Notes. It takes t_rise for the recorded luminosity to rise from 5 × 10⁸ L_⊙  to L_bol,max. The parameter Δt_max is the time during which L_bol remains above a tenth of L_bol,max; f_drop is the factor by which L_bol decreases in one day after the time of maximum; gives the time integrated bolometric luminosity from first detection until 15 d later; R_⋆ is the progenitor radius, which corresponds to the RSG surface in the mesa model; M_ejecta and E_kin are the ejecta mass and kinetic energy (without the atmosphere/wind material); H_ρ is the atmospheric scale height in the intermediate region between R_⋆ and the base of the wind; and n_ρ is the exponent of the power law joining this atmosphere and the base of the wind. The next column gives the wind mass loss rate within 2−5 × 10¹⁴ cm; beyond this radius the wind mass loss rate is always set to 10^-6 M_⊙ yr^-1. The subscript “ext” refers to the external material located beyond R_⋆. Its optical depth is below unity before shock breakout (because of its low original temperature, typically below the RSG effective temperature of ~3000 K). Here, we give its optical depth for post-shock breakout conditions, i.e., when H and He are fully ionized (κ = 0.34 cm² g^-1). Numbers in parenthesis represent powers of ten.