J/A+A/644/A144 Dusty star-forming galaxies physical properties (Donevski+, 2020)
In pursuit of giants.
I. The evolution of the dust-to-stellar mass ratio in distant dusty galaxies.
Donevski D., Lapi A., Malek K., Liu D., Gomez-Guijarro C., Dave R.,
Kraljic K., Pantoni L., Man A., Fujimoto S., Feltre A., Pearson W., Li Q.,
Narayanan, D.
<Astron. Astrophys. 644, A144 (2020)>
=2020A&A...644A.144D 2020A&A...644A.144D (SIMBAD/NED BibCode)
ADC_Keywords: Galaxy catalogs; Photometry, millimetric/submm
Keywords: galaxies: evolution - galaxies: ISM - galaxies: starburst -
galaxies: high-redshift - galaxies: star formation -
submillimeter: galaxies
Abstract:
The dust-to-stellar mass ratio (Mdust/M*) is a crucial yet poorly
constrained quantity to understand the complex physical processes
involved in the production of dust, metals and stars in galaxy
evolution. In this work we explore trends of Mdust/M* with different
physica parameters using observations of 300 massive, dusty
star-forming galaxies detected with ALMA up to z∼5. Additionally, we
interpret our findings with different models of dusty galaxy
formation. We find that Mdust/M* evolves with redshift, stellar
mass, specific star formation rate and integrated dust size,
differently for main sequence and starburst galaxies. In both galaxy
populations Mdust/M* increases until z∼2 followed by a roughly flat
trend towards higher redshifts, suggesting efficient dust growth in
the distant universe. We confirm that the inverse relation between
Mdust/M* and M* holds up to z∼5 and can be interpreted as an
evolutionary transition from early to late starburst phases. We
demonstrate that Mdust/M* in starbursts reflects the increase in
molecular gas fraction with redshift, and attains the highest values
for sources with the most compact dusty star-formation.
The state-of-the-art cosmological simulations that include
self-consistent dust growth, broadly reproduce the evolution of
Mdust/M* in main sequence galaxies, but underestimate it in
starbursts. The latter is found to be linked to lower gas-phase
metallicities and longer dust growth timescales relative to
observations. Phenomenological models based on the
main-sequence/starburst dichotomy and analytical models that include
recipes for rapid metal enrichment are consistent with our
observations. Therefore, our results strongly suggest that high
Mdust/M* is due to rapid dust grain growth in metal enriched
interstellar medium. This work highlights multifold benefits of using
Mdust/M* as a diagnostic tool for: (1) disentangling main sequence
and starburst galaxies up to z∼5; (2) probing the evolutionary phase
of massive objects; and (3) refining the treatment of the dust life
cycle in simulations.
Description:
The catalogue contains main physical properties for 300 distant, dusty
star-forming galaxies detected with ALMA that are analysed in this
work. We make use of panchromatic data coverage of our sources in the
COSMOS field and apply full SED (UV+IR) modelling with the newest
release of code CIGALE. We note that for each parameter CIGALE makes a
probability distribution function (PDF) analysis, and the output value
is the likelihood-weighted mean of the PDF (and consequently, the
associated error is likelihood-weighted standard deviation).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 120 300 List of selected DSFGs and their physical properties
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See also:
J/ApJS/244/40 : A3COSMOS. I. ALMA continuum photometry catalogs (Liu+, 2019)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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3- 18 A16 --- SourceID Source name (as in HELP database,
HELP_JHHMMSS.sss)
22- 28 F7.3 deg RAdeg Right ascension (J2000)
32- 36 F5.3 deg DEdeg Declination (J2000)
40- 44 F5.3 --- z Source observed redshift
48- 53 F6.3 [Msun] logMs Source stellar mass (log scale)
57- 61 F5.3 [Msun] e_logMs Uncertainty on source logMs (log scale)
65- 70 F6.3 [Lsun] logLIR Infrared luminosity integrated over 8-1000um
(log scale)
74- 78 F5.3 [Lsun] e_logLIR Uncertainty on source logLIR (log scale)
82- 86 F5.3 [Msun] logMd Source dust mass (log scale)
90- 94 F5.3 [Msun] e_logMd Uncertainty on source logMd (log scale)
98-102 F5.3 mJy Salma ALMA flux estimation at nu frequency (1)
106-110 F5.3 mJy e_Salma Uncertainty on ALMA flux
114-120 F7.3 GHz nu Observed ALMA frequency
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Note (1): Corresponding to A3COSMOS database (fitted total flux with Gaussian
source models, corrected for flux bias and PBA), Liu et al.,
2019ApJS..244...40L 2019ApJS..244...40L, Cat. J/ApJS/244/40
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Acknowledgements:
Darko Donevski, darko.donevski(at)sissa.it
(End) Patricia Vannier [CDS] 18-Sep-2020