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%% This is a sample manuscript marked up using the
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%% AASTeX is now based on Alexey Vikhlinin's emulateapj.cls 
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\documentclass[twocolumn]{aastex62}

\usepackage{enumitem}
\usepackage{amsmath}

\newcommand{\vdag}{(v)^\dagger}
\newcommand\aastex{AAS\TeX}
\newcommand\latex{La\TeX}


\shorttitle{Magnetic Activity of 53 M-Dwarfs}
\shortauthors{Boudreaux et al.}

\begin{document}

\title{The Ca II H\&K Rotation-Activity Relation in 53 mid-to-late type M-Dwarfs}

\author[0000-0002-2600-7513]{Thomas M. Boudreaux}
\affiliation{Department of Physics and Astronomy, Dartmouth College, Hanover, NH 03755, USA}

\author[0000-0003-4150-841X]{Elisabeth R. Newton}
\affiliation{Department of Physics and Astronomy, Dartmouth College, Hanover, NH 03755, USA}

\author[0000-0003-0295-293X]{Nicholas Mondrik}
\affiliation{Department of Physics , Harvard University , 17 Oxford Street Cambridge MA 02138, USA}

\author[0000-0002-9003-484X]{David Charbonneau}
\affiliation{Center for Astrophysics, Harvard \& Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA}

\author{Jonathan Irwin}
\affiliation{Center for Astrophysics, Harvard \& Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA}

\received{23 September, 2021}
\revised{1 March, 2022}
\accepted{9 March, 2022}



%% Mark off the abstract in the ``abstract'' environment. 
\begin{abstract}
In the canonical theory of stellar magnetic dynamo, the tachocline in partially
	convective stars serves to arrange small-scale fields, generated by
	stochastic movement of plasma into a coherent large-scale field.
	Mid-to-late M-dwarfs, which are fully convective, show more magnetic
	activity than classical magnetic dymano theory predicts. However,
	mid-to-late M-dwarfs show tight correlations between rotation and magnetic
	activity, consistent with elements of classical dynamo theory. We use data
	from Magellan Inamori Kyocera Echelle (MIKE) Spectrograph to detail the
	relation between Ca II H\&K flux and rotation period for these low-mass
	stars. We measure $R'_{HK}$ values for 53 spectroscopically identified
	M-dwarfs selected from the MEarth survey; these stars span spectral classes
	from M5.0 to M3.5 and have rotation periods ranging from hours to months.
	We present the rotation--activity relationship as traced through these
	data. We find power law and saturated regimes consistent to within one
	sigma of previously published results and observe a mass dependence in
	R'$_{HK}$.
\vspace{1cm}
\end{abstract}


\keywords{M dwarf stars (982), Stellar Activity (1580)}

%%%%%%%%%%%%%%%%%
%% INTRODUCTION
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\vspace{1in}
\input{Introduction.tex}

\input{Observations.tex}

\input{Analysis.tex}

\input{Results.tex}

\input{Conclusions.tex}

\acknowledgments{
This work has made use of the NASA Astrophysical Data System. We thank Dan
Kelson for assistance with the \texttt{CarPy} data reduction suite. Additionally, we
would like to thank Zach Berta-Thompson, Brian Chaboyer, and John Thorstensen
for their support. We acknowledge support for an NSF AAPF awarded to Elisabeth
R. Newton (award \# 1602597). This material is based upon work supported by the
National Science Foundation under grant AST-1616624, and by a grant from the
John Templeton Foundation. The opinions expressed in this publication are those
of the authors and do not necessarily reflect the views of the John Templeton
Foundation. N.M. was supported by the National Science Foundation Graduate
Research Fellowship Program, under NSF grant No. DGE1745303. N.M. thanks the
LSSTC Data Science Fellowship Program; his time as a Fellow has greatly
benefited this work. \citep{Leh2021}}


%% If you wish to include an acknowledgments section in your paper,
%% separate it off from the body of the text using the \acknowledgments
%% command.
\acknowledgments

\bibliography{ms}
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\end{document}
