# Double-lined M dwarf eclipsing binaries from Catalina Sky Survey and LAMOST

## TL;DR

This study identifies and characterizes three faint M2-M3 type double-lined eclipsing binaries using data from Catalina Sky Survey, LAMOST, and Gemini North, providing precise stellar parameters to improve low-mass stellar models.

## Contribution

First detailed mass and radius measurements of faint M dwarf eclipsing binaries from combined photometric and spectroscopic data.

## Key findings

- Derived stellar masses between 0.28-0.42 M_sun.
- Derived stellar radii between 0.29-0.67 R_sun.
- Provided benchmarks for low-mass stellar models.

## Abstract

Eclipsing binaries provide a unique opportunity to determine fundamental stellar properties. In the era of wide-field cameras and all-sky imaging surveys, thousands of eclipsing binaries have been reported through light curve classification, yet their basic properties remain unexplored due to the extensive efforts needed to follow them up spectroscopically. In this paper we investigate three M2-M3 type double-lined eclipsing binaries discovered by cross-matching eclipsing binaries from the Catalina Sky Survey wtih spectroscopically classified M dwarfs from the Large Sky Area Multi-Object Fiber Spectroscopic Telescope survey data release one and two. Because these three M dwarf binaries are faint, we further acquire radial velocity measurements using GMOS on the Gemini North telescope with R~40000, enabling us to determine the mass and radius of individual stellar components. By jointly fitting the light and radial velocity curves of these systems, we derive the mass and radius of the primary and secondary components of these three systems, in the range between 0.28-0.42 M_sun and 0.29-0.67 R_sun, respectively. Future observations with a high resolution spectrograph will help us pin down the uncertainties in their stellar parameters, and render these systems benchmarks to study m dwarfs, providing inputs to improving stellar models in the low mass regime, or establishing an empirical mass-radius relation for M dwarf stars.