SKIRT 9: Redesigning an advanced dust radiative transfer code to allow kinematics, line transfer and polarization by aligned dust grains

Camps, Peter; Baes, M.

doi:10.1016/j.ascom.2020.100381

Cited by 120 publications

(85 citation statements)

References 86 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…S (Jonsson 2006), R -3 (Dullemond et al 2012), (Camps & Baes 2015), P (Narayanan et al 2021), etc) available, most relying on sophisticated Monte-Carlo methods. For this study we use the publicly available code , version 9 (Camps & Baes 2020).…”

Section: Spectral Energy Distribution Modellingmentioning

confidence: 99%

First Light And Reionisation Epoch Simulations (FLARES) II: The Photometric Properties of High-Redshift Galaxies

Vijayan

Lovell

Wilkins

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present the photometric properties of galaxies in the First Light and Reionisation Epoch Simulations (Flares). The simulations trace the evolution of galaxies in a range of overdensities through the Epoch of Reionistion (EoR). With a novel weighting scheme we combine these overdensities, extending significantly the dynamic range of observed composite distribution functions compared to periodic simulation boxes. Flares predicts a significantly larger number of intrinsically bright galaxies, which can be explained through a simple model linking dust-attenuation to the metal content of the interstellar medium, using a line-of-sight (LOS) extinction model. With this model we present the photometric properties of the Flares galaxies for z ∈ [5, 10]. We show that the ultraviolet (UV) luminosity function (LF) matches the observations at all redshifts. The function is fit by Schechter and double power-law forms, with the latter being favoured at these redshifts by the Flares composite UV LF. We also present predictions for the UV continuum slope as well as the attenuation in the UV. The impact of environment on the UV LF is also explored, with the brightest galaxies forming in the densest environments. We then present the line luminosity and equivalent widths of some prominent nebular emission lines arising from the galaxies, finding rough agreement with available observations. We also look at the relative contribution of obscured and unobscured star formation, finding comparable contributions at these redshifts.

show abstract

Section: Spectral Energy Distribution Modellingmentioning

confidence: 99%

First Light And Reionisation Epoch Simulations (FLARES) II: The Photometric Properties of High-Redshift Galaxies

Vijayan

Lovell

Wilkins

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…First, we build a galaxy model that sets the distribution of stars and dust (dust-stars geometry). Secondly, we perform radiative transfer calculations using SKIRT9 1 (Camps & Baes 2020) and extract the attenuation curve by comparing the intrinsic stellar SED and the emergent galaxy SED. We further output the IRX-β relations.…”

Section: E T H O D Smentioning

confidence: 99%

Geometry effects on dust attenuation curves with different grain sources at high redshift

Lin

Hirashita

Camps

et al. 2021

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Dust has been detected in high-redshift (z > 5) galaxies but its origin is still being debated. Dust production in high-redshift galaxies could be dominated by stellar production or by accretion (dust growth) in the interstellar medium. Previous studies have shown that these two dust sources predict different grain-size distributions, which lead to significantly different extinction curves. In this paper, by performing radiative transfer calculations, we investigate how the difference in the extinction curves affects the dust attenuation properties of galaxies. To examine the major effects of the dust–stars distribution geometry, we adopt two representative cases in spherical symmetry: the well-mixed geometry (stars and dust are homogeneously mixed) and the two-layer geometry (young stars are more concentrated in the centre). In both cases, we confirm that the attenuation curve can be drastically steepened by scattering and by different optical depths between young and old stellar populations, and can be flattened by the existence of unobscured stellar populations. We can reproduce similar attenuation curves even with very different extinction curves. Thus, we conclude that it is difficult to distinguish dust sources only with attenuation curves. However, if we include information on dust emission and plot the relation between infrared excess (IRX) and the ultraviolet spectral slope (β), then different dust sources predict different positions in the IRX–β diagram. A larger β is preferred under a similar IRX if dust growth is the dominant dust source.

show abstract

“…in skirt yet; however, the framework to implement them is now ready (Camps & Baes 2020). Finally, the model falls short fitting the peak of the dust emission in the FIR (the difference in PACS 70 and 160 µm is 0.18 dex and 0.2 dex, respectively), while the luminosities of the longest FIR wavelengths (≥250 µm) are in excellent agreement, with residuals below 0.1 dex.…”

Section: Sed Fitting With Skirtmentioning

confidence: 97%

High-resolution, 3D radiative transfer modelling

Nersesian

Viaene

Baes

et al. 2020

A&A

View full text Add to dashboard Cite

Context. Investigating the dust heating mechanisms in galaxies provides a deeper understanding of how the internal energy balance drives their evolution. Over the last decade radiative transfer simulations based on the Monte Carlo method have emphasised the role of the various stellar populations heating the diffuse dust. Beyond the expected heating through ongoing star formation, older stellar populations (≥8 Gyr) and even active galactic nuclei can both contribute energy to the infrared emission of diffuse dust. Aims. In this particular study we examine how the radiation of an external heating source, such as the less massive galaxy NGC 5195 in the M 51 interacting system, could affect the heating of the diffuse dust of its parent galaxy NGC 5194, and vice versa. Our goal is to quantify the exchange of energy between the two galaxies by mapping the 3D distribution of their radiation field. Methods. We used SKIRT, a state-of-the-art 3D Monte Carlo radiative transfer code, to construct the 3D model of the radiation field of M 51, following the methodology defined in the DustPedia framework. In the interest of modelling, the assumed centre-to-centre distance separation between the two galaxies is ∼10 kpc. Results. Our model is able to reproduce the global spectral energy distribution of the system, and it matches the resolved optical and infrared images fairly well. In total, 40.7% of the intrinsic stellar radiation of the combined system is absorbed by dust. Furthermore, we quantify the contribution of the various dust heating sources in the system, and find that the young stellar population of NGC 5194 is the predominant dust-heating agent, with a global heating fraction of 71.2%. Another 23% is provided by the older stellar population of the same galaxy, while the remaining 5.8% has its origin in NGC 5195. Locally, we find that the regions of NGC 5194 closer to NGC 5195 are significantly affected by the radiation field of the latter, with the absorbed energy fraction rising up to 38%. The contribution of NGC 5195 remains under the percentage level in the outskirts of the disc of NGC 5194. This is the first time that the heating of the diffuse dust by a companion galaxy is quantified in a nearby interacting system.

show abstract

SKIRT 9: Redesigning an advanced dust radiative transfer code to allow kinematics, line transfer and polarization by aligned dust grains

Cited by 120 publications

References 86 publications

First Light And Reionisation Epoch Simulations (FLARES) II: The Photometric Properties of High-Redshift Galaxies

First Light And Reionisation Epoch Simulations (FLARES) II: The Photometric Properties of High-Redshift Galaxies

Geometry effects on dust attenuation curves with different grain sources at high redshift

High-resolution, 3D radiative transfer modelling

Contact Info

Product

Resources

About