TY - JOUR
T1 - From the far-ultraviolet to the far-infrared - galaxy emission at 0 ≤ z ≤ 10 in the SHARK semi-analytic model
AU - Lagos, Claudia Del P.
AU - Robotham, Aaron S. G.
AU - Trayford, James W.
AU - Tobar, Rodrigo
AU - Bravo, Matías
AU - Bellstedt, Sabine
AU - Davies, Luke J. M.
AU - Driver, Simon P.
AU - Elahi, Pascal J.
AU - Obreschkow, Danail
AU - Power, Chris
N1 - Funding Information:
We thank Cedric Lacey, Carlton Baugh, and Desika Narayanan for useful discussions about the results in this paper, and the anonymous referee for their constructive report. CL has received funding from the ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. CL also thanks the MERAC Foundation for a Postdoctoral Research Award. JT and CL also thank the University of Western Australia for a Research Collaboration Award, which facilitated the face-to-face interaction that led to this work. This work was supported by resources provided by The Pawsey Supercomputing Centre with funding from the Australian Government and the Government of Western Australia. Cosmic Dawn Centre is funded by the Danish National Research Foundation.
Publisher Copyright:
© 2019 The Author(s).
PY - 2019/11/1
Y1 - 2019/11/1
N2 - We combine the SHARK semi-analytic model of galaxy formation with the PROSPECT software tool for spectral energy distribution (SED) generation to study the multiwavelength emission of galaxies from the far-ultraviolet (FUV) to the far-infrared (FIR) at 0 ≤ z ≤ 10. We produce a physical model for the attenuation of galaxies across cosmic time by combining a local Universe empirical relation to compute the dust mass of galaxies from their gas metallicity and mass, attenuation curves derived from radiative transfer calculations of galaxies in the EAGLE hydrodynamic simulation suite, and the properties of SHARK galaxies. We are able to produce a wide range of galaxies, from the z = 8 star-forming galaxies with almost no extinction, z = 2 submillimetre galaxies, down to the normal star-forming and red-sequence galaxies at z = 0. Quantitatively, we find that SHARK reproduces the observed (i) z = 0 FUV-to-FIR, (ii) 0 ≤ z ≤ 3 rest-frame K-band, and (iii) 0 ≤ z ≤ 10 rest-frame FUV luminosity functions, (iv) z ≤ 8 UV slopes, (v) the FUV-to-FIR number counts (including the widely disputed 850 μm), (vi) redshift distribution of bright 850 μm galaxies, and (vii) the integrated cosmic SED from z = 0 to 1 to an unprecedented level. This is achieved without the need to invoke changes in the stellar initial mass function, dust-to-metal mass ratio, or metal enrichment time-scales. Our model predicts star formation in galaxy discs to dominate in the FUV-to-optical, while bulges dominate at the NIR at all redshifts. The FIR sees a strong evolution in which discs dominate at z ≤ 1 and starbursts (triggered by both galaxy mergers and disc instabilities, in an even mix) dominate at higher redshifts, even out to z = 10.
AB - We combine the SHARK semi-analytic model of galaxy formation with the PROSPECT software tool for spectral energy distribution (SED) generation to study the multiwavelength emission of galaxies from the far-ultraviolet (FUV) to the far-infrared (FIR) at 0 ≤ z ≤ 10. We produce a physical model for the attenuation of galaxies across cosmic time by combining a local Universe empirical relation to compute the dust mass of galaxies from their gas metallicity and mass, attenuation curves derived from radiative transfer calculations of galaxies in the EAGLE hydrodynamic simulation suite, and the properties of SHARK galaxies. We are able to produce a wide range of galaxies, from the z = 8 star-forming galaxies with almost no extinction, z = 2 submillimetre galaxies, down to the normal star-forming and red-sequence galaxies at z = 0. Quantitatively, we find that SHARK reproduces the observed (i) z = 0 FUV-to-FIR, (ii) 0 ≤ z ≤ 3 rest-frame K-band, and (iii) 0 ≤ z ≤ 10 rest-frame FUV luminosity functions, (iv) z ≤ 8 UV slopes, (v) the FUV-to-FIR number counts (including the widely disputed 850 μm), (vi) redshift distribution of bright 850 μm galaxies, and (vii) the integrated cosmic SED from z = 0 to 1 to an unprecedented level. This is achieved without the need to invoke changes in the stellar initial mass function, dust-to-metal mass ratio, or metal enrichment time-scales. Our model predicts star formation in galaxy discs to dominate in the FUV-to-optical, while bulges dominate at the NIR at all redshifts. The FIR sees a strong evolution in which discs dominate at z ≤ 1 and starbursts (triggered by both galaxy mergers and disc instabilities, in an even mix) dominate at higher redshifts, even out to z = 10.
KW - Galaxies: Evolution
KW - Galaxies: Formation
KW - Galaxies: Luminosity function
KW - ISM: Dust, extinction
UR - http://www.scopus.com/inward/record.url?scp=85075162450&partnerID=8YFLogxK
U2 - 10.1093/mnras/stz2427
DO - 10.1093/mnras/stz2427
M3 - Article
AN - SCOPUS:85075162450
SN - 0035-8711
VL - 489
SP - 4196
EP - 4216
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 3
ER -