redback.transient_models.afterglow_models.kilonova_afterglow

redback.transient_models.afterglow_models.kilonova_afterglow(time, redshift, umax, umin, loge0, k, mej, logn0, p, logepse, logepsb, ksin, g0, **kwargs)[source]

A kilonova afterglow model from afterglowpy, similar to cocoon but with constraints.

Parameters:

  • time – time in days in observer frame

  • redshift – source redshift

  • umax – initial outflow 4 velocity maximum

  • umin – minimum outflow 4 velocity

  • loge0 – log10 fidicial energy in velocity distribution E(>u) = E0u^-k in erg

  • k – power law index of energy velocity distribution

  • mej – mass of material at umax in solar masses

  • logn0 – log10 number density of ISM in cm^-3

  • p – electron distribution power law index. Must be greater than 2.

  • logepse – log10 fraction of thermal energy in electrons

  • logepsb – log10 fraction of thermal energy in magnetic field

  • ksin – fraction of electrons that get accelerated

  • g0 – initial lorentz factor

  • kwargs – Additional keyword arguments

  • spread – whether jet can spread, defaults to False

  • latres – latitudinal resolution for structured jets, defaults to 2

  • tres – time resolution of shock evolution, defaults to 100

  • spectype – whether to have inverse compton, defaults to 0, i.e., no inverse compton. Change to 1 for including inverse compton emission.

  • q (l0, ts,) – energy injection parameters, defaults to 0

  • 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.