Notes. The bolometric luminosity (L_bol), envelope mass (M_env), and stellar mass (m_*) are taken from Fedriani et al. (2023). ^(a) The velocity was derived from the 6.7 GHz methanol maser line (Xu et al. 2009). The CO(J = 1−0) spectrum shows a peak around −10 km s⁻¹ (Sugitani et al. 1989). ^(b) No available data for the systemic velocity.^(c) Taken from the RMS Database Server².^(d) Taken from Lundquist et al. (2014).^(e) This source has been categorized as a high-mass protostar (Beuther et al. 2023). The dynamical mass was derived to be ~9 M_⊙ by fitting a Keplerian rotation disk seen in the CH₃CN lines (Cesaroni et al. 2019).^(f) Taken from de A. Schutzer et al. (2022). They considered its luminosity to be 100 L_⊙.^(𝑔) This source was suggested to be between Class 0 and I by Liu et al. (2020), whereas Fiorellino et al. (2023) proposed it to be Class I. ^(h) Taken from Gueth et al. (2001).⁽ⁱ⁾ Taken from Fedriani et al. (2023).^(j) Taken from Palau et al. (2007).^(k) Taken from Lundquist et al. (2014).^(l) Taken from Sánchez-Monge et al. (2010). ^(m) Taken from Molinari et al. (1998). ⁽ⁿ⁾ An alternative distance of 820 pc was used for Cep E by de A. Schutzer et al. (2022), which is based on the measurement of the distance of the Cep OB3b cluster at 819 ± 16 pc by Karnath et al. (2019). Here we have retained the distance that was used in the SOMA SED fitting analysis but acknowledge that, as is typical for most star-forming regions, distances can be uncertain by at least ~10%.^(o) Taken from the SOMA V paper by Telkamp et al. (in prep.).^(p) Obtained from the SED fitting with the same method developed by Fedriani et al. (2023).