Fig. A.1
Spectral-type series for region around Hα. Each normalised spectrum (blue line) is offset by 0.2 in flux density for clarity purposes. The continuumfor each spectrum is marked with a dashed grey line. The position of the line centre is marked with a grey dashed vertical line. While early M dwarfs are typically inactive (showing Hα in absorption), mid- to late-type M dwarfs are typically active, with very variable Hα emission. The shown stars are (same as in Fig. 2): M0.0 V: J03463+262/HD 23453. M0.5 V: J02222+478/BD+ 47 612. M1.0 V: J00051+457/GJ 2. M1.5 V: J02123+035/BD+02 348. M2.0 V: J01013+613/GJ 47. M2.5 V: J00389+306/Wolf 1056. M3.0 V: J02015+637/G 244-047. M3.5 V: J12479+097/Wolf 437. M4.0 V: J01339-176/LP 768-113. M4.5 V: J01125-169/YZ Cet. M5.5 V: J00067-075/GJ 1002. M6.0 V: J14321+081/LP 560-035 M7.0 V: J02530+ 168/Teegarden’s star. M8.0 V: J19169+051S/vB10.
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