Comparison of the E_B−V derived in this work and the E_B−V from the 3D map of Green et al. (2019). We only consider stars with reliable Gaia parallax measurements (﹩\varpi /{\sigma }_{\varpi }\gt 5﹩). For stars without emission lines, the mean and dispersion of the E_B−V difference are 0.04 mag and 0.09 mag, respectively, whereas for stars with emission lines in the spectra we find a shifted mean of 0.11 mag and a standard deviation of 0.13 mag. The larger E_B−V for stars with emission lines indicates that these stars are more extincted by the associated H II regions or by their surrounding gas and dust.