tokens: not trivial, the main obstacle being the lack of robust estimates for key parameters (e.g., distance, Doppler factor), as well as the lack of contemporaneous multi-wavelength radio observations. In most cases, the range of available frequencies was confined in the lower frequency range (43 GHz). The observed flux density at higher frequencies was the result of extrapolation by assuming that the spectral index derived from the highest available frequencies of each microquasar remains constant up to 142.33 GHz (which is the highest available frequency for the supermassive BH sample). To estimate the relativistic boosting and revert to the rest frame, we gathered for each source all available estimates in the literature for the velocity of the jet, distance, and viewing angle (Table 1 ). For each source, we created a parameter space set by the extrema of the aforementioned quantities. We then uniformly drew a random value for each of these parameters and calculated . We repeated this process 10 4 times and calculated the mean and spread (minimum, maximum) of for each source. The y -values for the microquasars in Figure 3 are the mean, and the y -axis errorbars the spread for each of the sources that resulted from the random sampling. We follow a similar procedure for the , by gathering all the available estimates in the literature and calculating the mean and spread. The x -values for the microquasars in Figure 3 are the mean, and the x -axis errorbars are the spread for each of the sources. The microquasars, parameter ranges, and the references to them are the following. For SS 433. we used radio data from Trushkin et al. ( 2003 ), and parameter values from Seward et al. ( 1980 ), Fender ( 2001 ), Trushkin et al. ( 2003 ), Bowler ( 2010 ), Panferov ( 2010 ), Cherepashchuk et al. ( 2013 ), and references therein. For GRS 1915+105, we used radio data from Rodriguez et al. ( 1995 ), and parameter values from Mirabel Rodríguez ( 1994 ), Fender ( 2001 , 2003 ), Fender Belloni ( 2004 ), Miller-Jones et al. ( 2005 ), Punsly ( 2011 ), Reid et al. ( 2014 ), Zdziarski ( 2014 ), Punsly Rodriguez ( 2016 ), and references therein. For Cyg X-3, we used radio data from Koljonen et al. ( 2010 ), and parameter values from Fender et al. ( 1997 ), Ling et al. ( 2009 ), Hjalmarsdotter et al. ( 2009 ), Vilhu et al. ( 2009 ), Dubus et al. ( 2010 ), Vilhu Hannikainen ( 2013 ), Zdziarski et al. ( 2012 , 2013 , 2016 ), and references therein. For GRO J1655-40, we used radio data from Hannikainen et al. ( 2000 ), and parameter values from Hannikainen et al. ( 2000 ), Trushkin ( 2000 ), Mirabel et al. ( 2002 ), Fender ( 2003 ), Fender et al. ( 2004 , 2010 ), Narayan McClintock ( 2005 ), Motta et al. ( 2014 ), Stuchlík Kološ ( 2016 ), and references therein. For V* V404 Cyg, we used radio data from Gallo et al. ( 2005 ), and parameter values from Cherepashchuk et al. 2004 , Heinz Merloni ( 2004 ), Miller-Jones et al. ( 2009 ), Khargharia et al. ( 2010 ), Xie et al. ( 2014
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