• Power law Models (multiband_early engine)

powerlaw_post_baseline(times[, t_0, ...])	power law function
powerlaw_full(times[, t_0, amplitude, ...])	power law fits (based on Miller et al, https://ui.adsabs.harvard.edu/abs/2020ApJ...902...47M/abstract), constant (background) before explosion, and power law post explosion.

• Bazin Models (multiband_main engine)

bazin(time, A, t0, tfall, trise, C)	bazin 2009 et al model
bazin1(time, A, t0, tfall)	bazin model part I
bazin2(time, A, t0, trise)	bazin model part II

• Villar Models (multiband_main engine)

villar(time, a, b, t0, t1, tfall, trise, c)

Villar et al 2019 (https://iopscience.iop.org/article/10.3847/1538-4357/ab418c/pdf), function 1

• Piro Models (bol_early engine)

shock_fit(time, Me, Re, Ee[, texp])	shock cooling fit with Piro et al 2020 model (https://arxiv.org/pdf/2007.08543.pdf)
shock_arnett_fit(time, Me, Re, Ee, mni, taum)	shock cooling + Arnett (mni, taum) fit
shock_arnett_mejek_fit(time, Me, Re, Ee, ...)	shock cooling + Arnett (mni, mej, ek) fit

• Arnett Models (bol_main engine)

Arnett_fit_taum(times, m_ni, taum[, texp])	output Arnett bolometric luminosities
taum_to_MejEk(tau_m[, taum_err, k_opt, sntype])	from characteristic time, taum (unit: day) to the product of kinetic energy (unit: foe) and ejecta mass (unit: solar mass), i.e. M$_{ej}^{3/4}$ E$_{kin}^{-1/4}$.
taum_to_Mej_Ek(tau_m, v_ej[, taum_err, ...])	break the degenracy of kinetic energy and ejecta mass, with the help of velocity.
taum_to_Mej_Ek_1(tau_m, v_ej[, taum_err, ...])	break the degenracy of kinetic energy and ejecta mass, with the help of velocity.
Mej_Ek_to_taum(Mej, Ek[, k_opt, sntype])	from kinetic energy (unit: foe) and ejecta mass (unit: solar mass) to taum (unit: day)
Mej_Ek_to_vej(mej, ek)	from kinetic energy (unit: foe) and ejecta mass (unit: solar mass) to photospheric velocity (unit: 10**3 km/s)
Mej_vej_to_Ek(mej, vej)	from ejecta mass (unit: solar mass) and photospheric velocity (unit: 10**3 km/s) to kinteic energy (unit: foe)
Arnett_fit_Mej_Ek(times, f_ni, Ek, Mej[, ...])	fit Arnett model with Ek (unit: foe), Mej (unit: solar mass),

• Tail Models (bol_tail engine)

tail_fit_t0(t, mni, t0)	fit radioactive tail with Wygoda 2019 Eq 10, 11 and 12 (https://arxiv.org/pdf/1711.00969.pdf)
t0_to_Mej_Ek(...)	from tail characteristic time, t0 to kinetic energy and ejecta mass seperately t0 = sqrt(c*kgamma*Mej**2/Ekin) vej = sqrt(2*Ekin/Mej)
Mej_Ek_to_t0(Mej, Ek[, k_gamma])	from kinetic energy and ejecta mass to t0
tail_fit_Mej_Ek(times, f_ni, Ek, Mej[, k_gamma])	fit tail model on Ek, Mej, with photospheric velocity, vm as free parameter as well

• Arnett+Tail Models (bol_full engine)

joint_fit_taum_t0(times, mni, taum, t0, ts)	for the full range, Arnett_fit_taum fit + tail_fit_t0 fit, with ts as free parameter
joint_fit_Mej_Ek(times, mni, Mej, Ek, ts[, ...])	for the full range, Arnett_fit_Mej_Ek fit + tail_fit_Mej_Ek fit, with ts as free parameter

• Gaussian Models (specline engine)

gauss(x, H, A, x0, sigma)	gaussian function
double_gauss(x, H, A1, x01, sigma1, A2, x02, ...)	double gaussian function

• Voigt Models (specline engine)

voigt(x, H, A, x0, sigma, gamma)

voigt function

• Exponential Models (specv_evolution engine)

exp(t, a, b, c)

exponential function