Left: Isotropic-equivalent gamma-ray energies (1 − 10 000 keV; rest frame) of both short (black squares) and long duration (gray circles) GRBs versus redshift (Sakamoto et al. 2011; Lien et al. 2016; Atteia et al. 2017; O’Connor et al. 2024). A population of low-luminosity GRBs is shown with orange pentagons (e.g., Iwamoto et al. 1998; Galama et al. 1998, 1999; Malesani et al. 2004; Sakamoto et al. 2004; Soderberg et al. 2004a,b, 2006; Campana et al. 2006; Ofek et al. 2007; Starling et al. 2011; Cano et al. 2011; D’Elia et al. 2018; Izzo et al. 2019; HESS Collaboration 2021; Dichiara et al. 2022). The approximate energy release (0.5 − 4 keV; rest frame) of the initial EP detection of EP241021a is shown as a red star (Section 2.1; Hu et al. 2024). No bolometric correction has been applied due to the unknown spectral shape at > 4 keV; the presented energy is therefore a lower bound. Downward red arrows indicate the gamma-ray limits for EP241021a from Konus-Wind for gamma-ray emission durations between 3 s (bottom arrow) and 100 s (top arrow). The 1 − 10 000 keV energy release of EP241021a is bounded by these values. For comparison, EP240414a is shown as a blue diamond (0.5 − 4 keV; Sun et al. 2025). Right: Rest-frame X-ray light curves (0.3 − 10 keV) of Swift long GRBs (gray; duration > 2 s) and low-luminosity GRBs (orange; GRBs 060218, 100316D, 171205A, and 190829A) compared with X-ray light curves of EP241021a (taken from Shu et al. 2025) and EP240414a (taken from Sun et al. 2025; van Dalen et al. 2025).