Diving Beneath the Sea of Stellar Activity: Chromatic Radial Velocities of the Young AU Mic Planetary System

Abstract

We present updated radial-velocity (RV) analyses of the AU Mic system. AU Mic is a young (22 Myr) early M dwarf known to host two transiting planets - $P_b\sim 8.46$ days, $R_b=4.38_{-0.18}^{+0.18}{R}_{\oplus }$, $P_c\sim 18.86$ days, $R_c=3.51_{-0.16}^{+0.16}{R}_{\oplus }$. With visible RVs from CARMENES-VIS, CHIRON, HARPS, HIRES, {\sc {\textsc{Minerva}}}-Australis, and TRES, as well as near-infrared (NIR) RVs from CARMENES-NIR, CSHELL, IRD, iSHELL, NIRSPEC, and SPIRou, we provide a $5\ddot{I}ƒ$ upper limit to the mass of AU Mic c of $M_c\le 20.13M_{\oplus }$ and present a refined mass of AU Mic b of $M_b=20.12_{-1.57}^{+1.72}{M}_{\oplus }$. Used in our analyses is a new RV modeling toolkit to exploit the wavelength dependence of stellar activity present in our RVs via wavelength-dependent Gaussian processes. By obtaining near-simultaneous visible and near-infrared RVs, we also compute the temporal evolution of RV-``color'' and introduce a regressional method to aid in isolating Keplerian from stellar activity signals when modeling RVs in future works. Using a multi-wavelength Gaussian process model, we demonstrate the ability to recover injected planets at $5\ddot{I}ƒ$ significance with semi-amplitudes down to $\approx$ 10\,m\,s${}^{-1}$ with a known ephemeris, more than an order of magnitude below the stellar activity amplitude. However, we find that the accuracy of the recovered semi-amplitudes is $\sim$50\% for such signals with our model.