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Deriving Stellar Inclination of Slow Rotators Using Stellar Activity

  • Authors: X. Dumusque

Dumusque 2014 The Astrophysical Journal 796 133.

  • Provider: AAS Journals

Caption: Figure 7.

Marginalized posterior distributions returned by our MCMC fit to the data of α Cen B. The mode (black thick line) of the distribution for each parameter, with its 1σ uncertainty (purple shaded regions delimited by red dashed lines) and 2σ uncertainty (delimited by green thin lines) can be found on each plot. The title of each plot gives the value for the mode of the distribution and its 1σ uncertainty.

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