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High-resolution, 3D radiative transfer modeling of M51

Published online by Cambridge University Press:  09 February 2015

Ilse De Looze
Affiliation:
Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, B-9000Gent, Belgium
Jacopo Fritz
Affiliation:
Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, B-9000Gent, Belgium
Maarten Baes
Affiliation:
Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, B-9000Gent, Belgium
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Abstract

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We present a new technique developed to model the radiative transfer (RT) effects in nearby face-on galaxies. The face-on perspective provides insight into the star-forming regions and clumpy structure, imposing the need for high-resolution 3D models to recover the asymmetric stellar and dust geometries observed in galaxies. RT modeling of the continuum emission of stars and its interaction with the embedding dust in a galaxy's interstellar medium enables a self-consistent study of the main dust heating mechanisms in galaxies. The main advantage of RT calculations is the non-local character of dust heating that can be addressed by tracing the propagation of stellar radiation through the dusty galaxy medium.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2015 

References

Baes, M., Verstappen, J., De Looze, I., et al. 2011, ApJS, 196, 22CrossRefGoogle Scholar