High-resolution, 3D radiative transfer modelling. II. The early-type spiral galaxy M81. Verstocken, S., Nersesian, A., Baes, M., Viaene, S., Bianchi, S., Casasola, V., Clark, C. J. R., Davies, J. I., De Looze, I., De Vis, P., Dobbels, W., Galliano, F., Jones, A. P., Madden, S. C., Mosenkov, A. V., Trčka, A., & Xilouris, E. M. arXiv e-prints, 2004:arXiv:2004.03615, April, 2020. ![High-resolution, 3D radiative transfer modelling. II. The early-type spiral galaxy M81 [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper abstract bibtex Interstellar dust absorbs stellar light very efficiently and thus shapes the energetic output of galaxies. Studying the impact of different stellar populations on the dust heating remains hard because it requires decoupling the relative geometry of stars and dust, and involves complex processes as scattering and non-local dust heating. We aim to constrain the relative distribution of dust and stellar populations in the spiral galaxy M81 and create a realistic model of the radiation field that describes the observations. Investigating the dust-starlight interaction on local scales, we want to quantify the contribution of young and old stellar populations to the dust heating. We aim to standardise the setup and model selection of such inverse radiative transfer simulations so this can be used for comparable modelling of other nearby galaxies. We present a semi-automated radiative transfer modelling pipeline that implements the necessary steps such as the geometric model construction and the normalisation of the components through an optimisation routine. We use the Monte Carlo radiative transfer code SKIRT to calculate a self-consistent, panchromatic model of the interstellar radiation field. By looking at different stellar populations independently, we can quantify to what extent different stellar age populations contribute to the dust heating. Our method takes into account the effects of non-local heating. We obtain a realistic 3D radiative transfer model of the face-on galaxy M81. We find that only 50.2\textbackslash% of the dust heating can be attributed to young stellar populations. We confirm a tight correlation between the specific star formation rate and the heating fraction by young stellar populations, both in sky projection and in 3D, also found for radiative transfer models of M31 and M51. We conclude that... (abridged)
@article{verstocken_high-resolution_2020,
title = {High-resolution, {3D} radiative transfer modelling. {II}. {The} early-type spiral galaxy {M81}},
volume = {2004},
url = {http://adsabs.harvard.edu/abs/2020arXiv200403615V},
abstract = {Interstellar dust absorbs stellar light very efficiently and thus shapes
the energetic output of galaxies. Studying the impact of different
stellar populations on the dust heating remains hard because it requires
decoupling the relative geometry of stars and dust, and involves complex
processes as scattering and non-local dust heating. We aim to constrain
the relative distribution of dust and stellar populations in the spiral
galaxy M81 and create a realistic model of the radiation field that
describes the observations. Investigating the dust-starlight interaction
on local scales, we want to quantify the contribution of young and old
stellar populations to the dust heating. We aim to standardise the setup
and model selection of such inverse radiative transfer simulations so
this can be used for comparable modelling of other nearby galaxies. We
present a semi-automated radiative transfer modelling pipeline that
implements the necessary steps such as the geometric model construction
and the normalisation of the components through an optimisation routine.
We use the Monte Carlo radiative transfer code SKIRT to calculate a
self-consistent, panchromatic model of the interstellar radiation field.
By looking at different stellar populations independently, we can
quantify to what extent different stellar age populations contribute to
the dust heating. Our method takes into account the effects of non-local
heating. We obtain a realistic 3D radiative transfer model of the
face-on galaxy M81. We find that only 50.2{\textbackslash}\% of the dust heating can be
attributed to young stellar populations. We confirm a tight correlation
between the specific star formation rate and the heating fraction by
young stellar populations, both in sky projection and in 3D, also found
for radiative transfer models of M31 and M51. We conclude that...
(abridged)},
urldate = {2020-04-13},
journal = {arXiv e-prints},
author = {Verstocken, Sam and Nersesian, Angelos and Baes, Maarten and Viaene, Sébastien and Bianchi, Simone and Casasola, Viviana and Clark, Christopher J. R. and Davies, Jonathan I. and De Looze, Ilse and De Vis, Pieter and Dobbels, Wouter and Galliano, FrédÉric and Jones, Anthony P. and Madden, Suzanne C. and Mosenkov, Aleksandr V. and Trčka, Ana and Xilouris, Emmanuel M.},
month = apr,
year = {2020},
keywords = {Astrophysics - Astrophysics of Galaxies},
pages = {arXiv:2004.03615},
}
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Studying the impact of different stellar populations on the dust heating remains hard because it requires decoupling the relative geometry of stars and dust, and involves complex processes as scattering and non-local dust heating. We aim to constrain the relative distribution of dust and stellar populations in the spiral galaxy M81 and create a realistic model of the radiation field that describes the observations. Investigating the dust-starlight interaction on local scales, we want to quantify the contribution of young and old stellar populations to the dust heating. We aim to standardise the setup and model selection of such inverse radiative transfer simulations so this can be used for comparable modelling of other nearby galaxies. We present a semi-automated radiative transfer modelling pipeline that implements the necessary steps such as the geometric model construction and the normalisation of the components through an optimisation routine. We use the Monte Carlo radiative transfer code SKIRT to calculate a self-consistent, panchromatic model of the interstellar radiation field. By looking at different stellar populations independently, we can quantify to what extent different stellar age populations contribute to the dust heating. Our method takes into account the effects of non-local heating. We obtain a realistic 3D radiative transfer model of the face-on galaxy M81. We find that only 50.2\\textbackslash% of the dust heating can be attributed to young stellar populations. We confirm a tight correlation between the specific star formation rate and the heating fraction by young stellar populations, both in sky projection and in 3D, also found for radiative transfer models of M31 and M51. We conclude that... (abridged)","urldate":"2020-04-13","journal":"arXiv e-prints","author":[{"propositions":[],"lastnames":["Verstocken"],"firstnames":["Sam"],"suffixes":[]},{"propositions":[],"lastnames":["Nersesian"],"firstnames":["Angelos"],"suffixes":[]},{"propositions":[],"lastnames":["Baes"],"firstnames":["Maarten"],"suffixes":[]},{"propositions":[],"lastnames":["Viaene"],"firstnames":["Sébastien"],"suffixes":[]},{"propositions":[],"lastnames":["Bianchi"],"firstnames":["Simone"],"suffixes":[]},{"propositions":[],"lastnames":["Casasola"],"firstnames":["Viviana"],"suffixes":[]},{"propositions":[],"lastnames":["Clark"],"firstnames":["Christopher","J.","R."],"suffixes":[]},{"propositions":[],"lastnames":["Davies"],"firstnames":["Jonathan","I."],"suffixes":[]},{"propositions":[],"lastnames":["De","Looze"],"firstnames":["Ilse"],"suffixes":[]},{"propositions":[],"lastnames":["De","Vis"],"firstnames":["Pieter"],"suffixes":[]},{"propositions":[],"lastnames":["Dobbels"],"firstnames":["Wouter"],"suffixes":[]},{"propositions":[],"lastnames":["Galliano"],"firstnames":["FrédÉric"],"suffixes":[]},{"propositions":[],"lastnames":["Jones"],"firstnames":["Anthony","P."],"suffixes":[]},{"propositions":[],"lastnames":["Madden"],"firstnames":["Suzanne","C."],"suffixes":[]},{"propositions":[],"lastnames":["Mosenkov"],"firstnames":["Aleksandr","V."],"suffixes":[]},{"propositions":[],"lastnames":["Trčka"],"firstnames":["Ana"],"suffixes":[]},{"propositions":[],"lastnames":["Xilouris"],"firstnames":["Emmanuel","M."],"suffixes":[]}],"month":"April","year":"2020","keywords":"Astrophysics - Astrophysics of Galaxies","pages":"arXiv:2004.03615","bibtex":"@article{verstocken_high-resolution_2020,\n\ttitle = {High-resolution, {3D} radiative transfer modelling. {II}. {The} early-type spiral galaxy {M81}},\n\tvolume = {2004},\n\turl = {http://adsabs.harvard.edu/abs/2020arXiv200403615V},\n\tabstract = {Interstellar dust absorbs stellar light very efficiently and thus shapes \nthe energetic output of galaxies. Studying the impact of different\nstellar populations on the dust heating remains hard because it requires\ndecoupling the relative geometry of stars and dust, and involves complex\nprocesses as scattering and non-local dust heating. We aim to constrain\nthe relative distribution of dust and stellar populations in the spiral\ngalaxy M81 and create a realistic model of the radiation field that\ndescribes the observations. Investigating the dust-starlight interaction\non local scales, we want to quantify the contribution of young and old\nstellar populations to the dust heating. We aim to standardise the setup\nand model selection of such inverse radiative transfer simulations so\nthis can be used for comparable modelling of other nearby galaxies. We\npresent a semi-automated radiative transfer modelling pipeline that\nimplements the necessary steps such as the geometric model construction\nand the normalisation of the components through an optimisation routine.\nWe use the Monte Carlo radiative transfer code SKIRT to calculate a\nself-consistent, panchromatic model of the interstellar radiation field.\nBy looking at different stellar populations independently, we can\nquantify to what extent different stellar age populations contribute to\nthe dust heating. Our method takes into account the effects of non-local\nheating. We obtain a realistic 3D radiative transfer model of the\nface-on galaxy M81. We find that only 50.2{\\textbackslash}\\% of the dust heating can be\nattributed to young stellar populations. We confirm a tight correlation\nbetween the specific star formation rate and the heating fraction by\nyoung stellar populations, both in sky projection and in 3D, also found\nfor radiative transfer models of M31 and M51. 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