TOI-132 b: A short-period planet in the Neptune desert transiting a V = 11.3 G-type star. Issue 1 (29th January 2020)

• Record Type: Journal Article
• Authors: Díaz, Matías R; Jenkins, James S; Gandolfi, Davide; Lopez, Eric D; Soto, Maritza G; Cortés-Zuleta, Pía; Berdiñas, Zaira M; Stassun, Keivan G; Collins, Karen A; Vines, José I; Ziegler, Carl; Fridlund, Malcom; Jensen, Eric L N; Murgas, Felipe; Santerne, Alexandre; Wilson, Paul A; Esposito, Massimiliano; Hatzes, Artie P; Johnson, Marshall C; Lam, Kristine W F; Livingston, John H; Van Eylen, Vincent; Narita, Norio; Briceño, Cesar; Collins, Kevin I; Csizmadia, Szilárd; Fausnaugh, Michael; Gan, Tianjun; García, Rafael A; Georgieva, Iska; Glidden, Ana; González-Cuesta, Lucía; Jenkins, Jon M; Latham, David W; Law, Nicholas M; Mann, Andrew W; Mathur, Savita; Mireles, Ismael; Morris, Robert; Pallé, Enric; Persson, Carina M; Ricker, George; Rinehart, Stephen; Rose, Mark E; Seager, Sara; Smith, Jeffrey C; Tan, Thiam-Guan; Tokovinin, Andrei; Vanderburg, Andrew; Vanderspek, Roland; Winn, Joshua N; Yahalomi, Daniel A;
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 493:Issue 1(2020)
• Page Start: 973
• Page End: 985
• Publication Date: 2020-01-29
• Subjects: techniques: photometric -- techniques: radial velocities -- planets and satellites: fundamental parameters -- planetary systems; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/staa277
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: The Neptune desert is a feature seen in the radius-period plane, whereby a notable dearth of short period, Neptune-like planets is found. Here, we report the Transiting Exoplanet Survey Satellite ( TESS ) discovery of a new short-period planet in the Neptune desert, orbiting the G-type dwarf TYC 8003-1117-1 (TOI-132). TESS photometry shows transit-like dips at the level of ∼1400 ppm occurring every ∼2.11 d. High-precision radial velocity follow-up with High Accuracy Radial Velocity Planet Searcher confirmed the planetary nature of the transit signal and provided a semi-amplitude radial velocity variation of 11.38 $^{+0.84}_{-0.85}$ m s −1, which, when combined with the stellar mass of 0.97 ± 0.06 M⊙, provides a planetary mass of 22.40$^{+1.90}_{-1.92}$ M ⊕ . Modelling the TESS light curve returns a planet radius of 3.42$^{+0.13}_{-0.14}$ R ⊕, and therefore the planet bulk density is found to be 3.08$^{+0.44}_{-0.46}$ g cm −3 . Planet structure models suggest that the bulk of the planet mass is in the form of a rocky core, with an atmospheric mass fraction of 4.3$^{+1.2}_{-2.3}$ per cent. TOI-132 b is a TESS Level 1 Science Requirement candidate, and therefore priority follow-up will allow the search for additional planets in the system, whilst helping to constrain low-mass planet formation and evolution models, particularly valuable for better understanding of the Neptune desert.