Planetary system LHS 1140 revisited with ESPRESSO and TESS

J. Lillo-Box; P. Figueira; A. Leleu; L. Acuña; J. P. Faria; N. Hara; N. C. Santos; A. C. M. Correia; P. Robutel; M. Deleuil; D. Barrado; S. Sousa; X. Bonfils; O. Mousis; J. M. Almenara; N. Astudillo-Defru; E. Marcq; S. Udry; C. Lovis; F. Pepe

doi:10.1051/0004-6361/202038922

paper

Planetary system LHS 1140 revisited with ESPRESSO and TESS

arXiv:2010.06928 · doi:10.1051/0004-6361/202038922

Abstract

LHS 1140 is an M dwarf known to host two known transiting planets at orbital periods of 3.77 and 24.7 days. The external planet (LHS 1140 b) is a rocky super-Earth that is located in the middle of the habitable zone of this low-mass star, placing this system at the forefront of the habitable exoplanet exploration. We further characterize this system by improving the physical and orbital properties and search for additional planetary-mass components in the system, also exploring the possibility of co-orbitals. We collected 113 new radial velocity observations with ESPRESSO over a 1.5-year time span with an average photon-noise precision of 1.07 m/s. We determine new masses with a precision of 6% for LHS 1140 b ( $6.48 \pm 0.46 M_{\oplus}$ ) and 9% for LHS 1140 c ( $m_{c} = 1.78 \pm 0.17 M_{\oplus}$ ), reducing by half the previously published uncertainties. Although both planets have Earth-like bulk compositions, the internal structure analysis suggests that LHS 1140 b might be iron-enriched. In both cases, the water content is compatible to a maximum fraction of 10-12% in mass, which is equivalent to a deep ocean layer of $779 \pm 650$ km for the habitable-zone planet LHS 1140 b. Our results also provide evidence for a new planet candidate in the system ( $m_{d} = 4.8 \pm 1.1 M_{\oplus}$ ) on a ~78.9-day orbital period, which is detected through three independent methods. The analysis also allows us to discard other planets above 0.5 $M_{\oplus}$ for periods shorter than 10 days and above 2 $M_{\oplus}$ for periods up to one year. Finally, our analysis discards co-orbital planets of LHS 1140 b down to 1 $M_{\oplus}$ . Indications for a possible co-orbital signal in LHS 1140 c are detected in both radial velocity and photometric data, however. The new characterization of the system make it a key target for atmospheric studies of rocky worlds at different stellar irradiations

22 pages, 16 figures, 5 tables, published in A&A journal (see https://www.aanda.org/component/article?access=doi&doi=10.1051/0004-6361/202038922)

Planetary system LHS 1140 revisited with ESPRESSO and TESS

Abstract

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