Beth A. BillerAntoine GrandjeanMESSINA, SergioSergioMESSINADESIDERA, SilvanoSilvanoDESIDERAPhilippe DelormeAnne-Marie LagrangeFranz-Josef HambschMESA, DinoDinoMESAMarkus JansonGRATTON, RaffaeleRaffaeleGRATTONValentina D'OraziMaud LangloisAnne-Lise MaireJoshua SchliederThomas HenningAlice ZurloJanis HagelbergS. BrownC. RomeroMickaël BonnefoyGael ChauvinMarkus FeldtMichael MeyerArthur ViganA. PavlovC. SoenkeD. LeMignantA. Roux2025-01-212025-01-2120220004-6361http://hdl.handle.net/20.500.12386/35687We present orbital fits and dynamical masses for HIP 113201AB and HIP 36985AB, two M1 + mid-M dwarf binary systems monitored as part of the SPHERE SHINE survey. To robustly determine ages via gyrochronology, we undertook a photometric monitoring campaign for HIP 113201 and for GJ 282AB, the two wide K star companions to HIP 36985, using the 40 cm Remote Observatory Atacama Desert (ROAD) telescope. We adopt ages of 1.2$\pm$0.1 Gyr for HIP 113201AB and 750$\pm$100 Myr for HIP 36985AB. To derive dynamical masses for all components of these systems, we used parallel-tempering Markov Chain Monte Carlo sampling to fit a combination of radial velocity, direct imaging, and Gaia and Hipparcos astrometry. Fitting the direct imaging and radial velocity data for HIP 113201 yields a primary mass of 0.54$\pm$0.03 M$_{\odot}$, fully consistent with its M1 spectral type, and a secondary mass of 0.145$\pm$ M$_{\odot}$. The secondary masses derived with and without including Hipparcos/Gaia data are more massive than the 0.1 M$_{\odot}$ estimated mass from the photometry of the companion. An undetected brown dwarf companion to HIP 113201B could be a natural explanation for this apparent discrepancy. At an age $>$1 Gyr, a 30 M$_{Jup}$ companion to HIP 113201B would make a negligible ($<$1$\%$) contribution to the system luminosity, but could have strong dynamical impacts. Fitting the direct imaging, radial velocity, and Hipparcos/Gaia proper motion anomaly for HIP 36985AB, we find a primary mass of 0.54$\pm$0.01 M$_{\odot}$ and a secondary mass of 0.185$\pm$0.001 M$_{\odot}$ which agree well with photometric estimates of component masses, the masses estimated from $M_{K}$-- mass relationships for M dwarf stars, and previous dynamical masses in the literature.STAMPAenArticle10.1051/0004-6361/2021424382-s2.0-85124705156http://arxiv.org/abs/2112.05457v1https://www.aanda.org/articles/aa/full_html/2022/02/aa42438-21/aa42438-21.html2022A&A...658A.145BFIS/05 - ASTRONOMIA E ASTROFISICA