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A Reanalysis of the UVES M Dwarf Planet Search Program

• Authors: R. P. Butler, H. R. A. Jones, F. Feng, M. Tuomi, G. Anglada-Escudé, and Sandy Keiser

2019 The Astronomical Journal 158 251.

• Provider: AAS Journals

Caption: Figure 4.

Probabilistic detection limits for the new UVES data of 34 M dwarfs. The N statistically significant signals found in a given data set are denoted by the red circles. The gray region in each panel shows the probabilistic detection limit, which is defined by the 50% quantile of the posterior distribution of semi-amplitude (K50%) and the maximum of semi-amplitude Kmax in the posterior samples for the N + 1 signal. The habitable zone denoted by dashed lines is calculated using the method introduced by Kopparapu et al. (2014). The blue horizontal line represents the 10 M limit.