Paper

NIRPS and TESS reveal a peculiar system around the M dwarf TOI-756: A transiting sub-Neptune and a cold eccentric giant

João Gomes da Silva, Vandal, Thomas, Khaled Al Moulla, Cristo, Eduardo, Jayawardhana, Ray, Hubin, Norbert, Grieves, Nolan, Blind, Nicolas, Delisle, Jean-Baptiste, Charbonneau, David, Frensch, Yolanda G C, Messamah, Lina, Messias, Yuri S, Silber, Armin, Fontinele, Dasaev O, Reshetov, Vladimir, Hans-Ulrich Käufl, Gromek, Nicole, Segovia, Alex, Bryan, Marta, Darveau-Bernier, Antoine, Delfosse, Xavier, Roseane de Lima Gomes, Cabral, Alexandre, Moranta, Leslie, Poulin-Girard, Anne-Sophie, Matthews, Jaymie, Stefanov, Atanas K, Yariv, Vincent, Rebolo, Rafael, Delgado-Mena, Elisa, Carmona, Andres, Pasquini, Luca, Chazelas, Bruno, Dauplaise, Laurie, Thibault, Simon, veille, Thierry, Osborn, Ares, Santos, Nuno C, Ségransan, Damien, Aguiar, José L A, Hoeijmakers, Jens H, Sordet, Michael, Sosnowska, Danuta, Arial, Tomy, Nielsen, Louise D, Auger, Hugues, Kung, Benjamin, Figueira, Pedro, Lamontagne, Pierrot, Barros, Susana C C, Abreu, Manuel, Hobson, Melissa J, Peroux, Céline, Izan de Castro Leão, Malo, Lison, Ouellet, Mathieu, Weisserman, Drew, Boisse, Isabelle, Wevers, Ivan, Bovay, Sébastien, Passegger, Vera M, Ehrenre

2025

Overview

The Near InfraRed Planet Searcher (NIRPS) joined HARPS on the 3.6-m ESO telescope at La Silla Observatory in April 2023, dedicating part of its Guaranteed Time Observations (GTO) program to the radial velocity follow-up of TESS planet candidates to confirm and characterize transiting planets around M dwarfs. We report the first results of this program with the characterization of the TOI-756 system, which consists of TOI-756 b, a transiting sub-Neptune candidate detected by TESS, as well as TOI-756 c, an additional non-transiting planet discovered by NIRPS and HARPS. TOI-756 b is a 1.24-day period sub-Neptune with a radius of 2.81 \\(\\pm\\) 0.10 \\(R_\\oplus\\) and a mass of 9.8\\(^{+1.8}_{-1.6}\\) \\(M_\\oplus\\). TOI-756 c is a cold eccentric (e\\(_c\\) = 0.45 \\(\\pm\\) 0.01) giant planet orbiting with a period of 149.6 days around its star with a minimum mass of 4.05 \\(\\pm\\) 0.11 \\(M_\\mathrm{jup}\\). Additionally, a linear trend of 146\\(~\\mathrm{m\\,s}^{-1}\\,\\mathrm{yr}^{-1}\\) is visible in the radial velocities, hinting at a third component, possibly in the planetary or brown dwarf regime. This system is unique in the exoplanet landscape, standing as the first confirmed example of such a planetary architecture around an M dwarf. With a density of 2.42 \\(\\pm\\) 0.49 g cm\\(^{-3}\\), the inner planet, TOI-756 b, is a volatile-rich sub-Neptune. Assuming a pure H/He envelope, we inferred an atmospheric mass fraction of 0.023 and a core mass fraction of 0.27, which is well constrained by stellar refractory abundances derived from NIRPS spectra. It falls within the still poorly explored radius cliff and at the lower boundary of the Neptune desert, making it a prime target for a future atmospheric characterization with JWST to improve our understanding of this population.

• Publisher: Cornell University Library, arXiv.org
• Subject: European Southern Observatory / Extrasolar planets / Neptune / Radial velocity / Red dwarf stars / Transit