DustPedia: A Definitive Study of Cosmic Dust in the Local Universe

Davies, J. I.; Baes, M.; Bianchi, S.; Jones, A. P.; Madden, S.; Xilouris, E. M.; Bocchio, Marco; Casasola, V.; Cassarà, L. P.; Clark, Christopher; Looze, I. De; Evans, R.; Fritz, J.; Galametz, M.; Galliano, F.; Lianou, S.; Mosenkov, Aleksandr V.; Smith, M.; Verstocken, Sam; Viaene, S.; Vika, Marina; Wagle, Gururaj A.; Ysard, N.

doi:10.1088/1538-3873/129/974/044102

Cited by 118 publications

(140 citation statements)

References 139 publications

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“…A number of papers have already used and made reference to the THEMIS model to explore the nature and evolution of interstellar dust in the Milky Way (Jones & Habart 2015;Jones et al 2016;Ysard et al 2016;Bianchi et al 2017;De Looze et al 2017) and within other galaxies (Bocchio et al 2016;Viaene et al 2016;Mosenkov et al 2016;Clark et al 2016;Davies et al 2016;Chastenet et al 2017). …”

Section: Future Developmentsmentioning

confidence: 99%

The global dust modelling framework THEMIS

Jones

Koehler

Ysard

et al. 2017

A&A

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257

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Here we introduce the interstellar dust modelling framework THEMIS (The Heterogeneous dust Evolution Model for Interstellar Solids), which takes a global view of dust and its evolution in response to the local conditions in interstellar media. This approach is built upon a core model that was developed to explain the dust extinction and emission in the diffuse interstellar medium. The model was then further developed to self-consistently include the effects of dust evolution in the transition to denser regions. The THEMIS approach is under continuous development and we are currently extending the framework to explore the implications of dust evolution in HII regions and the photon-dominated regions associated with star formation. We provide links to the THEMIS, DustEM and DustPedia websites where more information about the model, its input data and applications can be found.

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Section: Future Developmentsmentioning

confidence: 99%

The global dust modelling framework THEMIS

Jones

Koehler

Ysard

et al. 2017

A&A

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257

345

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“…Full details of our Herschel data reduction process are provided in Davies et al (2017); here we provide only a brief summary, for the sake of completeness. For both Spectral and Photometric Imaging REceiver (SPIRE; Griffin et al 2010) and Photodetector Array Camera and Spectrometer (PACS; Poglitsch et al 2010) data, the Herschel Science Archive (HSA 6 ) was queried to find all Herschel photometer observations that provided coverage of each DustPedia galaxy.…”

Section: Herschel Imagerymentioning

confidence: 99%

DustPedia: Multiwavelength photometry and imagery of 875 nearby galaxies in 42 ultraviolet-microwave bands

Clark

Verstocken

Bianchi

et al. 2018

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Aims. The DustPedia project is capitalising on the legacy of the Herschel Space Observatory, using cutting-edge modelling techniques to study dust in the 875 DustPedia galaxies -representing the vast majority of extended galaxies within 3000 km s −1 that were observed by Herschel. This work requires a database of multiwavelength imagery and photometry that greatly exceeds the scope (in terms of wavelength coverage and number of galaxies) of any previous local-Universe survey. Methods. We constructed a database containing our own custom Herschel reductions, along with standardised archival observations from GALEX, SDSS, DSS, 2MASS, WISE, Spitzer, and Planck. Using these data, we performed consistent aperture-matched photometry, which we combined with external supplementary photometry from IRAS and Planck. Results. We present our multiwavelength imagery and photometry across 42 UV-microwave bands for the 875 DustPedia galaxies. Our aperture-matched photometry, combined with the external supplementary photometry, represents a total of 21 857 photometric measurements. A typical DustPedia galaxy has multiwavelength photometry spanning 25 bands. We also present the Comprehensive & Adaptable Aperture Photometry Routine (CAAPR), the pipeline we developed to carry out our aperture-matched photometry. CAAPR is designed to produce consistent photometry for the enormous range of galaxy and observation types in our data. In particular, CAAPR is able to determine robust cross-compatible uncertainties, thanks to a novel method for reliably extrapolating the aperture noise for observations that cover a very limited amount of background. Our rich database of imagery and photometry is being made available to the community.

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“…For the purposes of this work, we selected galaxies from the DustPedia sample (Davies et al 2017) with large angular diameters, so that they are well-resolved even at infrared and submm wavelengths. The sample consists of four nearby, spiral galaxies with a prominent bar in their centres; NGC 1365, M 83, M 95, and M 100.…”

Section: Galaxy Sample and Datamentioning

confidence: 99%

High-resolution, 3D radiative transfer modelling

Nersesian

Verstocken

Viaene

et al. 2020

A&A

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Context. Dust in late-type galaxies in the local Universe is responsible for absorbing approximately one third of the energy emitted by stars. It is often assumed that dust heating is mainly attributable to the absorption of ultraviolet and optical photons emitted by the youngest (≤ 100 Myr) stars. Consequently, thermal re-emission by dust at far-infrared wavelengths is often linked to the starformation activity of a galaxy. However, several studies argue that the contribution to dust heating by much older stellar populations might be more significant than previously thought. Advances in radiation transfer simulations finally allow us to actually quantify the heating mechanisms of diffuse dust by the stellar radiation field. Aims. As one of the main goals in the DustPedia project, we have developed a framework to construct detailed 3D stellar and dust radiative transfer models for nearby galaxies. In this study, we analyse the contribution of the different stellar populations to the dust heating in four nearby face-on barred galaxies: NGC 1365, M 83, M 95, and M 100. We aim to quantify the fraction directly related to young stellar populations, both globally and on local scales, and to assess the influence of the bar on the heating fraction. Methods. From 2D images we derive the 3D distributions of stars and dust. To model the complex geometries, we used SKIRT, a state-of-the-art 3D Monte Carlo radiative transfer code designed to self-consistently simulate the absorption, scattering, and thermal re-emission by the dust for arbitrary 3D distributions. Results. We derive global attenuation laws for each galaxy and confirm that galaxies of high specific star-formation rate have shallower attenuation curves and weaker UV bumps. On average, 36.5% of the bolometric luminosity is absorbed by dust in our galaxy sample. We report a clear effect of the bar structure on the radial profiles of the dust-heating fraction by the young stellar populations, and the dust temperature. We find that the young stellar populations are the main contributors to the dust heating, donating, on average ∼ 59% of their luminosity to this purpose throughout the galaxy. This dust-heating fraction drops to ∼ 53% in the bar region and ∼ 38% in the bulge region where the old stars are the dominant contributors to the dust heating. We also find a strong link between the heating fraction by the young stellar populations and the specific star-formation rate.

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DustPedia: A Definitive Study of Cosmic Dust in the Local Universe

Cited by 118 publications

References 139 publications

The global dust modelling framework THEMIS

The global dust modelling framework THEMIS

DustPedia: Multiwavelength photometry and imagery of 875 nearby galaxies in 42 ultraviolet-microwave bands

High-resolution, 3D radiative transfer modelling

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