Nonparametric galaxy morphology from UV to submm wavelengths. (arXiv:2007.02012v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Baes_M/0/1/0/all/0/1">Maarten Baes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nersesian_A/0/1/0/all/0/1">Angelos Nersesian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Casasola_V/0/1/0/all/0/1">Viviana Casasola</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bianchi_S/0/1/0/all/0/1">Simone Bianchi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cassara_L/0/1/0/all/0/1">Letizia P. Cassarà</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Clark_C/0/1/0/all/0/1">Christopher J. R. Clark</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Looze_I/0/1/0/all/0/1">Ilse De Looze</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dobbels_W/0/1/0/all/0/1">Wouter Dobbels</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fritz_J/0/1/0/all/0/1">Jacopo Fritz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galametz_M/0/1/0/all/0/1">Maud Galametz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galliano_F/0/1/0/all/0/1">Frédéric Galliano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Madden_S/0/1/0/all/0/1">Suzanne C. Madden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mosenkov_A/0/1/0/all/0/1">Aleksandr V. Mosenkov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Viaene_S/0/1/0/all/0/1">Sébastien Viaene</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Trcka_A/0/1/0/all/0/1">Ana Trčka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xilouris_E/0/1/0/all/0/1">Emmanuel M. Xilouris</a>
We present the first nonparametric morphological analysis of a set of spiral
galaxies from UV to submm wavelengths. Our study is based on high-quality
multi-wavelength imaging for nine well-resolved spiral galaxies from the
DustPedia database, combined with nonparametric morphology indicators
calculated in a consistent way using the {tt{StatMorph}} package. We measure
the half-light radius, the concentration index, the asymmetry index, the
smoothness index, the Gini coefficient and the $M_{20}$ indicator in various
wavebands from UV to submm wavelengths, as well as in stellar mass, dust mass
and star formation rate maps. We find that the interstellar dust in galaxies is
distributed in a more extended, less centrally concentrated, more asymmetric,
and more clumpy way than the stars. This is particularly evident when comparing
morphological indicators based on the stellar mass and dust mass maps. This
should serve as a warning sign against treating the dust in galaxies as a
simple smooth component. We argue that the nonparametric galaxy morphology of
galaxies from UV to submm wavelengths is an interesting test for cosmological
hydrodynamics simulations.
We present the first nonparametric morphological analysis of a set of spiral
galaxies from UV to submm wavelengths. Our study is based on high-quality
multi-wavelength imaging for nine well-resolved spiral galaxies from the
DustPedia database, combined with nonparametric morphology indicators
calculated in a consistent way using the {tt{StatMorph}} package. We measure
the half-light radius, the concentration index, the asymmetry index, the
smoothness index, the Gini coefficient and the $M_{20}$ indicator in various
wavebands from UV to submm wavelengths, as well as in stellar mass, dust mass
and star formation rate maps. We find that the interstellar dust in galaxies is
distributed in a more extended, less centrally concentrated, more asymmetric,
and more clumpy way than the stars. This is particularly evident when comparing
morphological indicators based on the stellar mass and dust mass maps. This
should serve as a warning sign against treating the dust in galaxies as a
simple smooth component. We argue that the nonparametric galaxy morphology of
galaxies from UV to submm wavelengths is an interesting test for cosmological
hydrodynamics simulations.
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