Comparison of posteriors for accretion-to-jet efficiency and application of our model. Left panel: Posteriors for the accretion to jet efficiency for the case of GRB170817A. The green line represents the efficiency derived from ou algorithm, and the red line shows the efficiency from Salafia & Giacomazzo (2021). They both use the kinetic energy distribution from Ghirlanda et al. (2019). The blue line corresponds to the kinetic energy distribution from a strongly magnetized jet from Nathanail et al. (2021). The overplotted points refer to efficiencies from general relativity magnetohydrodynamics simulations. Right panel: Resulting posterior distributions analyzing GRB201221D with our algorithm, assuming an efficiency similar to GRB170817A.