J/A+A/627/A132 GAS II. UV luminosity functions & InfraRed eXcess (Cousin+, 2019)
G.A.S. II:
Dust extinction in galaxies; Luminosity functions and infrared excess.
Cousin M., Buat V., Lagache G., Bethermin M.
<Astron. Astrophys. 627, A132 (2019)>
=2019A&A...627A.132C 2019A&A...627A.132C (SIMBAD/NED BibCode)
ADC_Keywords: Models ; Galaxies ; Infrared ; Ultraviolet ; Interstellar medium
Keywords: galaxies: formation - galaxies: evolution - infrared: galaxies -
ultraviolet: galaxies - dust: galaxies
Abstract:
Dust is a crucial component of the interstellar medium of galaxies.
The presence of dust strongly affects the light produced by stars within
a galaxy. As these photons are our main information vector to explore
the stellar mass assembly and therefore understand a galaxy's
evolution, modeling the luminous properties of galaxies and taking
into account the impact of the dust is a fundamental challenge for
semi-analytical models.
We present the complete prescription of dust attenuation implemented
in the new semi-analytical model (SAM): G.A.S. . This model is based
on a two-phase medium originating from a physically motivated
turbulent model of gas structuring (G.A.S. I paper).
Dust impact is treated by taking into account three dust components:
Polycyclic Aromatic Hydrocarbons, Very Small Grains, and Big Grains.
All three components evolve in both a diffuse and a fragmented/dense
gas phase. Each phase has its own stars, dust content and geometry.
Dust content evolves according to the metallicity of it associated
phase.
The G.A.S. model is used to predict both the UV and the IR luminosity
functions from z=9.0 to z=0.1. Our two-phase ISM prescription catches
very well the evolution of UV and IR luminosity functions. We note a
small overproduction of the IR luminosity at low redshift (z<0.5).
We also focus on the Infrared-Excess (IRX) and explore its dependency
with the stellar mass, UV slope, stellar age, metallicity and slope of
the attenuation curves. Our model predicts large scatters for
relations based on IRX, especially for the IRX- relation. Our analysis
reveals that the slope of the attenuation curve is more driven by
absolute attenuation in the FUV band than by disk inclination.We
confirm that the age of the stellar population and the slope of the
attenuation curve can both shift galaxies below the fiducial
star-birth relation in the IRX- diagram. Main results presented in
this paper (e.g. luminosity functions) and in the two other associated
G.A.S. papers are stored and available in the GALAKSIENN library
through the ZENODO platform.
Description:
In this paper (paper II of the G.A.S. model presentation set), we
present the set of prescriptions implemented in the G.A.S. model to
describe the effects of the dust attenuation onto the stellar light.
Physical prescriptions associated to the gas physics is describe in
Cousin et al. (2019) (paper G.A.S. I).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
fuv_int.dat 173 20 Rest-Frame Galex-FUV luminosity functions predicted
by the G.A.S. model, Intrinsic luminosity functions
fuv_ext.dat 173 20 Rest-Frame Galex-FUV luminosity functions predicted
by the G.A.S. model, Extinguish luminosity functions
totlir.dat 172 18 Total InfraRed luminosity functions predicted by the
G.A.S. model, total IR luminosity functions
birlir.dat 172 18 Total InfraRed luminosity functions predicted by the
G.A.S. model, birth cloud IR luminosity functions
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See also:
J/A+A/627/A131 : GAS I. Stellar mass functions (Cousin+, 2019)
https://zenodo.org/record/1451229#.XIJp24XjIeM : ALL G.A.S. data
Byte-by-byte Description of file (#): fuv_int.dat fuv_ext.dat
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Bytes Format Units Label Explanations
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1- 7 F7.3 mag FUVMAG Absolute FUV magnitude (AB)
11- 19 E9.4 Mpc-3 CD0.30 Comoving density at z=0.30 (in gal/dex/Mpc3 unit)
25- 33 E9.4 Mpc-3 CD0.51 Comoving density at z=0.51 (in gal/dex/Mpc3 unit)
39- 47 E9.4 Mpc-3 CD0.90 Comoving density at z=0.90 (in gal/dex/Mpc3 unit)
53- 61 E9.4 Mpc-3 CD1.16 Comoving density at z=1.16 (in gal/dex/Mpc3 unit)
67- 75 E9.4 Mpc-3 CD2.12 Comoving density at z=2.12 (in gal/dex/Mpc3 unit)
81- 89 E9.4 Mpc-3 CD3.02 Comoving density at z=3.02 (in gal/dex/Mpc3 unit)
95-103 E9.4 Mpc-3 CD3.99 Comoving density at z=3.99 (in gal/dex/Mpc3 unit)
109-117 E9.4 Mpc-3 CD4.98 Comoving density at z=4.98 (in gal/dex/Mpc3 unit)
123-131 E9.4 Mpc-3 CD6.12 Comoving density at z=6.12 (in gal/dex/Mpc3 unit)
137-145 E9.4 Mpc-3 CD6.95 Comoving density at z=6.95 (in gal/dex/Mpc3 unit)
151-159 E9.4 Mpc-3 CD8.21 Comoving density at z=8.21 (in gal/dex/Mpc3 unit)
165-173 E9.4 Mpc-3 CD8.91 Comoving density at z=8.91 (in gal/dex/Mpc3 unit)
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Byte-by-byte Description of file (#): totlir.dat birlir.dat
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Bytes Format Units Label Explanations
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1- 6 F6.3 [Lsun] logLIR Infrared luminosity
10- 18 E9.4 Mpc-3 CD0.10 Comoving density at z=0.10 (in gal/dex/Mpc3 unit)
24- 32 E9.4 Mpc-3 CD0.41 Comoving density at z=0.41 (in gal/dex/Mpc3 unit)
38- 46 E9.4 Mpc-3 CD0.59 Comoving density at z=0.59 (in gal/dex/Mpc3 unit)
52- 60 E9.4 Mpc-3 CD0.90 Comoving density at z=0.90 (in gal/dex/Mpc3 unit)
66- 74 E9.4 Mpc-3 CD1.21 Comoving density at z=2.12 (in gal/dex/Mpc3 unit)
80- 88 E9.4 Mpc-3 CD1.53 Comoving density at z=1.53 (in gal/dex/Mpc3 unit)
94-102 E9.4 Mpc-3 CD2.07 Comoving density at z=2.07 (in gal/dex/Mpc3 unit)
108-116 E9.4 Mpc-3 CD2.84 Comoving density at z=2.84 (in gal/dex/Mpc3 unit)
122-130 E9.4 Mpc-3 CD3.69 Comoving density at z=3.69 (in gal/dex/Mpc3 unit)
136-144 E9.4 Mpc-3 CD4.75 Comoving density at z=4.75 (in gal/dex/Mpc3 unit)
150-158 E9.4 Mpc-3 CD6.12 Comoving density at z=6.12 (in gal/dex/Mpc3 unit)
164-172 E9.4 Mpc-3 CD6.95 Comoving density at z=6.95 (in gal/dex/Mpc3 unit)
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History:
Copied at https://zenodo.org/
References:
Cousin et al., Paper I 2019A&A...627A.131C 2019A&A...627A.131C
(End) Patricia Vannier [CDS] 06-Mar-2019