The mass of TOI-519 b: A close-in giant planet transiting a metal-rich mid-M dwarf

We report on the determination of the mass of TOI-519 b, a transiting substellar object around a mid-M dwarf. We carried out radial velocity measurements using Subaru/InfraRed Doppler (IRD), revealing that TOI-519 b is a planet with a mass of 0.463(-0.088)(+0.082) M-Jup. We also found that the host star is metal rich ([Fe/H] = 0.27 +/- 0.09 dex) and has the lowest effective temperature (T-eff = 3322 +/- 49 K) among all stars hosting known close-in giant planets based on the IRD spectra andmid-resolution infrared spectra obtained withNASA Infrared Telescope Facility/SpeX. The core mass of TOI-519 b inferred from a thermal evolution model ranges from 0 to similar to 30M(circle plus), which can be explained by both core accretion and disk instability models as the formation origins of this planet. However, TOI-519 is in line with the emerging trend that M dwarfs with close-in giant planets tend to have high metallicity, which may indicate that they formed in the core accretionmodel. The system is also consistent with the potential trend that close-in giant planets around M dwarfs tend to be less massive than those around FGK dwarfs.

Automated summary

We determined the mass of TOI-519 b, a substellar object orbiting an M-dwarf star, to be 0.463(-0.088)(+0.082) M-Jup using radial velocity measurements. The host star was found to have high metallicity and the lowest effective temperature among all stars hosting known close-in giant planets. The core mass of TOI-519 b can be explained by both core accretion and disk instability models, and the system is in line with the trend of high metallicity in M dwarfs with close-in giant planets and less massive giant planets around M dwarfs compared to FGK dwarfs.