An old warm Jupiter orbiting the metal-poor G-dwarf TOI-5542

被引：8

作者：

Grieves, Nolan ^{[1
]}

Bouchy, Francois ^{[1
]}

Ulmer-Moll, Solene ^{[1
]}

Gill, Samuel ^{[2
,3
]}

Anderson, David R. ^{[2
,3
]}

Psaridi, Angelica ^{[1
]}

Lendl, Monika ^{[1
]}

Stassun, Keivan G. ^{[4
]}

Jenkins, Jon M. ^{[5
]}

Burleigh, Matthew R. ^{[6
]}

Acton, Jack S. ^{[6
]}

Boyd, Patricia T. ^{[7
]}

Casewell, Sarah L. ^{[6
]}

Eigmueller, Philipp ^{[8
]}

Goad, Michael R. ^{[6
]}

Goeke, Robert F. ^{[9
,10
]}

Guenther, Maximilian N. ^{[11
]}

Hawthorn, Faith ^{[2
,3
]}

Henderson, Beth A. ^{[6
]}

Henze, Christopher E. ^{[5
]}

Jordan, Andres ^{[12
,13
]}

Kendall, Alicia ^{[6
]}

Mishra, Lokesh ^{[1
]}

Moyano, Maximiliano ^{[14
]}

Osborn, Hugh ^{[9
,10
,15
]}

Revol, Alexandre ^{[1
]}

Sefako, Ramotholo R. ^{[16
]}

Tilbrook, Rosanna H. ^{[6
]}

Udry, Stephane ^{[1
]}

Unger, Nicolas ^{[1
]}

Vines, Jose, I ^{[17
]}

West, Richard G. ^{[2
,3
]}

Worters, Hannah L. ^{[16
]}

机构：

[1] Univ Geneva, Observ Geneve, 51 Chemin Pegasi, CH-1290 Versoix, Switzerland

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

[3] Univ Warwick, Ctr Exoplanets & Habitabil, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England

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

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

[6] Univ Leicester, Sch Phys & Astron, Leicester LE1 7RH, Leics, England

[7] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[8] German Aerosp Ctr, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany

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

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

[11] European Space Agcy ESA, European Space Res & Technol Ctr ESTEC, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands

[12] Univ Adolfo Ibanez, Fac Ingn & Ciencias, Av Diagonal Torres 2640, Santiago 7941169, Chile

[13] Millennium Inst Astrophys, Camino El Observatorio 1515, Santiago, Chile

[14] Univ Catolica Norte, Inst Astron, Angamos 0610, Antofagasta 1270709, Chile

[15] Univ Bern, Phys Inst, Sidlerstr 5, CH-3012 Bern, Switzerland

[16] South African Astron Observ, POB 9,Observ 7935, Cape Town, South Africa

[17] Univ Chile, Dept Astron, Casilla 36-D, Santiago, Chile

来源：

ASTRONOMY & ASTROPHYSICS | 2022年 / 668卷

基金：

瑞士国家科学基金会;

关键词：

planets and satellites: detection; planets and satellites: dynamical evolution and stability; planets and satellites: formation; planets and satellites: fundamental parameters; planets and satellites: gaseous planets; IN-SITU FORMATION; CA-II H; GIANT PLANETS; HOST STARS; MODEL ATMOSPHERES; ECLIPSING BINARY; HOT JUPITERS; CHROMOSPHERIC VARIATIONS; STELLAR METALLICITY; ERROR-CORRECTION;

D O I：

10.1051/0004-6361/202244077

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report the discovery of a 1.32(-0.10)(+0.10)M(Jup) planet orbiting on a 75.12 day period around the G3V 10.8(-3.6)(+2.1) Gyr old star TOI-5542 (TIC 466206508; TYC 9086-1210-1). The planet was first detected by the Transiting Exoplanet Survey Satellite (TESS) as a single transit event in TESS Sector 13. A second transit was observed 376 days later in TESS Sector 27. The planetary nature of the object has been confirmed by ground-based spectroscopic and radial velocity observations from the CORALIE and HARPS spectrographs. A third transit event was detected by the ground-based facilities NGTS, EulerCam, and SAAO. We find the planet has a radius of 1.009(-0.035)(+0.036)R(Jup) and an insolation of 9.6(-0.8)(+0.9)S(circle plus), along with a circular orbit that most likely formed via disk migration or in situ formation, rather than high-eccentricity migration mechanisms. Our analysis of the HARPS spectra yields a host star metallicity of [Fe/H] = -0.21 +/- 0.08, which does not follow the traditional trend of high host star metallicity for giant planets and does not bolster studies suggesting a difference among low- and high-mass giant planet host star metallicities. Additionally, when analyzing a sample of 216 well-characterized giant planets, we find that both high masses (4 M-Jup < M-p < 13 M-Jup) and low masses (0.5 M-Jup < M-p < 4 M-Jup), as well as both both warm (P > 10 days) and hot (P < 10 days) giant planets are preferentially located around metal-rich stars (mean [Fe/H] > 0.1). TOI-5542b is one of the oldest known warm Jupiters and it is cool enough to be unaffected by inflation due to stellar incident flux, making it a valuable contribution in the context of planetary composition and formation studies.

引用

页数：16

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