redback.transient_models.afterglow_models.kilonova_afterglow_redback

redback.transient_models.afterglow_models.kilonova_afterglow_redback(time, redshift, loge0, mej, logn0, logepse, logepsb, p, **kwargs)[source]

Calculate the afterglow emission from a kilonova remnant, following the model of Sarin et al. 2022. This model was modified by Nikhil Sarin following code provided by Ben Margalit.

Parameters:

  • time – time in observer frame (days) in observer frame

  • redshift – source redshift

  • loge0 – log10 of the initial kinetic energy of the ejecta (erg)

  • mej – ejecta mass (solar masses)

  • logn0 – log10 of the circumburst density (cm^-3)

  • logepse – log10 of the fraction of shock energy given to electrons

  • logepsb – log10 of the fraction of shock energy given to magnetic field

  • p – power-law index of the electron energy distribution

  • kwargs – Additional keyword arguments

  • zeta_e – fraction of electrons participating in diffusive shock acceleration. Default is 1.

  • output_format – Whether to output flux density or AB mag

  • frequency – frequency in Hz for the flux density calculation

  • cosmology – Cosmology to use for luminosity distance calculation. Defaults to Planck18. Must be a astropy.cosmology object.

Returns:

flux density or AB mag. Note this is going to give the monochromatic magnitude at the effective frequency for the band. For a proper calculation of the magntitude use the sed variant models.