Notes. Their stellar luminosity, mass, K-band magnitude, distance, and presence of the CO bandheads are also listed. For the four MYSOs that are highly embedded and therefore do not have available Gaia parallaxes, the bolometric luminosity, K-band magnitude, and distance are taken from the RMS database. It is found that for massive objects, the stellar luminosity dominates the total luminosity (e.g. Herbig AeBes Fairlamb et al. 2015, ~10%). Therefore, we assume that the bolometric luminosity can be represented by the stellar luminosity for these four sources. The mass is extrapolated following the methods adopted for main sequence objects (Martins et al. 2005). ^(⋆)We note that masses derived with this approach come with a high uncertainty of 35–50%. ^(†)The properties of those sources are based on kinematic distances with a typical uncertainty of 1.0 kpc, while the typical uncertainty on the reported luminosities is 34% Mottram et al. (2011). ^(a)Also known as PDS 37. ^(b)Also known as PDS 27. ^(c)These are the only two MYSOs in this sample with available and reliable measured parallaxes and stellar properties using Gaia (EDR3, DR2; Guzmán-Díaz et al. 2021; Wichittanakom et al. 2020).