Stellar chromospheric activity database of solar-like stars based on the LAMOST Low-Resolution Spectroscopic Survey - II. The bolometric and photospheric calibration

Open Access

Fig. A.2

Scatter plot of log R′_HK,PHOENIX (T_eff,LASP) versus log R′_HK,PHOENIX (T_eff,A2020) for stars in Figure A.1. Error bars are displayed for data points with known uncertainty values. The dashed red line represents the ratio of $\frac{\log R_{H K, P H O E N I X}^{'} (T_{e f f, L A S P})}{\log R_{H K, P H O E N I X}^{'} T_{e f f, A 2020})} = 1 .$ $\[\frac{\log R_{\mathrm{HK}, \mathrm{PHOENIX}}^{\prime}\left(T_{\mathrm{eff}, \mathrm{LASP}}\right)}{\left.\log R_{\mathrm{HK}, \mathrm{PHOENIX}}^{\prime} T_{\mathrm{eff}, \mathrm{A} 2020}\right)}=1.\]$ . The lower panel shows the distribution of Δ log R′_HK,PHOENIX against log R′_HK,PHOENIX (T_eff,LASP).

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