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Fig. 4


Photometric colours of main sequence stars, for different effective temperatures, from Pecaut & Mamajek (2013). Red lines represent the spline approximation for each curve. The temperature for a given colour is computed as the root of the (m1m2) − (m1,⋆m2,⋆) curve, wherem1m2 is the chosencolour, and m1,⋆, m2,⋆ are the star’s colours.

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