Probing the variability of M dwarf stars using Pan-STARRS

An understanding of M dwarf stars, the most abundant type of star in our Galaxy, are essential to the understanding of our universe. Studying M dwarf flares and variability provides insight into two important fields. First, M dwarf variability can be used to measure the properties of the magnetic fields and chromospheres of the least massive stars. Second, studying flares in these stars serves as a guide for the feasibility of habitability of exoplanets orbiting in the compact habitable zones of low-mass stars. Using data from the medium-deep fields of the Pan-STARRS survey on Mount Haleakala, Hawaii, we have created a large statistical catalog of M0-M9 type stars in the g,r,i,z, and y bands in order to facilitate the study of short time-scale variability of M dwarfs in the time domain. The medium deep survey allows for detailed and sustained observation of the stars, as this area of the sky was imaged about every other night for four years. This paper outlines the method used to identify and classify the M dwarfs from the photometric images obtained of the medium deep fields. The projected statistical sample achieved is about 800,000 M dwarfs of varying class out of a set of about 9,600,000 detected objects in the survey. We will use this catalog to create light curves encompassing about 500 points over 3 years for each M dwarf, facilitating the study of the variability of the star in the time domain