Most massive stellar mass to embedded cluster mass (m_str,max–M_ecl) relation. The optimally sampled results for the most, second, and third massive star mass as a function of embedded cluster mass are shown as a solid curve, blue dashed curve, and green dotted curve, respectively. Observational data come from Kirk & Myers (2012; orange dots), Stephens et al. (2017; red dots), Weidner et al. (2013a; gray dots), and Ramírez Alegría et al. (2016; blue dots), where Weidner et al. (2013a) is an inhomogeneous set of data culled from the literature for very young clusters without supernova remnants. The average M_ecl uncertainty is 0.34 dex; the average m_str,max uncertainty, 0.16 dex, is indicated by gray dots and light gray indicates data points with larger uncertainties. The thin solid line indicates the M_ecl = m_str,max limit and the horizontal thin dashed line indicates the 150 M_⊙ limit in our Eq. (4).