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

被引：5

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

共 21 条

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Grieves, Nolan
Bouchy, Francois
Ulmer-Moll, Solene
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Henderson, Beth A.
Henze, Christopher E.
Jordan, Andres
Kendall, Alicia
Mishra, Lokesh
Moyano, Maximiliano
Osborn, Hugh
Revol, Alexandre
Sefako, Ramotholo R.
Tilbrook, Rosanna H.
Udry, Stephane
Unger, Nicolas
Vines, Jose I.
West, Richard G.
Worters, Hannah L.
ASTRONOMY & ASTROPHYSICS, 2022, 668
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