TOI-179: A young system with a transiting compact Neptune-mass planet and a low-mass companion in outer orbit☆☆☆

被引：8

作者：

Desidera, S. ^{[1
]}

Damasso, M. ^{[2
]}

Gratton, R. ^{[1
]}

Benatti, S. ^{[3
]}

Nardiello, D. ^{[1
,4
]}

D'Orazi, V. ^{[1
,5
]}

Lanza, A. F. ^{[6
]}

Locci, D. ^{[3
]}

Marzari, F. ^{[1
,7
]}

Mesa, D. ^{[1
]}

Messina, S. ^{[4
]}

Pillitteri, I. ^{[3
]}

Sozzetti, A. ^{[2
]}

Girard, J. ^{[8
]}

Maggio, A. ^{[3
]}

Micela, G. ^{[3
]}

Malavolta, L. ^{[1
,9
]}

Nascimbeni, V. ^{[1
,9
]}

Pinamonti, M. ^{[2
]}

Squicciarini, V. ^{[1
,9
]}

Alcala, J. ^{[10
]}

Biazzo, K. ^{[11
]}

Bohn, A. ^{[12
]}

Bonavita, M. ^{[1
,13
,14
]}

Brooks, K. ^{[15
]}

Chauvin, G. ^{[16
]}

Covino, E. ^{[10
]}

Delorme, P. ^{[17
]}

Hagelberg, J. ^{[18
]}

Janson, M. ^{[19
]}

Lagrange, A. -M. ^{[17
]}

Lazzoni, C. ^{[1
,20
]}

机构：

[1] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy

[2] INAF Osservatorio Astrofisico Torino, Via Osservatorio 20, I-10025 Pino Torinese, TO, Italy

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

[4] Aix Marseille Univ, CNRS, CNES, LAM, F-13000 Marseille, France

[5] Monash Univ, Monash Ctr Astrophys, Sch Phys & Astron, Melbourne 3800, Australia

[6] INAF Osservatorio Astrofisico Catania, Via S Sofia 78, I-95123 Catania, Italy

[7] Unive Padova, Dipartimento Fis & Astron, Via Marzolo 8, I-35121 Padua, Italy

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

[9] Univ Padua, Dipartimento Fis & Astron, Vicolo Osservatorio 3, I-35122 Padua, Italy

[10] INAF Osservatorio Astron Capodimonte, Salita Moiariello 16, I-80131 Naples, Italy

[11] INAF Osservatorio Astron Roma, Via Frascati 33, I-00078 Rome, Italy

[12] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands

[13] Open Univ, Sch Phys Sci, Walton Hall, Milton Keynes MK7 6AA, England

[14] Univ Edinburgh, Inst Astron, SUPA, Blackford Hill, Edinburgh EH9 3HJ, Scotland

[15] Lab Atmospher & Space Phys, Innovat Dr Boulder 1234, 1234 Innovat Dr, Boulder, CO 80303 USA

[16] Univ Cote Azur, Observatoire Cote Azur, CNRS, Lab Lagrange, Bd Observatoire, CS 34229, F-06304 Nice 4, France

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

[18] Univ Geneva, Observ Geneve, 51 Ch Maillette, CH-1290 Sauverny, Switzerland

[19] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden

[20] Univ Exeter, Astrophys Grp, Phys Bldg, Stocker Rd, Exeter EX4 4QL, England

来源：

ASTRONOMY & ASTROPHYSICS | 2023年 / 675卷

关键词：

planetary systems; stars; individual; HD; 18599; planets and satellites; TOI-179b; binaries; close; techniques; radial velocities; high angular resolution; PRE-MAIN-SEQUENCE; SOLAR-TYPE STARS; TESS INPUT CATALOG; CHAIN MONTE-CARLO; GAPS PROGRAM; LITHIUM ABUNDANCES; ROTATION PERIODS; ERROR-CORRECTION; VARIABLE-STARS; GIANT PLANETS;

D O I：

10.1051/0004-6361/202244611

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Transiting planets around young stars are key benchmarks for our understanding of planetary systems. One such candidate, TOI-179, was identified around the K dwarf HD 18599 by TESS.Aims. We present the confirmation of the transiting planet and the characterization of the host star and of the TOI-179 system over a broad range of angular separations.Methods. We exploited the TESS photometric time series, intensive radial velocity monitoring performed with HARPS, and deep high-contrast imaging observations obtained with SPHERE and NACO at VLT. The inclusion of Gaussian process regression analysis was effective to properly model the magnetic activity of the star and identify the Keplerian signature of the transiting planet.Results. The star, with an age of 400 & PLUSMN;100 Myr, is orbited by a transiting planet with period 4.137436 days, mass 24 & PLUSMN;7 M-& OPLUS;, radius 2.62(-0.12)(+0.15) R-& OPLUS;, and significant eccentricity (0.34(-0.09)(+0.07)). Adaptive optics observations identified a low-mass companion at the boundary between brown dwarfs and very low-mass stars (mass derived from luminosity 83(-6)(+4) M-J) at a very small projected separation (84.5 mas, 3.3 au at the distance of the star). Coupling the imaging detection with the long-term radial velocity trend and the astrometric signature, we constrained the orbit of the low-mass companion, identifying two families of possible orbital solutions.Conclusions. The TOI-179 system represents a high-merit laboratory for our understanding of the physical evolution of planets and other low-mass objects and of how the planet properties are influenced by dynamical effects and interactions with the parent star.

引用

页数：25

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