Fig. 4
Flux per pixel as a function of wavelength for the v sin i = 1.0 km s-1 and spectral types M0, M3, M6, and M9 (top to bottom panels) spectra at a resolution of 100 000. For comparison, the offset original spectra is presented after smoothing with a boxcar of 2000 pxl (dashed line), a crude approximation of the stellar continuum. Flux units are arbitrary.
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