J/A+A/649/A18 Nearby galaxy perspective on dust evolution (Galliano+, 2021)
A nearby galaxy perspective on dust evolution.
Scaling relations and constraints on the dust build-up in galaxies with the
DustPedia and DGS samples.
Galliano F., Nersesian A., Bianchi S., De Looze I., Roychowdhury S.,
Baes M., Casasola V., Cassara L.P., Dobbels W., Fritz J., Galametz M.,
Jones A.P., Madden S.C., Mosenkov A., Xilouris E.M., Ysard N.
<Astron. Astrophys. 649, A18 (2021)>
=2021A&A...649A..18G 2021A&A...649A..18G (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Abundances
Keywords: ISM: abundances, dust, evolution - galaxies: evolution -
methods: statistical
Abstract:
The efficiency of the different processes responsible for the
evolution of interstellar dust on the scale of a galaxy are, to date,
very uncertain, spanning several orders of magnitude in the
literature. Yet, precise knowledge of the grain properties is key to
addressing numerous open questions about the physics of the
interstellar medium and galaxy evolution.
This article presents an empirical statistical study, aimed at
quantifying the timescales of the main cosmic dust evolution processes
as a function of the global properties of a galaxy.
We have modelled a sample of ∼800 nearby galaxies, spanning a wide
range of metallicity, gas fraction, specific star formation rate and
Hubble stage. We have derived the dust properties of each object from
its spectral energy distribution. Throughout this paper, we have
adopted a hierarchical Bayesian approach, resulting in a single large
probability distribution of all the parameters of all the galaxies, to
ensure the most rigorous interpretation of our data.
We confirm the drastic evolution with metallicity of the dust-to-metal
mass ratio (by two orders of magnitude), found by previous studies. We
confirm the well-known evolution of the aromatic-feature-emitting
grain mass fraction as a function of metallicity and interstellar
radiation field intensity. Our data indicate the relation with
metallicity is significantly stronger.
Our results provide valuable constraints for simulations of galaxies.
They imply that grain growth is the likely dust production mechanism
in dusty high-redshift objects. We also emphasize the determinant role
of local, low metallicity systems in order to address these questions.
Description:
This table gives the hierarchical Bayesian SED fitting results for 798
galaxies. We quote the dust mass, mean starlight intensity, fraction
of small amorphous carbon grains, gas mass, fraction of molecular gas,
stellar mass, specific star formation rate, and metallicity. The
rigorous uncertainty of each of these parameters is also provided.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableh1.dat 255 798 SED fitting results
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See also:
http://dustpedia.astro.noa.gr : DustPedia catalog Home Page
Byte-by-byte Description of file: tableh1.dat
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Bytes Format Units Label Explanations
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1- 15 A15 --- Galaxy Galaxy name according to the DustPedia
catalog (1)
16- 30 E15.5 [Msun] logMdust Decimal logarithm of the dust mass
31- 45 E15.5 [Msun] e_logMdust Uncertainty on logMdust
46- 60 E15.5 [2.2E-5W/m2] logUav Decimal logarithm of the average
starlight intensity, U, in 2.2E-5W/m2
61- 75 E15.5 [2.2E-5W/m2] e_logUav Uncertainty on logUav
76- 90 E15.5 [-] logqAF Decimal logarithm of the mass fraction
of small a-C(:H) grains
91-105 E15.5 [-] e_logqAF Uncertainty on logqAF
106-120 E15.5 [Msun] logMgas ?=- Decimal logarithm of the gas mass
121-135 E15.5 [Msun] e_logMgas ?=- Uncertainty on logMgas
136-150 E15.5 [-] logfmol ?=- Decimal logarithm of the mass
fraction of molecular gas
151-165 E15.5 [-] e_logfmol ?=- Uncertainty on logfmol
166-180 E15.5 [Msun] logMstar ?=- Decimal logarithm of the stellar
mass
181-195 E15.5 [Msun] e_logMstar ?=- Uncertainty on logMstar
196-210 E15.5 [yr-1] logsSFR ?=- Decimal logarithm of the specific
star formation rate
211-225 E15.5 [yr-1] e_logsSFR ?=- Uncertainty on logsSFR
226-240 E15.5 [-] logOovHp12 ?=- Metallicity expressed as
12+log(O/H)
241-255 E15.5 [-] e_logOovHp12 ?=- Uncertainty on 12+log(O/H)
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Note (1): DustPedia catalog at http://dustpedia.astro.noa.gr/
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Acknowledgements:
Frederic Galliano, frederic.galliano(at)cea.fr
(End) Frederic Galliano [AIM, France], Patricia Vannier [CDS] 07-Jan-2021