The global dust modelling framework THEMIS

Jones, A. P.; Koehler, Melanie; Ysard, N.; Bocchio, Marco; Verstraete, L.

doi:10.1051/0004-6361/201630225

Cited by 257 publications

(363 citation statements)

References 159 publications

(260 reference statements)

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“…Nonetheless IRAS photometry is valuable for DustPedia, particularly in the 60 µm band; fluxes in this part of the spectrum are important for constraining dust emission and properties (see Jones et al 2016Jones et al , 2017, and references therein).…”

Section: Iras Scanpi Photometrymentioning

confidence: 99%

“…DustPedia is combining cutting-edge methods for studying dust: physically-motivated dust modelling with The Heterogeneous Evolution Model for Interstellar Solids (THEMIS; Jones et al 2016;Jones et al 2017;Ysard et al 2016); hierarchical Bayesian spectral energy distribution (SED) fitting with Hierarchial Bayesian Inference for dust Emission (HerBIE; Galliano et al, in prep. ); and 3-dimensional radiative transfer modelling and fitting with Stellar Kinematics Including Radiative Transfer (SKIRT; Baes et al 2011;Camps & Baes 2015) and FitSKIRT (De Geyter et al 2013).…”

Section: Introductionmentioning

confidence: 99%

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

Clark

Verstocken

Bianchi

et al. 2018

A&A

Self Cite

117

190

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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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Section: Iras Scanpi Photometrymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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

Clark

Verstocken

Bianchi

et al. 2018

A&A

Self Cite

117

190

View full text Add to dashboard Cite

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“…We adopted the optical properties and grain size distributions of the THEMIS 13 dust model, as described in Jones et al (2013) and successive updates (Köhler et al 2014;Ysard et al 2015;Jones et al 2017). We assumed that the emission is due to grains exposed to a radiation field with the same spectrum as that of the local interstellar radiation field (LISRF, Mathis et al 1983), and intensity scaled up and down via the parameter U to account for different heating environments within the galaxy (U=1 for the same conditions as in the Solar neighborhood).…”

Section: Dust Massmentioning

confidence: 99%

Radial distribution of dust, stars, gas, and star-formation rate in DustPedia face-on galaxies

Casasola

Cassarà

Bianchi

et al. 2017

A&A

Self Cite

128

140

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Aims. The purpose of this work is the characterization of the radial distribution of dust, stars, gas, and star-formation rate (SFR) in a sub-sample of 18 face-on spiral galaxies extracted from the DustPedia sample. Methods. This study is performed by exploiting the multi-wavelength, from ultraviolet (UV) to sub-millimeter bands, DustPedia database, in addition to molecular ( 12 CO) and atomic (Hi) gas maps and metallicity abundance information available in the literature. We fitted the surface brightness profiles of the tracers of dust and stars, the mass surface density profiles of dust, stars, molecular gas, and total gas, and the SFR surface density profiles with an exponential curve and derived their scale-lengths. We also developed a method to solve for the CO-to-H 2 conversion factor (α CO ) per galaxy by using dust and gas mass profiles. Results. Although each galaxy has its own peculiar behaviour, we identified a common trend of the exponential scale-lengths vs. wavelength. On average, the scale-lengths normalized to the B-band 25 mag/arcsec 2 radius decrease from UV to 70 µm, from 0.4 to 0.2, and then increase back up to ∼0.3 at 500 microns. The main result is that, on average, the dust mass surface density scale-length is about 1.8 times the stellar one derived from IRAC data and the 3.6 µm surface brightness, and close to that in the UV. We found a mild dependence of the scale-lengths on the Hubble stage T: the scale-lengths of the Herschel bands and the 3.6 µm scale-length tend to increase from earlier to later types, the scale-length at 70 µm tends to be smaller than that at longer sub-mm wavelength with ratios between longer sub-mm wavelengths and 70 µm that decrease with increasing T. The scale-length ratio of SFR and stars shows a weak increasing trend towards later types. Our α CO determinations are in the range (0.3 − 9) M pc −2 (K km s −1 ) −1 , almost invariant by using a fixed dust-to-gas ratio mass (DGR) or a DGR depending on metallicity gradient.

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“…A much more detailed model for the volatile carbonaceous component of the interstellar medium (ISM) dust is developed in Jones et al (2013Jones et al ( , 2014, Jones (2016), Köhler et al (2015), and Ysard et al (2015). An overview on this model is given in Jones et al (2017). The solid material of accretion disks around newly formed stars is derived from such material, although this material is probably somewhat modified in the parent molecular cloud and during the collapse phase to the proto-star before it is added to the disc.…”

Section: Introductionmentioning

confidence: 99%

Spatial distribution of carbon dust in the early solar nebula and the carbon content of planetesimals

Gail

Trieloff

2017

A&A

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Context. A high fraction of carbon bound in solid carbonaceous material is observed to exist in bodies formed in the cold outskirts of the solar nebula, while bodies in the region of terrestrial planets contain only very small mass fractions of carbon. Most of the solid carbon component is lost and converted into CO during the spiral-in of matter as the Sun accretes matter from the solar nebula. Aims. We study the fate of the carbonaceous material that entered the proto-solar disc by comparing the initial carbon abundance in primitive solar system material and the abundance of residual carbon in planetesimals and planets in the asteroid belt and the terrestrial planet region. Methods. We constructed a model for the composition of the pristine carbonaceous material from observational data on the composition of the dust component in comets and of interplanetary dust particles and from published data on pyrolysis experiments. This material entered the inner parts of the solar nebula during the course of the build-up of the proto-sun by accreting matter from the proto-stellar disc. Based on a one-zone evolution model of the solar nebula, we studied the pyrolysis of the refractory and volatile organic component and the concomitant release of hydrocarbons of high molecular weight under quiescent conditions of disc evolution, while matter migrates into the central parts of the solar nebula. We also studied the decomposition and oxidation of the carbonaceous material during violent flash heating events, which are thought to be responsible for the formation of chondrules. To do this, we calculated pyrolysis and oxidation of the carbonaceous material in temperature spikes that were modeled according to cosmochemical models for the temperature history of chondrules. Results. We find that the complex hydrocarbon components of the carbonaceous material are removed from the disc matter in the temperature range between 250 and 400 K, but the amorphous carbon component survives to temperatures of 1200 K. Without efficient carbon destruction during flash-heating associated with chondrule formation, the carbon abundance of terrestrial planets, except for Mercury, would be of several percent and not as low as it is found in cosmochemical studies. Chondrule formation seems to be a crucial process for the carbon-poor composition of the material of terrestrial planets.

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The global dust modelling framework THEMIS

Cited by 257 publications

References 159 publications

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

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

Radial distribution of dust, stars, gas, and star-formation rate in DustPedia face-on galaxies

Spatial distribution of carbon dust in the early solar nebula and the carbon content of planetesimals

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