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Table B.1.

CIGALE modules and input parameters used for all the fits. BC03 means Bruzual & Charlot (2003), and the Chabrier IMF refers to Chabrier (2003).

Parameters Symbol Run #1 Run #2
Target sample 173 NIRSpec-observed objects 173 NIRSpec-observed objects
Delayed SFH and recent burst

e-folding time scale of the delayed SFH τmain [Myr] 500

Age of the main population Agemain[Myr] 2, 5, 10, 25, 50, 250, 500, 1000

e-folding time scale of the delayed SFH τburst [Myr] 10000

Age of the young population Ageburst[Myr] 1

Periodic SFH

Type of the individual star formation episodes delayed

Elapsed time between the beginning of each burst δburst [Myr] 10, 50, 100, 250

e-folding time scale of the delayed SFH τburst [Myr] 10, 100

Age of the episodes Age [Myr] 1, 5, 10, 50, 100, 200, 400, 600, 800, 1000

SSP

SSP BC03 BC03

Initial mass function IMF Chabrier Chabrier

Metallicity Z 0.0001, 0.0004, 0.004, 0.008, 0.02, 0.05 0.0001, 0.0004, 0.004, 0.008, 0.02, 0.05

Nebular emission

Ionization parameter logU -1.0, -1.2, -1.4, -1.6, -1.8, -2.0, -2.2, -2.4, -2.6, -2.8, -3.0, -3.2, -3.4, -3.6, -3.8, -4.0 -1.0, -1.2, -1.4, -1.6, -1.8, -2.0, -2.2, -2.4, -2.6, -2.8, -3.0, -3.2, -3.4, -3.6, -3.8, -4.0

Gas metallicity Zgas 0.0001, 0.0004, 0.001, 0.002, 0.0025, 0.003, 0.004, 0.005 0.0001, 0.0004, 0.001, 0.002, 0.0025, 0.003, 0.004, 0.005

Electron density nH 10, 100, 1000 10, 100, 1000
Line width [km/s] 150 150

Dust attenuation law

Color excess for both the old and young stellar populations E_BV_lines 1e-4, 0.001, 0.010, 0.050, 0.10, 0.15, 0.20, 0.25, 0.30, 0.50, 0.75, 1.0, 1.5, 2.0, 3.0, 5.0 1e-4, 0.001, 0.010, 0.050, 0.10, 0.15, 0.20, 0.25, 0.30, 0.50, 0.75, 1.0, 1.5, 2.0, 3.0, 5.0

Reduction factor to apply on E_BV_lines to compute E(B-V)s the stellar continuum attenuation. E_BV_factor 0.44 0.44

Bump amplitude uv_bump_amplitude 0.0 0.0

Power law slope power law_slope -0.6, -0.30, 0.0, 0.30, 0.6 -0.6, -0.30, 0.0, 0.30, 0.6

Dust emission (DL2014)

Mass fraction of PAH qPAH 0.47 0.47

Minimum radiation field Umin 17.0 17.0

Power law slope dU/dM ≈ Uα α 2.4 2.4

Dust fraction in PDRs γ 0.54 0.54

No AGN emission

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