As found by Salim+18, the modified Calzetti law provides a flexible and physically motivated way to describe the diversity of dust attenuation curves observed in galaxies. By adding parameters for the curve’s slope (δ) and UV bump strength (B), they can better match observations, leading to more accurate SFRs, stellar masses, and attenuation estimates. This approach avoids biases from assuming a single Calzetti curve and provides usable attenuation laws for different galaxy populations.
Would it be possible to implement this modified Calzetti attenuation law in the ProSpect code in future versions?
As found by Salim+18, the modified Calzetti law provides a flexible and physically motivated way to describe the diversity of dust attenuation curves observed in galaxies. By adding parameters for the curve’s slope (δ) and UV bump strength (B), they can better match observations, leading to more accurate SFRs, stellar masses, and attenuation estimates. This approach avoids biases from assuming a single Calzetti curve and provides usable attenuation laws for different galaxy populations.
Would it be possible to implement this modified Calzetti attenuation law in the ProSpect code in future versions?