We present an analysis of 126 new radial velocity measurements from the MAROON-X spectrograph to investigate the TOI-1266 system, which hosts two transiting sub-Neptunes at 10.8 and 18.8 days. We measure masses of $M_{ b}=4.01~\pm~0.55~M_{ \oplus}$ for TOI-1266 b and $M_{ c}=2.00~\pm~0.72~M_{ \oplus}$ for TOI-1266 c. Our mass measurements agree with existing HARPS-N observations which we combined using a weighted average yielding masses for TOI-1266 b, and c of $M_{ b}=4.10~\pm~0.43~M_{ \oplus}$, $M_{ c}=2.4~\pm~0.54~M_{ \oplus}$ respectively. The combined dataset enabled a $\approx30\%$ improvement in mass precision. With bulk densities of $\rho_{ b}$ = 1.25 $\pm$ 0.36 g cm$^{ -3}$ and $\rho_{ c}$ = 1.36 $\pm$ 0.31 g cm$^{ -3}$, the planets are among the lowest density sub-Neptunes orbiting an M dwarf. They are both consistent with rocky cores surrounded by hydrogen helium envelopes. TOI-1266 c may also be consistent with a water-rich composition, but we disfavor that interpretation from an Occam's razor perspective.
Categories: astro-ph.EP
