lisbon, Portugal

[20] Univ Lisbon, Fac Ciencias, Dept Fis, Edificio C8, P-1749016 Lisbon, Portugal

[21] Caltech IPAC, 1200 E Calif Blvd, Pasadena, CA 91125 USA

[22] MIT, Dept Phys, Cambridge, MA 02139 USA

[23] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA

[24] European Southern Observ, ESO, Alonso Cordova 3107, Santiago, Chile

[25] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA

[26] Harvard & Smithsonian, Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA

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

[28] Osserv Astron Palermo, INAF, Piazza Parlamento 1, I-90134 Palermo, Italy

[29] Univ Zurich, Inst Computat Sci, Winterthurerstr 190, CH-8057 Zurich, Switzerland

[30] Osserv Astron Brera, INAF, Via Bianchi 46, I-23807 Merate, Italy

[31] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA

[32] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA

[33] MIT, Dept Aeronaut & Astronaut, 77 Massachusetts Ave, Cambridge, MA 02139 USA

[34] SETI Inst, Mountain View, CA 94043 USA

来源：

ASTRONOMY & ASTROPHYSICS | 2021年 / 648卷

基金：

欧洲研究理事会; 瑞士国家科学基金会;

关键词：

planetary systems; planets and satellites: composition; stars: individual: HD 5278 (TOI-130); techniques: radial velocities; techniques: photometric; methods: miscellaneous; MEAN MOTION RESONANCES; SUPER-EARTH; RADIUS DISTRIBUTION; TRANSMISSION SPECTROSCOPY; PLANET OCCURRENCE; ERROR-CORRECTION; I-ARCHITECTURE; CORALIE SURVEY; WATER-VAPOR; LONG-PERIOD;

D O I：

10.1051/0004-6361/202040034

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Transiting sub-Neptune-type planets, with radii approximately between 2 and 4 R-circle plus, are of particular interest as their study allows us to gain insight into the formation and evolution of a class of planets that are not found in our Solar System.Aims. We exploit the extreme radial velocity (RV) precision of the ultra-stable echelle spectrograph ESPRESSO on the VLT to unveil the physical properties of the transiting sub-Neptune TOI-130 b, uncovered by the TESS mission orbiting the nearby, bright, late F-type star HD 5278 (TOI-130) with a period of P-b = 14.3 days. Methods. We used 43 ESPRESSO high-resolution spectra and broad-band photometry information to derive accurate stellar atmospheric and physical parameters of HD 5278. We exploited the TESS light curve and spectroscopic diagnostics to gauge the impact of stellar activity on the ESPRESSO RVs. We performed separate as well as joint analyses of the TESS photometry and the ESPRESSO RVs using fully Bayesian frameworks to determine the system parameters. Results. Based on the ESPRESSO spectra, the updated stellar parameters of HD 5278 are T-eff = 6203 +/- 64 K, log g = 4.50 +/- 0.11 dex, [Fe/H] = -0.12 +/- 0.04 dex, M-star=1.126(-0.035)(+0.036) M-circle dot, and R-star=1.194(-0.016)(+0.017) R star=1.194(-0.016)(+0.017) R-circle dot. We determine HD 5278 b's mass and radius to be M-b=7.8(-1.4)(+1.5) M-circle plus and R-b = 2.45 +/- 0.05R(circle plus). The derived mean density, rho(b)=2.9(-0.5)(+0.6) g cm(-3), is consistent with the bulk composition of a sub-Neptune with a substantial (similar to 30%) water mass fraction and with a gas envelope comprising similar to 17% of the measured radius. Given the host brightness and irradiation levels, HD 5278 b is one of the best targetsorbiting G-F primaries for follow-up atmospheric characterization measurements with HST and JWST. We discover a second, non-transiting companion in the system, with a period of P-c=40.87(-0.17)(+0.18) days and a minimum mass of M-c sini(c)=18.4(-1.9)(+1.8) M-circle plus. We study emerging trends in parameters space (e.g., mass, radius, stellar insolation, and mean density) of the growing population of transiting sub-Neptunes, and provide statistical evidence for a low occurrence of close-in, 10 - 15M(circle plus) companions around G-F primaries with T-eff greater than or similar to 5500 K.

引用

页数：25

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