Extended Data Fig. 5: Corner plot showing posterior distributions for the binary-based kilonova model.
From: A kilonova following a long-duration gamma-ray burst at 350 Mpc
The model consists of three ejecta components whose masses, velocities and opacities depend on the chirp mass and binary mass ratio (q) and the fraction of ejecta lost through disk (ε) and magnetic (α) winds. A fraction ζ of the blue (low-lanthanide) ejecta is heated by shocks from the GRB jet over a timescale tshock. The final parameter is a white-noise term for modelling systematics in the data. The labelled 1σ error bars are statistical only; we estimate further systematic error of about 50% on these parameters (see Methods).
