Dust contribution to the panchromatic galaxy emission

Abstract

We have developed a pipeline called \mentari to generate the far-ultraviolet to far-infrared spectral energy distribution (SED) of galaxies from the \dustysage semi-analytic galaxy formation model (SAM). \dustysage incorporates dust-related processes directly on top of the basic ingredients of galaxy formation like gas infall, cooling, star formation, feedback, and mergers. We derive a physically motivated attenuation model from the computed dust properties in \dustysage, so each galaxy has a self-consistent set of attenuation parameters based on the complicated dust physics that occurred across the galaxy's assembly history. Then, we explore several dust emission templates to produce infrared spectra. Our results show that a physically-motivated attenuation model is better for obtaining a consistent multi-wavelength description of galaxy formation and evolution, compared to using a constant attenuation. We compare our predictions with a compilation of observations and find that the fiducial model is in reasonable agreement with: (i) the observed $z=0$ luminosity functions from the far-ultraviolet to far-infrared simultaneously, and hence (ii) the local cosmic SED in the same range, (iii) the rest-frame K-band luminosity function across $0<z<3$, and (iv) the rest-frame far-ultraviolet luminosity function across $0<z<1$. Our model underproduces the far-ultraviolet emission at $z=2$ and $z=3$, which can be improved by altering the AGN feedback and dust processes in \dustysage. However, this combination thus worses the agreement at $z=0$, which suggests that more detailed treatment of such processes is required.

20 pages, 14 figures, accepted for publication in MNRAS

References in corpus (18)

• The NumPy array: a structure for efficient numerical computation
• The EAGLE project: Simulating the evolution and assembly of galaxies and their environments
• Infrared Emission from Interstellar Dust. IV. The Silicate-Graphite-PAH Model in the Post-Spitzer Era
• A simple model to interpret the ultraviolet, optical and infrared emission from galaxies
• An ALMA survey of Sub-millimeter Galaxies in the Extended Chandra Deep Field South: Physical properties derived from ultraviolet-to-radio modelling
• Submillimetre galaxies in a hierarchical universe: number counts, redshift distribution, and implications for the IMF
• The Constant Average Relationship between Dust-obscured Star Formation and Stellar Mass from $z=0$ to $z=2.5$
• Destruction of Interstellar Dust in Evolving Supernova Remnant Shock Waves
• How to distinguish starbursts and quiescently star-forming galaxies: The `bimodal' submillimetre galaxy population as a case study
• Dust origin in late-type dwarf galaxies: ISM growth vs. type II supernovae
• On the importance of using appropriate spectral models to derive physical properties of galaxies at 0.7<z<2.8
• AGN-driven outflows and the AGN feedback efficiency in young radio galaxies
• The origin of dust in galaxies across cosmic time
• The Herschel-ATLAS: Evolution of the 250um luminosity function out to z=0.5
• Deep Extragalactic VIsible Legacy Survey (DEVILS): Identification of AGN through SED Fitting and the Evolution of the Bolometric AGN Luminosity Function
• Galaxy And Mass Assembly: the evolution of the cosmic spectral energy distribution from z = 1 to z = 0
• The cosmic spectral energy distribution in the EAGLE simulation
• Exploring the relation between dust mass and galaxy properties using Dusty SAGE

Cited by in corpus (1)

• Measurement of the evolving galaxy luminosity and mass function using clustering-based redshift inference