redback.transient_models.tde_models.bpl_cooling_envelope

redback.transient_models.tde_models.bpl_cooling_envelope(time, redshift, peak_time, alpha_1, alpha_2, mbh_6, stellar_mass, eta, alpha, beta, **kwargs)[source]

Full lightcurve, with gaussian rise till fallback time and then the metzger tde model, photometric version where each band is fit/joint separately

Parameters:

  • time – time in observer frame in days

  • redshift – redshift

  • peak_time – peak time in days

  • alpha_1 – power law index for first power law

  • alpha_2 – power law index for second power law (should be positive)

  • mbh_6 – mass of supermassive black hole in units of 10^6 solar mass

  • stellar_mass – stellar mass in units of solar masses

  • eta – SMBH feedback efficiency (typical range: etamin - 0.1)

  • alpha – disk viscosity

  • beta – TDE penetration factor (typical range: 1 - beta_max)

  • kwargs – Additional parameters

  • xi – Optional argument (default set to one) to change the point where lightcurve switches from Gaussian rise to cooling envelope. stitching_point = xi * tfb (where tfb is fallback time). So a xi=1 means the stitching point is at fallback time.

  • 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’, ‘flux’

  • 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’, ‘flux’