A low-mass sub-Neptune planet transiting the bright active star HD 73344

被引：1

作者：

Sulis, S. ^{[1
]}

Crossfield, I. J. M. ^{[2
]}

Santerne, A. ^{[1
]}

Saillenfest, M. ^{[3
]}

Sousa, S. ^{[4
]}

Mary, D. ^{[5
]}

Aguichine, A. ^{[6
]}

Deleuil, M. ^{[1
]}

Mena, E. Delgado ^{[4
]}

Mathur, S. ^{[7
,8
]}

Polanski, A. ^{[2
]}

Adibekyan, V. ^{[4
,9
]}

Boisse, I. ^{[1
]}

Costes, J. C. ^{[1
]}

Cretignier, M. ^{[10
]}

Heidari, N. ^{[11
]}

Lebarbe, C. ^{[3
]}

Forveille, T. ^{[12
]}

Hara, N. ^{[1
]}

Meunier, N. ^{[12
]}

Santos, N. ^{[4
,9
]}

Balcarcel-Salazar, S. ^{[13
]}

Cortes-Zuleta, P. ^{[14
]}

Dalal, S. ^{[15
]}

Gorjian, V. ^{[16
]}

Halverson, S. ^{[16
]}

Howard, A. W. ^{[17
]}

Kosiarek, M. R. ^{[6
]}

Lopez, T. A. ^{[1
]}

Martin, D. V. ^{[18
]}

Mousis, O. ^{[1
,19
]}

Rajkumar, B. ^{[5
]}

Strom, P. A. ^{[20
]}

Udry, S. ^{[21
]}

Venot, O. ^{[22
,23
]}

Willett, E. ^{[24
]}

机构：

[1] Univ Aix Marseille, CNRS, CNES, LAM, Marseille, France

[2] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA

[3] Univ Lille, Sorbonne Univ, PSL Res Univ, CNRS,Observ Paris,IMCCE, F-75014 Paris, France

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

[5] Univ Cote Azur, Observ Cote Azur, CNRS, Lab Lagrange, Bd Observ,CS 34229, F-06304 Nice, France

[6] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA USA

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

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

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

[10] Univ Oxford, Subdept Astrophys, Dept Phys, Oxford OX1 3RH, England

[11] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR 7095, 98 Bis Bd Arago, F-75014 Paris, France

[12] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France

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

[14] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Scotland

[15] Univ Exeter, Astrophys Grp, Exeter EX4 2QL, England

[16] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

[17] CALTECH, Dept Astron, Pasadena, CA 91125 USA

[18] Tufts Univ, Dept Phys & Astron, 574 Boston Ave, Medford, MA 02155 USA

[19] Inst Univ France IUF, Paris, France

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

[21] Univ Geneva, Geneva Observ, Chemin Maillettes 51, CH-1290 Versoix, Switzerland

[22] Univ Paris Cite, F-75013 Paris, France

[23] Univ Paris Est Creteil, CNRS, LISA, F-75013 Paris, France

[24] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, England

来源：

ASTRONOMY & ASTROPHYSICS | 2024年 / 688卷

基金：

欧洲研究理事会; 英国科学技术设施理事会;

关键词：

planets and satellites: detection; planets and satellites: fundamental parameters; stars: individual: TOI 5140; stars: individual: HD 73344; SOLAR-LIKE OSCILLATIONS; 1111 FGK STARS; MAGNETIC-ACTIVITY; STELLAR ACTIVITY; RADIAL-VELOCITY; SOPHIE SEARCH; SUPER-EARTH; PHOTOMETRIC ACTIVITY; CHEMICAL ABUNDANCES; SURFACE ROTATION;

D O I：

10.1051/0004-6361/202449559

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Planets with radii of between 2 and 4 R-circle plus closely orbiting solar-type stars are of significant importance for studying the transition from rocky to giant planets, and are prime targets for atmospheric characterization by missions such as JWST and ARIEL. Unfortunately, only a handful of examples with precise mass measurements are known to orbit bright stars. Aims. Our goal is to determine the mass of a transiting planet around the very bright F6 star HD 73344 (Vmag = 6.9). This star exhibits high activity and has a rotation period that is close to the orbital period of the planet (P-b = 15.6 days). Methods. The transiting planet, initially a K2 candidate, is confirmed through TESS observations (TOI 5140.01). We refined its parameters using TESS data and rule out a false positive with Spitzer observations. We analyzed high-precision radial velocity (RV) data from the SOPHIE and HIRES spectrographs. We conducted separate and joint analyses of K2, TESS, SOPHIE, and HIRES data using the PASTIS software. Given the star's early type and high activity, we used a novel observing strategy, targeting the star at high cadence for two consecutive nights with SOPHIE to understand the short-term stellar variability. We modeled stellar noise with two Gaussian processes: one for rotationally modulated stellar processes, and one for short-term stellar variability. Results. High-cadence RV observations provide better constraints on stellar variability and precise orbital parameters for the transiting planet: a radius of R-b = 2.88(-0.07)(+0.08) R-circle plus and a mass of M-b = 2.98(-1.90)(+2.50) M-circle plus (upper-limit at 3 sigma is <10.48 M-circle plus). The derived mean density suggests a sub-Neptune-type composition, but uncertainties in the planet's mass prevent a detailed characterization. In addition, we find a periodic signal in the RV data that we attribute to the signature of a nontransiting exoplanet, without totally excluding the possibility of a nonplanetary origin. This planetary candidate would have a minimum mass of about M-c sin i(c) = 116.3 +/- (+12.8)(-13.0) M-circle plus and a period of P-c = 66.45(-0.25)(+0.10) days. Dynamical analyses confirm the stability of the two-planet system and provide constraints on the inclination of the candidate planet; these findings favor a near-coplanar system. Conclusions. While the transiting planet orbits the bright star at a short period, stellar activity prevented us from precise mass measurements despite intensive RV follow-up. Long-term RV tracking of this planet could improve this measurement, as well as our understanding of the activity of the host star. The latter will be essential if we are to characterize the atmosphere of planets around F-type stars using transmission spectroscopy.

引用

页数：25

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