HD 183579b: a warm sub-Neptune transiting a solar twin detected by TESS

Gan, Tianjun and Bedell, Megan and Wang, Sharon Xuesong and Foreman-Mackey, Daniel and Melendez, Jorge and Mao, Shude and Stassun, Keivan G. and Howell, Steve B. and Ziegler, Carl and Wittenmyer, Robert A. and Hellier, Coel and Collins, Karen A. and Shporer, Avi and Ricker, George R. and Vanderspek, Roland and Latham, David W. and Seager, Sara and Winn, Joshua N. and Jenkins, Jon M. and Addison, Brett C. ORCID: https://orcid.org/0000-0003-3216-0626 and Ballard, Sarah and Barclay, Thomas and Bean, Jacob L. and Bowler, Brendan P. and Briceno, Cesar and Crossfield, Ian J. M. and Dittmann, Jason and Horner, Jonathan and Jensen, Eric L. N. and Kane, Stephen R. and Kielkopf, John and Kreidberg, Laura and Law, Nicholas and Mann, Andrew W. and Mengel, Matthew W. ORCID: https://orcid.org/0000-0002-7830-6822 and Morgan, Edward H. and Okumura, Jack and Osborn, Hugh P. and Paegert, Martin and Plavchan, Peter and Schwarz, Richard P. and Shiao, Bernie and Smith, Jeffrey C. and Spina, Lorenzo and Tinney, C. G. and Torres, Guillermo and Twicken, Joseph D. and Vezie, Michael and Wang, Gavin and Wright, Duncan J. ORCID: https://orcid.org/0000-0001-7294-5386 and Zhang, Hui (2021) HD 183579b: a warm sub-Neptune transiting a solar twin detected by TESS. Monthly Notices of the Royal Astronomical Society, 507 (2). pp. 2220-2240. ISSN 0035-8711

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We report the discovery and characterization of a transiting warm sub-Neptune planet around the nearby bright (V = 8.75 mag, K = 7.15 mag) solar twin HD 183579, delivered by the Transiting Exoplanet Survey Satellite (TESS). The host star is located 56.8 +/- 0.1 pc away with a radius of R-* = 0.97 +/- 0.02R(circle dot) and a mass of M-* = 1.03 +/- 0.05M(circle dot). We confirm the planetary nature by combining space and ground-based photometry, spectroscopy, and imaging. We find that HD 183579b (TOI-1055b) has a radius of R-p = 3.53 +/- 0.13R(circle plus) on a 17.47 d orbit with a mass of M-p = 11.2 +/- 5.4M(circle plus) (3 sigma mass upper limit of 27.4M(circle plus)). HD 183579b is the fifth brightest known sub-Neptune planet system in the sky, making it an excellent target for future studies of the interior structure and atmospheric properties. By performing a line-by-line differential analysis using the high-resolution and signal-to-noise ratio HARPS spectra, we find that HD 183579 joins the typical solar twin sample, without a statistically significant refractory element depletion.

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Item Type: Article (Commonwealth Reporting Category C)
Refereed: Yes
Item Status: Live Archive
Additional Information: Published 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: 10 Jan 2022 04:17
Last Modified: 07 Feb 2022 04:53
Uncontrolled Keywords: planets and satellites: detection; planets and satellites: gaseous; planets; planets and satellites: individual: (HD 183579; HIP 96160; TIC; 320004517; TOI 1055); stars: abundances; stars: solar type; Astrophysics; - Earth and Planetary Astrophysics; Astrophysics - Solar and Stellar; 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/10.1093/mnras/stab2224
URI: http://eprints.usq.edu.au/id/eprint/44808

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