HADES RV Programme with HARPS-N at TNG - IV. Time resolved analysis of the Ca ii H&K and Hα chromospheric emission of low-activity early-type M dwarfs

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Fig. 5

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log (F_{CaII_H}) vs. log (F_{CaII_K}). Different colors represent different stars. The gray dashes show the RMA best fit in Eq. (2). Black crosses represent the typical measurement uncertainties at different activity levels.

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