J/A+A/624/A80 DustPedia SED fitting results (Nersesian+, 2019)
Old and young stellar populations in DustPedia galaxies and their role in
dust heating.
Nersesian A., Xilouris E.M., Bianchi S., Galliano F., Jones A.P., Baes M.,
Casasola V., Cassara L.P., Clark C.J.R., Davies J.I., Decleir M.,
Dobbels W., De Looze I., De Vis P., Fritz J., Galametz M., Madden S.C.,
Mosenkov A.V., Trcka A., Verstocken S., Viaene S., Lianou S.
<Astron. Astrophys. 624, A80 (2019)>
=2019A&A...624A..80N 2019A&A...624A..80N (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Galaxies, IR ; Galaxies, photometry ; Models ;
Energy distributions
Keywords: dust; extinction - infrared: galaxies - galaxies: photometry -
galaxies: ISM - galaxies: evolution
Abstract:
Within the framework of the DustPedia project we investigate the
properties of cosmic dust and its interaction with stellar radiation
(originating from different stellar populations) for 814 galaxies in
the nearby Universe, all observed by the Herschel Space Observatory.
We take advantage of the widely used fitting code CIGALE, properly
adapted to include the state-of-the-art dust model THEMIS. For
comparison purposes, an estimation of the dust properties is provided
by approximating the emission at far-infrared and sub-millimeter
wavelengths with a modified blackbody. Using the DustPedia photometry
we determine the physical properties of the galaxies, such as the dust
and stellar mass, the star-formation rate, the bolometric luminosity,
the unattenuated and the absorbed by dust stellar light, for both the
old (>200Myr) and young (≤200Myr) stellar populations. We show how
the mass of stars, dust, and atomic gas, as well as the star-formation
rate and the dust temperature vary between galaxies of different
morphologies and provide recipes to estimate these parameters given
their Hubble stage (T). We find a mild correlation between the mass
fraction of the small a-C(:H) grains with the specific star-formation
rate. On average, young stars are very efficient in heating the dust,
with absorption fractions reaching as high as 77% of the total
unattenuated luminosity of this population. On the other hand, the
maximum absorption fraction of old stars is 24%. Dust heating in
early-type galaxies is mainly due to old stars, up to a level of 90%.
Young stars progressively contribute more for typical spiral galaxies
and they become the dominant source of dust heating for Sm-type and
irregular galaxies, with 60% of their luminosity contributing to that
purpose. Finally, we find a strong correlation of the dust heating
fraction by young stars with morphology and the specific
star-formation rate.
Description:
We make use of the SED fitting code CIGALE to model and interpret the
SEDs of 814 DustPedia galaxies. The code fits the multi-wavelength
spectrum (UV-submm) of each galaxy in order to derive global
properties such as the star-formation rate (SFR), the stellar mass,
the bolometric luminosity as well as the absorbed by dust luminosity,
the minimum intensity value of the stellar radiation field and the
dust mass. The stellar component is described by providing the
relative contribution of both the young and the old stellar components
to the total SED of the galaxy. We fitted the dust emission using
THEMIS dust model. For comparison purposes, we performed an additional
fitting run with CIGALE using the widely adopted model by Draine and
Li, 2007ApJ...657..810D 2007ApJ...657..810D (updated in Draine et al. 2014ApJ...780..172D 2014ApJ...780..172D;
DL14). The parameter grid is the same as in the case of THEMIS (See
Section 3.1.2 in the paper), with only the polycyclic aromatic
hydrocarbon (PAH) abundance substituting the mass fraction of small
hydrocarbon solids (a-C(:H)). The small a-C(:H) component has the same
effect as the PAH component in the DL14 model; the only difference
should be a scaling factor of 2.2 between the two quantities. We
approximate the dust temperature using the strength of the
interstellar radiation field parametrized by the minimum intensity
value of the stellar radiation field. The global galaxy properties
derived with CIGALE using THEMIS dust model are given in the
themis.dat file, whereas the properties obtained by using the DL14
model are given in the dl14.dat file. Finally, we provide a catalog
with the global dust properties of the DustPedia galaxies by fitting a
single temperature modified black body to the FIR SED (mbb.dat).
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
dl14.dat 302 875 DustPedia cigale results obtained by using
the DL14 model
themis.dat 302 875 DustPedia cigale results derived with CIGALE
using THEMIS dust model
mbb.dat 112 875 DustPedia mbb results by fitting a single
temperature modified black body to the FIR SED
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See also:
J/A+A/609/A37 : 875 nearby galaxies multiwavelength photometry (Clark+, 2018)
J/A+A/620/A112 : Template SED of DustPedia galaxies (Bianchi+, 2018)
J/A+A/622/A132 : Dust emission profiles of DustPedia galaxies (Mosenkov+, 2019)
J/A+A/623/A5 : DustPedia metallicities and HI masses (De Vis+, 2019)
J/A+A/649/A18 : Nearby galaxy perspective on dust evolution (Galliano+, 2021)
J/A+A/699/A346 : Gas and dust in DustPedia galaxies (Salvestrini+, 2025)
Byte-by-byte Description of file: dl14.dat themis.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 23 A23 --- Galaxy Galaxy name (objname)
25- 33 F9.5 deg RAdeg Right Ascension (J2000) (ra2000)
35- 43 F9.5 deg DEdeg Declination ((J2000) de2000)
45- 48 F4.1 --- T Hubble stage (T)
50- 61 F12.9 Mpc Dist Distance (distanceMpc)
63- 70 E8.6 Msun/yr SFR ? Current star-formation rate
(SFRMsolperyr)
72- 79 E8.6 Msun/yr e_SFR ? Uncertainty on star-formation rate
(SFR_err)
81- 89 E9.4 Msun Mstar ? Stellar mass (MstarMsol)
91- 99 E9.4 Msun e_Mstar ? Uncertainty on stellar mass (Mstar_err)
101-109 E9.4 Lsun Lbol ? Bolometric luminosity (LboloLsol)
111-119 E9.4 Lsun e_Lbol ? Uncertainty on bolometric luminosity
(Lbolo_err)
121-129 E9.4 Lsun LoldUnatt ? Unattenuated luminosity of old stars
(Loldunatt_Lsol)
131-139 E9.4 Lsun e_LoldUnatt ? Uncertainty on the unattenuated
luminosity of old stars (Loldunatterr)
141-149 E9.4 Lsun LyoungUnatt ? Unattenuated luminosity of young stars
(Lyoungunatt_Lsol)
151-159 E9.4 Lsun e_LyoungUnatt ? Uncertainty on the unattenuated
luminosity of young stars
(Lyoungunatterr)
161-169 E9.4 Lsun LoldAbs ? Absorbed by dust, luminosity of the old
stars (Loldabs_Lsol)
171-179 E9.4 Lsun LyoungAbs ? Absorbed by dust, luminosity of the
young stars (Lyoungabs_Lsol)
181-185 F5.3 --- AFUV ? FUV attenuation (Afuv)
187-191 F5.3 --- e_AFUV ? Uncertainty on FUV attenuation
(Afuv_err)
193-197 F5.3 --- AV-B90 ? V-B90 colour attenuation (Av_b90)
199-203 F5.3 --- e_AV-B90 ? Uncertainty on V-B90 colour attenuation
(Avb90err)
205-213 E9.4 Msun Mdust ? Dust mass (MdustMsol)
215-223 E9.4 Msun e_Mdust ? Uncertainty on dust mass (Mdust_err)
225-233 E9.4 Lsun Ldust ? Dust luminosity (LdustLsol)
235-243 E9.4 Lsun e_Ldust ? Uncertainty on dust luminosity
(Ldust_err)
245-250 F6.3 --- Umin ? Minimum intensity value of the stellar
radiation field (Umin)
252-257 F6.3 --- e_Umin ? Uncertainty on Umin (Umin_err)
259-264 F6.3 K Tdust ? Dust temperature (TdustK)
266-271 F6.3 K e_Tdust ? Uncertainty on dust temperature
(Tdust_err)
273-277 F5.3 --- qpah ? Mass fractions of aromatic feature
emitting grains (PAH) (qpah)
279-283 F5.3 --- e_qpah ? Uncertainty on mass fractions qpah
(qpah_err)
285-289 F5.3 --- gamma ? Fraction of dust heated in
photo-dissociation regions (PDR) (gamma)
291-295 F5.3 --- e_gamma ? Uncertainty on gamma (gamma_err)
297-302 F6.3 --- redchi2 ? Reduced chi^2 (red_chi2)
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Byte-by-byte Description of file: mbb.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 23 A23 --- Galaxy Galaxy name (objname)
25- 33 F9.5 deg RAdeg Right Ascension (J2000) (ra2000)
35- 43 F9.5 deg DEdeg Declination (J2000) (de2000)
45- 48 F4.1 --- T Hubble stage (T)
50- 61 F12.9 Mpc Dist Distance (distanceMpc)
63- 68 F6.3 K Tdust ? Dust temperature (TdustK)
70- 75 F6.3 K e_Tdust ? Uncertainty on dust temperature (Tdust_err)
77- 85 E9.4 Msun Mdust ? Dust mass (MdustMsol)
87- 95 E9.4 Msun e_Mdust ? Uncertainty on dust mass (Mdust_err)
97-105 E9.4 Lsun Ldust ? Dust luminosity (LdustLsol)
107-112 F6.3 --- redchi2 ? Reduced chi^2 (red_chi2)
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Acknowledgements:
Angelos Nersesian, a.nersesian(at)noa.gr
(End) Patricia Vannier [CDS] 06-Jan-2026