An unusually low density ultra-short period super-Earth and three mini-Neptunes around the old star TOI-561. Issue 3 (8th December 2020)

• Record Type: Journal Article
• Authors: Lacedelli, G; Malavolta, L; Borsato, L; Piotto, G; Nardiello, D; Mortier, A; Stalport, M; Collier Cameron, A; Poretti, E; Buchhave, L A; López-Morales, M; Nascimbeni, V; Wilson, T G; Udry, S; Latham, D W; Bonomo, A S; Damasso, M; Dumusque, X; Jenkins, J M; Lovis, C; Rice, K; Sasselov, D; Winn, J N; Andreuzzi, G; Cosentino, R; Charbonneau, D; Di Fabrizio, L; Martnez Fiorenzano, A F; Ghedina, A; Harutyunyan, A; Lienhard, F; Micela, G; Molinari, E; Pagano, I; Pepe, F; Phillips, D F; Pinamonti, M; Ricker, G; Scandariato, G; Sozzetti, A; Watson, C A;
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 501:Issue 3(2021)
• Page Start: 4148
• Page End: 4166
• Publication Date: 2020-12-08
• Subjects: techniques: photometric -- techniques: radial velocities -- planets and satellites: composition -- planets and satellites: detection -- stars: individual: TOI-561 (TIC 377064495, Gaia DR2 3850421005290172416); Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/staa3728
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: Based on HARPS-N radial velocities (RVs) and TESS photometry, we present a full characterization of the planetary system orbiting the late G dwarf TOI-561. After the identification of three transiting candidates by TESS, we discovered two additional external planets from RV analysis. RVs cannot confirm the outer TESS transiting candidate, which would also make the system dynamically unstable. We demonstrate that the two transits initially associated with this candidate are instead due to single transits of the two planets discovered using RVs. The four planets orbiting TOI-561 include an ultra-short period (USP) super-Earth (TOI-561 b) with period P b = 0.45 d, mass M b = 1.59 ± 0.36 M⊕ and radius R b = 1.42 ± 0.07 R⊕, and three mini-Neptunes: TOI-561 c, with P c = 10.78 d, M c = 5.40 ± 0.98 M⊕, R c = 2.88 ± 0.09 R⊕ ; TOI-561 d, with P d = 25.6 d, M d = 11.9 ± 1.3 M⊕, R d = 2.53 ± 0.13 R⊕ ; and TOI-561 e, with P e = 77.2 d, M e = 16.0 ± 2.3 M⊕, R e = 2.67 ± 0.11 R⊕ . Having a density of 3.0 ± 0.8 g cm −3, TOI-561 b is the lowest density USP planet known to date. Our N-body simulations confirm the stability of the system and predict a strong, anti-correlated, long-term transit time variation signal between planets d and e. The unusual density of the inner super-Earth and the dynamical interactions between the outer planets make TOI-561 an interesting follow-up target.