Analysis of galaxy spectral energy distributions from far-UV to far-IR with CIGALE: studying a SINGS test sample

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Volume 507 / No 3 (December I 2009)

A&A, 507 3 (2009) 1793-1813

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Table 1:

Description of the output parameters of *CIGALE*.
Par.	Unit	Description	Dependencies
Z	--	metallicity ( ${Z}_\odot = 0.02$ )	basic
$\tau _{\rm oSP}$	Gyr	e-folding time for	basic
		old SP model
$t_{{\rm oSP}}$	Gyr	age of old SP model	basic
$\tau _{\rm ySP}$	Gyr	e-folding time for	basic
		young SP model
$t_{{\rm ySP}}$	Gyr	age of young SP model	basic
$f_{\rm burst}$	--	mass fraction of	basic
		young SP model
$t_{{\rm M}}$	Gyr	mass-weighted age	dep. on SP par.
$t_{{\rm D4000}}$	Gyr	D4000-related age	dep. on SP par.
$\lambda_0$	Å	central wavelength of	basic
		UV bump
$\gamma$	Å	FWHM of UV bump	basic
$E_{\rm bump}$	--	amplitude of UV bump	basic
$c_{\rm R}$	--	change of R_V	basic
$\delta$	--	slope correction of	basic
		Calzetti law
$A_{V,{\rm ySP}}$	mag	V-band attenuation	basic
		for young SP model
$f_{\rm att}$	--	reduction of A_V	basic
		for old SP model
$A_{\rm FUV}$	mag	attenuation at 1500 Å	dep. on SP and
			attenuation par.
A_V	mag	attenuation at 5500 Å	dep. on SP and
			attenuation par.
$\alpha$	--	slope of IR model	basic
$N_{\rm AGN}$	--	number of AGN model	basic
$f_{\rm AGN}$	--	$L_{\rm dust}$ fraction of	basic
		AGN model
$N_{\rm emlin}$	--	template number for	dep. on SP and
		optical lines	attenuation par.
$N_{\rm abslin}$	--	template number for	dep. on SP and
		UV lines	attenuation par.
$M_{\rm gal}$	$M_\odot$	galaxy mass	scaling par.
$M_{\rm star}$	$M_\odot$	total stellar mass	dep. on SP par.
			and $M_{\rm gal}$
SFR	$M_\odot$ /yr	instantaneous SFR	dep. on SP par.
			and $M_{\rm gal}$
$L_{\rm bol}$	$L_\odot$	bolometric luminosity	dep. on all basic
			par. and $M_{\rm gal}$
$L_{\rm dust}$	$L_\odot$	dust luminosity	dep. on all basic
			par. and $M_{\rm gal}$

Source LaTeX | All tables | In the text

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