J/A+A/699/A346 Gas and dust in DustPedia galaxies (Salvestrini+, 2025)
Exploring the interplay of dust and gas phases in DustPedia star-forming
galaxies.
Salvestrini F., Bianchi S., Corbelli E.
<Astron. Astrophys. 699, A346 (2025)>
=2025A&A...699A.346S 2025A&A...699A.346S (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Interstellar medium
Keywords: galaxiesL ISM - galaxies: star formation
Abstract:
Molecular gas is the key ingredient of the star formation cycle, and
tracing its dependencies on other galaxy properties is essential for
understanding galaxy evolution. In this work, we explore the relation
between the different phases of the interstellar medium (ISM), namely
molecular gas, atomic gas, and dust, and galaxy properties using a
sample of nearby late-type galaxies. To this goal, we collect CO maps
for 121 galaxies from the DustPedia project, ensuring an accurate
determination of MH2, the global molecular gas mass. We investigate
which scaling relations provide the best description of MH2, based on
the strength of the correlation and its intrinsic dispersion. Commonly
used correlations between MH2 and star formation rate (SFR) and
stellar mass (M*) are affected by large scatter, which accounts for
galaxies that are experiencing quenching of their star formation
activity. This issue can be partially mitigated by considering a
"fundamental plane" of star formation, fitting together MH2, Mstar,
and SFR. We confirm previous results from the DustPedia collaboration
that the total gas mass has the tightest connection with the dust mass
and that the molecular component also establishes a good correlation
with dust. Although dust grains are necessary for the formation of
hydrogen molecules, the strength of gravitational potential driven by
the stellar component plays a key role in driving density enhancements
and the atomic-to-molecular phase transition. Eventually, we
investigated the correlations between ISM components and monochromatic
luminosities at different wavelengths: we proposed mid and far-IR
luminosities as reliable proxies of L'CO for sources lacking dedicated
millimeter observations. Luminosities in mid-IR photometric bands
collecting PAH emission can be used to trace molecular gas and dust
masses.
Description:
The tables includes the main properties of the 121 galaxies from the
DustPedia sample analyzed in this work. The quantities are drwan from
the DustPedia archive, that is available online at
https://dustpedia.astro.noa.gr/.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 92 121 Properties of the 121 galaxies analyzed in
this work
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See also:
J/ApJS/257/21 : VERTICO: the Virgo EnviRonment Traced In CO survey
(Brown+, 2021)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Name Source name
12- 20 A9 --- Sample Survey that presented H2 data as in
Table 1 (1)
22- 24 F3.1 --- HT Hubble Type
26- 30 F5.2 [Msun] logMstar log of stellar mass
32- 35 F4.2 [Msun] e_logMstar Error on log of stellar mass
37- 41 F5.2 [Msun/yr] logSFR log of star formation rate
43- 46 F4.2 [Msun/yr] e_logSFR Error on log of SFR
48- 51 F4.2 [Msun] logMdust log of dust mass
53- 56 F4.2 [Msun] e_logMdust Error on log of dust mass
58 A1 --- l_logMH2 Limit flag on logMH2
59- 63 F5.2 [Msun] logMH2 log of H2 gas mass (2)
65- 68 F4.2 [Msun] e_logMH2 ? Error on log of H2 gas mass
70 A1 --- l_logMHIR25 Limit flag on logMHIR25
71- 75 F5.2 [Msun] logMHIR25 ? log of HI gas mass within R25
77- 80 F4.2 [Msun] e_logMHIR25 ? Error on log of HI gas mass within R25
82 A1 --- l_logMHItot Limit flag on logMHItot
83- 87 F5.2 [Msun] logMHItot ? log of total HI gas mass
89- 92 F4.2 [Msun] e_logMHItot ? Error on log of total HI gas mass
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Note (1): Sampla as follows:
COMING = Sorai et al. (2019PASJ...71S..14S 2019PASJ...71S..14S)
Chung+17 = Chung et al. (2017ApJ...843...50C 2017ApJ...843...50C)
Curran+01 = Curran et al. (2001A&A...368..824C 2001A&A...368..824C)
HERACLES = Groves et al. (2015ApJ...799...96G 2015ApJ...799...96G)
HeViCS = Corbelli et al. (2012A&A...542A..32C 2012A&A...542A..32C)
MM+22 = Morokuma-Matsui et al. (2022ApJS..263...40M 2022ApJS..263...40M)
VertiCO = Brown et al. (2021ApJS..257...21B 2021ApJS..257...21B, Cat. J/ApJS/257/21)
Note (2): The uncertainty on MH2 does not include the systematic uncertainty
of ∼30% due to the adoption of a CO-to-H2 convection factor as in
Bolatto et al., 2013ARA&A..51..207B 2013ARA&A..51..207B.
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Acknowledgements:
Francesco Salvestrini, francesco.salvestrini(at)inaf.it
(End) Patricia Vannier [CDS] 08-Jun-2025