Hobson, Melissa J. and Brahm, Rafael and Jordan, Andres and Espinoza, Nestor and Kossakowski, Diana and Henning, Thomas and Rojas, Felipe and Schlecker, Martin and Sarkis, Paula and Trifonov, Trifon and Thorngren, Daniel and Binnenfeld, Avraham and Shahaf, Sahar and Zucker, Shay and Ricker, George R. and Latham, David W. and Seager, S. and Winn, Joshua N. and Jenkins, Jon M. and Addison, Brett 
ORCID: https://orcid.org/0000-0003-3216-0626 and Bouchy, Francois and Bowler, Brendan P. and Briegal, Joshua T. and Bryant, Edward M. and Collins, Karen A. and Daylan, Tansu and Grieves, Nolan and Horner, Jonathan and Huang, Chelsea ORCID: https://orcid.org/0000-0003-0918-7484 and Kane, Stephen R. and Kielkopf, John and McLean, Brian and Mengel, Matthew W. ORCID: https://orcid.org/0000-0002-7830-6822 and Nielsen, Louise D. and Okumura, Jack and Jones, Matias and Plavchan, Peter and Shporer, Avi and Smith, Alexis M. S. and Tilbrook, Rosanna and Tinney, C. G. and Twicken, Joseph D. and Udry, Stephane and Unger, Nicolas and West, Richard and Wittenmyer, Robert A. and Wohler, Bill and Torres, Pascal and Wright, Duncan J.
(2021)
A transiting warm giant planet around the young active star TOI-201.
The Astronomical Journal, 161 (5):235.
ISSN 0004-6256
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Text (Submitted Version)
2103.02685.pdf Download (1MB) | Preview |
Abstract
We present the confirmation of the eccentric warm giant planet TOI-201 b, first identified as a candidate in Transiting Exoplanet Survey Satellite photometry (Sectors 1-8, 10-13, and 27-28) and confirmed using ground-based photometry from Next Generation Transit Survey and radial velocities from FEROS, HARPS, CORALIE, and Minerva-Australis. TOI-201 b orbits a young (0.87-0.49+0.46, Gyr) and bright (V = 9.07 mag) F-type star with a 52.9781 day period. The planet has a mass of 0.42-0.03+0.05, MJ, a radius of 1.008-0.015+0.012, RJ, and an orbital eccentricity of 0.28-0.09+0.06; it appears to still be undergoing fairly rapid cooling, as expected given the youth of the host star. The star also shows long-term variability in both the radial velocities and several activity indicators, which we attribute to stellar activity. The discovery and characterization of warm giant planets such as TOI-201 b are important for constraining formation and evolution theories for giant planets.
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Statistics for this ePrint Item |
| Item Type: | Article (Commonwealth Reporting Category C) |
|---|---|
| Refereed: | Yes |
| Item Status: | Live Archive |
| Additional Information: | © 2021. The American Astronomical Society. Submitted version deposited in accordance with the copyright policy of the publisher. |
| Faculty/School / Institute/Centre: | Current - Institute for Advanced Engineering and Space Sciences - Centre for Astrophysics (1 Aug 2018 -) |
| Faculty/School / Institute/Centre: | Current - Institute for Advanced Engineering and Space Sciences - Centre for Astrophysics (1 Aug 2018 -) |
| Date Deposited: | 29 Jul 2021 05:37 |
| Last Modified: | 29 Oct 2021 00:23 |
| Uncontrolled Keywords: | exoplanet astronomy; exoplanet detection methods; transit photometry; radial velocity; 486; 489; 1709; 1332; astrophysics; Earth; planetary astrophysics |
| Fields of Research (2008): | 02 Physical Sciences > 0201 Astronomical and Space Sciences > 020110 Stellar Astronomy and Planetary Systems |
| Fields of Research (2020): | 51 PHYSICAL SCIENCES > 5101 Astronomical sciences > 510109 Stellar astronomy and planetary systems |
| Socio-Economic Objectives (2008): | E Expanding Knowledge > 97 Expanding Knowledge > 970102 Expanding Knowledge in the Physical Sciences |
| Socio-Economic Objectives (2020): | 28 EXPANDING KNOWLEDGE > 2801 Expanding knowledge > 280120 Expanding knowledge in the physical sciences |
| Identification Number or DOI: | https://doi.org/10.3847/1538-3881/abeaa1 |
| URI: | http://eprints.usq.edu.au/id/eprint/42819 |
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