High-resolution panchromatic spectral models of galaxies including photoionization and dust

By P. Jonsson, B. Groves, Thomas J. Cox. 2009

185 citations recorded by the source corpus.

An updated version of the dust radiation-transfer code SUNRISE, including models for star-forming regions and a self-consistent calculation of the spatially dependent dust and PAH emission, is presented. Given a hydrodynamic simulation of a galaxy, this model can calculate a realistic 2D ultraviolet-submillimetre spectral energy distribution of the galaxy, including emission lines from H II regions, from any viewpoint. To model the emission from star-forming regions, the MAPPINGSIII photoionization code is used. The high wavelength resolution (∼1000 wavelengths) is made possible by the polychromatic Monte Carlo algorithm employed by SUNRISE. From the 2D spectral energy distributions (SEDs), images in any filter bands or integrated galaxy SEDs can be created. Using a suite of hydrodynamic simulations of disc galaxies, the output broad-band images and SEDs are compared with observed galaxies from the multiwavelength SINGS and SLUGS galaxy surveys. Overall, the output SEDs show a good match with observed galaxies in colours ranging from far-UV to submillimetre wavelengths. The only possible exception is the 160/850 μm colour, which the simulations underestimate by a factor of ∼5 compared to the SINGS sample. However, the simulations here agree with the SLUGS galaxies, which consistently have significantly larger amounts of cold dust than the SINGS galaxies. The SUNRISE model can be used to generate simulated observations of arbitrary hydrodynamic galaxy simulations. In this way, predictions of galaxy formation theories can be directly tested against observations of galaxies.

Subfields: Astronomy and Astrophysics, Global and Planetary Change

View Paper: https://www.semanticscholar.org/paper/09970c555fbcff0075bf531a27af4147e9a3c730

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Citations in the corpus

THE CENTRAL SLOPE OF DARK MATTER CORES IN DWARF GALAXIES: SIMULATIONS VERSUS THINGS (2010, methodology): “To properly compare the outputs from the simulation to real galaxies and make accurate estimates of the observable properties of galaxies (e.g., Sánchez-Janssen et al. 2010), we used the Monte Carlo radiation transfer code SUNRISE (Jonsson et al. 2010) to generate artificial optical images and spec”
The optical morphologies of galaxies in the IllustrisTNG simulation: a comparison to Pan-STARRS observations (2018, methodology): “…and subsequent analysis of synthetic images from hydrodynamic simulations is quickly becoming a powerful tool to connect galaxy formation theory with observations (e.g. Lotz et al. 2008a; Jonsson et al. 2010; Snyder et al. 2015a,b; Bignone et al. 2017; Bottrell et al. 2017a; Trayford et al. 2017).”
A general model for the CO–H2 conversion factor in galaxies with applications to the star formation law (2011, methodology): “We utilize the publicly available SUNRISE dust radiative transfer simulation package (Jonsson 2006; Jonsson et al. 2006, 2010; Jonsson & Primack 2010) for two purposes: to generate the adaptive mesh from the GADGET-3 simulations on which we run the radiative transfer, and to calculate dust…”
AN ALMA SURVEY OF SUB-MILLIMETER GALAXIES IN THE EXTENDED CHANDRA DEEP FIELD SOUTH: PHYSICAL PROPERTIES DERIVED FROM ULTRAVIOLET-TO-RADIO MODELING (2015, methodology): “…with higher AV being observed more edge-on), since viewing angle does not affect the shape and normalization of the dust emission because it is isotropic (for an illustration of the effect of viewing angle on SEDs computed using a radiative transfer code, see Figure 8 of Jonsson et al. 2010).”
CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY (2011, unknown): “…of hydrodynamic simulations with the SUNRISE radiative transfer code to produce realis- 49 See, for example, Darren Croton’s website at http://web.me.com/darrencroton/Homepage/Downloads.html. tic images and spectra, including the effects of absorption and scattering by dust (Jonsson et al. 2010).”
Physical Models of Galaxy Formation in a Cosmological Framework (2014, background): “However, with sufficiently high resolution, radiative transfer through a dusty ISM can be computed in post-processing to estimate the observed pan-chromatic properties of galaxies (e.g. Jonsson et al. 2010) and their line emission (e.g. Narayanan et al. 2008).”
The Horizon-AGN simulation: evolution of galaxy properties over cosmic time (2016, methodology): “We perform this check by using SUNRISE (Jonsson 2006; Jonsson et al. 2010), a Monte-Carlo radiative transfer code applicable to arbitrary dust geometries, on a small random sample of galaxies.”
Submillimetre galaxies in a hierarchical universe: number counts, redshift distribution, and implications for the IMF (2012, unknown): “We briefly review the details of SUNRISE here, but we refer the reader to Jonsson et al. (2006, 2010) and Jonsson & Primack (2010) for full details of the SUNRISE code.”
Dusty Star Forming Galaxies at High Redshift (2014, unknown): “These authors coupled these simulationswith sunrise, a 3DMonte Carlo dust radiative transfer code in order to produce the simulated SED and nebular line properties of their simulated galaxies (Jonsson, 2006; Jonsson et al., 2010; Jonsson and Primack, 2010).”
THE EMISSION BY DUST AND STARS OF NEARBY GALAXIES IN THE HERSCHEL KINGFISH SURVEY (2011, background): “Lastly, note that galaxy geometry (i.e., inclination) and differential extinction will affect these ratios within galaxies to some degree (e.g., Jonsson et al. 2010).”
A physical model for z∼ 2 dust-obscured galaxies (2009, methodology): “Effectively, what this means is that the radiative transfer models here do not account for absorption by GMCs outside of a given stellar cluster’s birthcloud (Jonsson et al. 2010).”
Fitting the integrated spectral energy distributions of galaxies (2010, methodology): “The new radiation field is converted to IR emission using models such as Dale and Helou (2002) or Draine and Li (2007) (see e.g. Juvela 2005; Jonsson et al. 2010).”
Galaxy morphology and star formation in the Illustris Simulation at z = 0 (2015, methodology): “We generate noiseless high-resolution images with an approach described by Torrey et al. (2015, hereafter T15) built around the Sunrise3 code (Jonsson 2006; Jonsson et al. 2010; Jonsson & Primack 2010).”
DUST-CORRECTED STAR FORMATION RATES OF GALAXIES. I. COMBINATIONS OF Hα AND INFRARED TRACERS (2009, background): “The predictions for more typical disk galaxies are inconclusive, with some studies suggesting a mild bias in attenuations estimated from the foreground dust screen approximation (e.g., Charlot & Fall 2000), but with other studies showing little or no bias (e.g., Jonsson et al. 2009).”