Predicting the stellar and non-equilibrium dust emission spectra of high-resolution simulated galaxies with dart-ray

Natale, Giovanni; Popescu, Cristina; Tuffs, R.; Debattista, Victor P.; Fischera, Joerg; Grootes, Meiert W.

doi:10.1093/mnras/stv286

Cited by 40 publications

(48 citation statements)

References 115 publications

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“…The results here are broadly consistent with the characterisation of the dust emission by these models. However, we observe the transition between SFR dust and ISRF dust at 70-100 µm, whereas in the model fits shown by Draine et al (2007), the transition generally takes place at shorter wavelengths (below 70 µm), while De Looze et al (2014) finds the transition to be around 60 µm, and the model of Natale et al (2015) has the transition at around 30 µm. These results are, of course, dependent on the implementation details of the modelling of the two components.…”

Section: Determination Of Dust Heating Mechanismcontrasting

confidence: 57%

Planckintermediate results

Ade

Aghanim

Arnaud

et al. 2015

A&A

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The Andromeda galaxy (M 31) is one of a few galaxies that has sufficient angular size on the sky to be resolved by the Planck satellite. Planck has detected M 31 in all of its frequency bands, and has mapped out the dust emission with the High Frequency Instrument, clearly resolving multiple spiral arms and sub-features. We examine the morphology of this long-wavelength dust emission as seen by Planck, including a study of its outermost spiral arms, and investigate the dust heating mechanism across M 31. We find that dust dominating the longer wavelength emission ( > ∼ 0.3 mm) is heated by the diffuse stellar population (as traced by 3.6 µm emission), with the dust dominating the shorter wavelength emission heated by a mix of the old stellar population and star-forming regions (as traced by 24 µm emission). We also fit spectral energy distributions for individual 5 pixels and quantify the dust properties across the galaxy, taking into account these different heating mechanisms, finding that there is a linear decrease in temperature with galactocentric distance for dust heated by the old stellar population, as would be expected, with temperatures ranging from around 22 K in the nucleus to 14 K outside of the 10 kpc ring. Finally, we measure the integrated spectrum of the whole galaxy, which we find to be well-fitted with a global dust temperature of (18.2 ± 1.0) K with a spectral index of 1.62 ± 0.11 (assuming a single modified blackbody), and a significant amount of free-free emission at intermediate frequencies of 20-60 GHz, which corresponds to a star formation rate of around 0.12 M yr −1 . We find a 2.3σ detection of the presence of spinning dust emission, with a 30 GHz amplitude of 0.7 ± 0.3 Jy, which is in line with expectations from our Galaxy.

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Section: Determination Of Dust Heating Mechanismcontrasting

confidence: 57%

Planckintermediate results

Ade

Aghanim

Arnaud

et al. 2015

A&A

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“…The galaxy inclination has also been observed to influence the attenuation of galaxies (e.g., Wild et al 2011) and is expected from theory (e.g., Pierini et al 2004;Tuffs et al 2004;Chevallard et al 2013;Natale et al 2015), but we defer exploring this parameter for our sample to a subsequent paper in order to perform a more in-depth analysis. We follow the same procedure outlined in Section 4.1 and divide each sample into six bins of t B l and construct average flux templates.…”

Section: The Variation Of the Attenuation Curvementioning

confidence: 95%

Characterizing Dust Attenuation in Local Star-forming Galaxies: Near-infrared Reddening and Normalization

Battisti

Calzetti

Chary

2017

ApJ

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We characterize the near-infrared dust attenuation for a sample of ∼5500 local (  z 0.1) star-forming galaxies and obtain an estimate of their average total-to-selective attenuation l ( ) k . We utilize data from the United Kingdom Infrared Telescope and the Two-Micron All Sky Survey, which is combined with previously measured UV-optical data for these galaxies. The average attenuation curve is slightly lower in the far-ultraviolet than in local starburst galaxies by roughly 15% but appears similar at longer wavelengths with a total-to-selective normalization of = -+ R 3.670.44 . Under the assumption of energy balance, the total attenuated energy inferred from this curve is found to be broadly consistent with the observed infrared dust emission (L TIR ) in a small sample of local galaxies for which far-infrared measurements are available. However, the significant scatter in this quantity among the sample may reflect large variations in the attenuation properties of individual galaxies. We also derive the attenuation curve for subpopulations of the main sample, separated according to mean stellar population age (via D 4000 n ), specific star formation rate, stellar mass, and metallicity, and find that they show only tentative trends with low significance, at least over the range that is probed by our sample. These results indicate that a single curve is reasonable for applications seeking to broadly characterize large samples of galaxies in the local universe, while applications to individual galaxies would yield large uncertainties and is not recommended.

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“…This code utilises adaptive Cartesian grids to define the distributions of stars and dust and an optimization technique to set the angular density of rays cast from each source. The dust emission can be calculated both for dust in equilibrium with the radiation field and dust that is stochastically heated (Natale et al 2015). The current version of DART-Ray does not include dust self-heating and dust emission scattering.…”

Section: Dart-raymentioning

confidence: 99%

Trust

Gordon

Baes

Bianchi

et al. 2017

A&A

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Context. The radiative transport of photons through arbitrary three-dimensional (3D) structures of dust is a challenging problem due to the anisotropic scattering of dust grains and strong coupling between different spatial regions. The radiative transfer problem in 3D is solved using Monte Carlo or Ray Tracing techniques as no full analytic solution exists for the true 3D structures. Aims. We provide the first 3D dust radiative transfer benchmark composed of a slab of dust with uniform density externally illuminated by a star. This simple 3D benchmark is explicitly formulated to provide tests of the different components of the radiative transfer problem including dust absorption, scattering, and emission. Methods. The details of the external star, the slab itself, and the dust properties are provided. This benchmark includes models with a range of dust optical depths fully probing cases that are optically thin at all wavelengths to optically thick at most wavelengths. The dust properties adopted are characteristic of the diffuse Milky Way interstellar medium. This benchmark includes solutions for the full dust emission including single photon (stochastic) heating as well as two simplifying approximations: One where all grains are considered in equilibrium with the radiation field and one where the emission is from a single effective grain with size-distributionaveraged properties. A total of six Monte Carlo codes and one Ray Tracing code provide solutions to this benchmark. Results. The solution to this benchmark is given as global spectral energy distributions (SEDs) and images at select diagnostic wavelengths from the ultraviolet through the infrared. Comparison of the results revealed that the global SEDs are consistent on average to a few percent for all but the scattered stellar flux at very high optical depths. The image results are consistent within 10%, again except for the stellar scattered flux at very high optical depths. The lack of agreement between different codes of the scattered flux at high optical depths is quantified for the first time. Convergence tests using one of the Monte Carlo codes illustrate the sensitivity of the solutions to various model parameters. Conclusions. We provide the first 3D dust radiative transfer benchmark and validate the accuracy of this benchmark through comparisons between multiple independent codes and detailed convergence tests.

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Predicting the stellar and non-equilibrium dust emission spectra of high-resolution simulated galaxies with dart-ray

Cited by 40 publications

References 115 publications

Planckintermediate results

Planckintermediate results

Characterizing Dust Attenuation in Local Star-forming Galaxies: Near-infrared Reddening and Normalization

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