The optical-infrared relation for active galactic nuclei: The role of contaminations

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Table 1.

CIGALE modules and input parameters used for all the fits.

Parameter	Symbol	Range
Delayed star formation history and recent burst

Age of the main population	age_main	4000.0, 6000.0, 9000.0, 12 000.0 Myr
e-folding timescale of the delayed SFH	τ	3500.0, 7500.0 Myr
Age of the burst	age_burst	100.0, 300.0 Myr
Burst stellar mass fraction	fburst	0.0, 0.01, 0.1, 0.3

Dust attenuation based on Charlot & Fall (2000)

V-band attenuation in the ISM	$A_{V}^{ISM}$ $Mathematical equation: $ A^{\mathrm{ISM}}_{V} $$	0.01, 0.3, 0.7, 1.5
Power-law slope of dust attenuation in the BCs	n_BC	−0.7
$A_{V}^{ISM} / (A_{V}^{ISM} + A_{V}^{BC})$ $Mathematical equation: $ A^{\mathrm{ISM}}_{V}/(A^{\mathrm{ISM}}_{V}+A_{V}^{\mathrm{BC}}) $$	μ	0.6, 0.44, 0.2
Power-law slope of dust attenuation in the ISM	n_ISM	−1.3, −0.7, −0.48, −0.2

Dust emission Dale et al. (2014) model

Alpha	α	2.0, 2.5, 3.25

AGN Skirtor Stalevski et al. (2016) model⁽¹⁾

AGN fraction	f_AGN	0.7, 0.75, 0.85, 0.9, 0.95, 0.99
Opening angle	Δ	10, 20, 40, 60, 70
Inclination	i	10, 20, 40, 60, 80
Color excess of the polar dust	E(B − V)_pd	0.0, 0.03, 0.1, 0.15, 0.25, 0.3 (0 for the fit without PD)
Temperature of the polar dust	T_pd	100.0, 500.0, 1500.0
Average edge-on optical depth at 9.7 micron	t	7, 11

Notes.

⁽¹⁾

For the fit without polar dust the E(B − V)_pd was set only to 0.

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