redback.transient_models.supernova_models.csm_shock_and_arnett_two_rphots

redback.transient_models.supernova_models.csm_shock_and_arnett_two_rphots(time, redshift, mej, f_nickel, csm_mass, v_min, beta, shell_radius, shell_width_ratio, kappa, **kwargs)[source]

Assumes CSM interaction for a shell-like CSM with a hard outer boundary and arnett model for radioactive decay. Assumes the photospheres for the CSM-interaction and the Arnett model are different.

Parameters:

  • time – time in days in observer frame

  • redshift – source redshift

  • mej – ejecta mass in solar masses

  • f_nickel – fraction of nickel mass

  • csm_mass – csm mass in solar masses

  • v_min – ejecta velocity in km/s

  • beta – velocity ratio in c (beta < 1)

  • shell_radius – radius of shell in 10^14 cm

  • kappa – opacity

  • shell_width_ratio – shell width ratio (deltaR/R0)

  • kwargs – kappa_gamma, temperature_floor, and any kwarg to change any other input physics/parameters from default.

  • frequency – Required if output_format is ‘flux_density’. frequency to calculate - Must be same length as time array or a single number).

  • bands – Required if output_format is ‘magnitude’ or ‘flux’.

  • output_format – ‘flux_density’, ‘magnitude’, ‘spectra’, ‘flux’, ‘sncosmo_source’

  • lambda_array – Optional argument to set your desired wavelength array (in Angstroms) to evaluate the SED on.

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

Returns:

set by output format - ‘flux_density’, ‘magnitude’, ‘spectra’, ‘flux’, ‘sncosmo_source’