Notes. The first four columns display the G, Bp, Rp, and K photometric colours from Gaia and 2MASS; the two following columns indicate the luminosity (L_⋆) and effective temperature (T_eff); the next three show the parallax (p) with its error (σ_ϖ) in mas and in AU; the last column reports the pulsation period (P_puls). ^(a) Gaia DR2 (Gaia Collaboration 2018) ^(b) 2MASS (Skrutskie et al. 2006) ^(c) Computed from K2MASS with a bolometric correction of 3.0 ^(d)The temperatureis based on Gaia Bp/Rp photometric colours and was estimated for sources brighter than G = 17 mag for 3000 K < T_eff < 10 000 K. Due to the degeneracy of the photometric temperature with interstellar extinction, an empirically trained machine learning algorithm was used forexternal spectroscopic datasets in low-extinction regions in order to derive temperatures (Andrae et al. 2018). However, due to the limited training set for cool stars, photometric temperatures have to be taken with extreme caution for these stars. ^(e) Jura et al. (1993).