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tokens: 2013 ) and radial velocities (Saar Donahue 1997 ; Korhonen et al. 2015 ). Stellar activity has even been the culprit behind false detections of exoplanets around M dwarfs in high-precision data (Robertson et al. 2014 ). The role of M dwarf magnetic activity on planetary habitability, particularly from X-ray and UV flux due to quiescent emission and flares, is an ongoing area of research (Scalo et al. 2007 ; Tarter et al. 2007 ; Seager Deming 2010 ). Planetary habitability is impacted by the properties and evolution of both the star and planet (e.g., Vidotto et al. 2013 ). While models from Segura et al. ( 2010 ) show that single large M dwarf flares do not pose a great risk to planetary habitability, young planets may be bombarded with much stronger and more frequent flares than previously predicted (Armstrong et al. 2016 ). M dwarf activity can strongly affect planetary atmospheres through photoevaporation on Gyr timescales (Cuntz Guinan 2016 ; Owen Mohanty 2016 ). Whether this has a net positive or negative impact on atmosphere loss and planetary habitability is debated (Luger et al. 2015 ; Owen Mohanty 2016 ). Accurate studies of M dwarf magnetic activity in X-rays, UV, and the blue optical are challenging due to the intrinsic faintness of these cool stars at short wavelengths. However, the nearest M dwarf to the Sun, Proxima Cen, has long been known as an active flare star (Thackeray 1950 ), with a moderately strong magnetic field for its spectral type of M5.5 (Reiners Basri 2008 ). At a distance of 1.3 pc, Proxima Cen enables unique characterization of activity in X-ray through optical (Güdel et al. 2004 ; Fuhrmeister et al. 2011 ), and even radio frequencies (Lim et al. 1996 ). High time resolution flare data from Proxima Cen has been used to better understand flare heating mechanisms (Reale et al. 2004 ; Kowalski et al. 2016 ). Decades-long spectroscopic monitoring has even revealed a possible activity cycle for Proxima Cen (Cincunegui et al. 2007 ). Proxima Cen has been the subject of multiple searches for exoplanets (e.g., Benedict et al. 1999 ; Endl Kürster 2008 ). Recently, Anglada-Escudé et al. ( 2016 ) discovered the existence of Proxima b, a 1.27 M ⊕ planet orbiting within the star’s habitable zone, using multiple years of high-precision radial velocity monitoring. Proxima Cen is therefore an important benchmark object for understanding planet formation around low-mass stars, the evolution of the magnetic dynamo, and the impact of stellar activity on planetary atmospheres. Using data from the Microvariability and Oscillations of STars microsatellite (hereafter MOST ; Walker et al. 2003 ), we have conducted a study of the white-light flares from Proxima Cen. Flares have previously been studied with MOST for the famous active M3.5 dwarf, AD Leo (Hunt-Walker et al. 2012 ). Despite its long history of study as an active M dwarf, the census of flares from Proxima has not been constrained by modern space-based photometric studies.