Physical properties of strong 1 < z < 3 Balmer and Paschen line emitters observed with JWST

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Volume 689 (September 2024)

A&A, 689 (2024) A102

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Table 4.

CIGALE modules and input parameters.

Parameter	Symbol	Range

Delayed SFH
Age of the main population	age_main	2000, 3000, 4000, 5000
e-folding timescale of the delayed SFH	τ_main	500, 2000, 5000, 8000
Age of the burst	age_burst	10, 20, 50, 100
Burst stellar mass fraction	f_burst	0.0, 0.1, 0.15, 0.2

Dust attenuation

V-band attenuation in the ISM	$A_{V}^{ISM}$ $A_{\mathrm{V}}^{\mathrm{ISM}}$	0 to 1.6 with 0.1 bins
$A_{V}^{ISM}$ $A_{\mathrm{V}}^{\mathrm{ISM}}$ / ( $A_{V}^{ISM}$ $A_{\mathrm{V}}^{\mathrm{ISM}}$ + $A_{V}^{BC}$ $A_{\mathrm{V}}^{\mathrm{BC}}$ )	μ	0 to 1.0 with 0.1 bins
Power-law slope of dust attenuation in the BCs	n^BC	0.7, 1.0, 1.3
Power-law slope of dust attenuation in the ISM	n^ISM	0.4 to 1.5 with 0.1 bins

Dust emission

Mass fraction of PAHs	q_PAH	0.47, 1.12, 3.90
Minimum radiation field	U_min	1.0, 5.0, 10.0
Fraction illuminated	γ	0.02, 0.05, 0.1

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