Notes. For the same sample as in Table 3, Cols. 2–7 indicate the nUV Balmer excess, the Hα luminosity, the accretion luminosity, the mass accretion rate, the presence of spectro-interferometric evidence indicating a Brγ or Hα emitting region more compact than that for the dust emission (“yes", “no” otherwise), and the SED group classification according to the Meeus et al. (2001) scheme. The main references – not indicated with a superscript – are Fairlamb et al. (2015; Col. 2), the Hα luminosities from Wichittanakom et al. (2020), which have been updated using Gaia EDR3 distances (Col. 3), this work (Cols. 4, 5, see text; and Col. 6 for the first five stars), and GD21 (Col. 7). The rest of the references are ^(a)Mendigutía et al. (2011), ⁽¹⁾Kreplin et al. (2018), ⁽²⁾Kurosawa et al. (2016), ⁽³⁾Kraus et al. (2008), ⁽⁴⁾Caratti o Garatti et al. (2015), ⁽⁵⁾Mendigutía et al. (2015a), ⁽⁶⁾Garcia Lopez et al. (2015), ⁽⁷⁾Mendigutía et al. (2017), ⁽⁸⁾Hone et al. (2019), ⁽⁹⁾Perraut et al. (2016), ⁽¹⁰⁾Malbet et al. (2007), ⁽¹¹⁾Weigelt et al. (2011), ⁽¹²⁾Garcia Lopez et al. (2016), ⁽¹³⁾Tambovtseva et al. (2020), ⁽¹⁴⁾Moura et al. (2020). “…” indicates that the corresponding data are not available. “–” indicates that accretion is considered negligible (see text).