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

Author:

Cale Bryson L.ORCID,Reefe Michael,Plavchan PeterORCID,Tanner Angelle,Gaidos EricORCID,Gagné JonathanORCID,Gao PeterORCID,Kane Stephen R.ORCID,Béjar Víctor J. S.ORCID,Lodieu NicolasORCID,Anglada-Escudé Guillem,Ribas IgnasiORCID,Pallé EnricORCID,Quirrenbach Andreas,Amado Pedro J.,Reiners Ansgar,Caballero José A.,Rosa Zapatero Osorio María,Dreizler Stefan,Howard Andrew W.ORCID,Fulton Benjamin J.ORCID,Xuesong Wang Sharon,Collins Kevin I.ORCID,El Mufti Mohammed,Wittrock JustinORCID,Gilbert Emily A.ORCID,Barclay ThomasORCID,Klein Baptiste,Martioli Eder,Wittenmyer RobertORCID,Wright DuncanORCID,Addison BrettORCID,Hirano TeruyukiORCID,Tamura MotohideORCID,Kotani Takayuki,Narita NorioORCID,Vermilion David,Lee Rena A.,Geneser Claire,Teske Johanna,Quinn Samuel N.ORCID,Latham David W.ORCID,Esquerdo Gilbert A.ORCID,Calkins Michael L.ORCID,Berlind Perry,Zohrabi Farzaneh,Stibbards Caitlin,Kotnana Srihan,Jenkins JonORCID,Twicken Joseph D.ORCID,Henze Christopher,Kidwell Richard,Burke ChristopherORCID,Villaseñor Joel,Boyd PatriciaORCID

Abstract

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 ∼ 8.46 days, R b = 4.38 0.18 + 0.18 R , P c ∼ 18.86 days, R c = 3.51 0.16 + 0.16 R . With visible RVs from Calar Alto high-Resolution search for M dwarfs with Exo-earths with Near-infrared and optical echelle Spectrographs (CARMENES)-VIS, CHIRON, HARPS, HIRES, Minerva-Australis, and Tillinghast Reflector Echelle Spectrograph, as well as near-infrared (NIR) RVs from CARMENES-NIR, CSHELL, IRD, iSHELL, NIRSPEC, and SPIRou, we provide a 5σ upper limit to the mass of AU Mic c of M c ≤ 20.13 M and present a refined mass of AU Mic b of M b = 20.12 1.57 + 1.72 M . 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 multiwavelength Gaussian process model, we demonstrate the ability to recover injected planets at 5σ significance with semi-amplitudes down to ≈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 ∼50% for such signals with our model.

Funder

National Aeronautics and Space Administration

National Science Foundation

Mt. Cuba Astronomical Foundation

Publisher

American Astronomical Society

Subject

Space and Planetary Science,Astronomy and Astrophysics

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