0.3–10 keV light curves of the nine CSC2 FXRTs in luminosity units (as in Fig. 16, 0.3–10 keV light curves were converted from 0.5–7 keV ones). The X-ray afterglow light curves of 64 LGRBs plus 32 SGRBs (taken from Bernardini et al. 2012; Lü et al. 2015) are shown as a 2D histogram, as are the X-ray afterglows of GRB 170817A (off-axis SGRB, solid dark green line; Nynka et al. 2018; D’Avanzo et al. 2018; Troja et al. 2020, 2022), SN 2020bvc (the first off-axis LGRB candidate, solid light green line; Izzo et al. 2020), and the ultra-long duration GRB 111209A (solid magenta line, z  =  0.677; Levan et al. 2014). Additionally, several individual transients are overplotted: the low-luminosity supernova SBO XRF 080109/SN 2008D (solid cyan lines, 27 Mpc;), XRF 060218/SN 2006aj (solid blue lines, 145 Mpc;), XRF 100316D/SN 2010bh (solid orange lines, 263 Mpc; Barniol Duran et al. 2015; Starling et al. 2011; Modjaz et al. 2009; Evans et al. 2007, 2009; Soderberg et al. 2008; Campana et al. 2006), the relativistically beamed TDE Swift J1644+57 (solid black lines, z  =  0.3543; Bloom et al. 2011; Levan et al. 2011), the non-beamed TDE J2150-05 (solid pink line, z  =  0.055; Lin et al. 2018), and CDF-S XT2 (solid indigo lines; Xue et al. 2019). For FXRTs 1, 7, 10, 11, 12, and 13 (open symbols), we assume z  =  1.0, we adopt z_photo  =  2.23 for FXRT 14 from Bauer et al. (2017), and for FXRTs 8 and 9 we consider the values from Table 8.