A Bayesian chemical evolution model of the DustPedia Galaxy M74. (arXiv:2305.05680v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Calura_F/0/1/0/all/0/1">Francesco Calura</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Palla_M/0/1/0/all/0/1">Marco Palla</a> (2,1), <a href="http://arxiv.org/find/astro-ph/1/au:+Morselli_L/0/1/0/all/0/1">Laura Morselli</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Spitoni_E/0/1/0/all/0/1">Emanuele Spitoni</a> (4,5), <a href="http://arxiv.org/find/astro-ph/1/au:+Casasola_V/0/1/0/all/0/1">Viviana Casasola</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Verma_K/0/1/0/all/0/1">Kuldeep Verma</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Enia_A/0/1/0/all/0/1">Andrea Enia</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Meneghetti_M/0/1/0/all/0/1">Massimo Meneghetti</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Bianchi_S/0/1/0/all/0/1">Simone Bianchi</a> (8), <a href="http://arxiv.org/find/astro-ph/1/au:+Pozzi_F/0/1/0/all/0/1">Francesca Pozzi</a> (9), <a href="http://arxiv.org/find/astro-ph/1/au:+Gruppioni_C/0/1/0/all/0/1">Carlotta Gruppioni</a> (1) ((1) INAF-OAS, Bologna, Italy, (2) Ghent University, Belgium, (3) CINECA, Italy, (4) INAF-OA Trieste, Italy, (5) Universite' Cote d'Azur, France, (6) INAF-IRA, Bologna, Italy, (7) Indian Institute of Technology, Varanasi, India, (8) INAF-OA Arcetri, Firenze, Italy, (9) Universita' di Bologna, Italy)
We introduce a new, multi-zone chemical evolution model of the DustPedia
galaxy M74, calibrated by means of MCMC methods.
We take into account the observed stellar and gas density profiles and use
Bayesian analysis to constrain two fundamental parameters characterising the
gas accretion and star formation timescale, i.e. the infall timescale tau and
the SF efficiency nu, respectively, as a function of galactocentric radius R.
Our analysis supports an infall timescale increasing with R and a star
formation efficiency decreasing with R, thus supporting an ‘Inside-Out’
formation for M74. For both tau and nu, we find a weaker radial dependence than
in the Milky Way.
We also investigate the dust content of M74, comparing the observed dust
density profile with the results of our chemical evolution models. Various
prescriptions have been considered for two key parameters, i.e. the typical
dust accretion timescale and the mass of gas cleared out of the dust by a
supernova remnant, regulating the dust growth and destruction rate,
respectively. Two models with a different current balance between destruction
and accretion, i.e. with equilibrium and dominion of accretion over
destruction, can equally reproduce the observed dust profile of M74. This
outlines the degeneracy between these parameters in shaping the interstellar
dust content in galaxies. Our methods will be extended to more DustPedia
galaxies to shed more light on the relative roles of dust production and
destruction.
We introduce a new, multi-zone chemical evolution model of the DustPedia
galaxy M74, calibrated by means of MCMC methods.
We take into account the observed stellar and gas density profiles and use
Bayesian analysis to constrain two fundamental parameters characterising the
gas accretion and star formation timescale, i.e. the infall timescale tau and
the SF efficiency nu, respectively, as a function of galactocentric radius R.
Our analysis supports an infall timescale increasing with R and a star
formation efficiency decreasing with R, thus supporting an ‘Inside-Out’
formation for M74. For both tau and nu, we find a weaker radial dependence than
in the Milky Way.
We also investigate the dust content of M74, comparing the observed dust
density profile with the results of our chemical evolution models. Various
prescriptions have been considered for two key parameters, i.e. the typical
dust accretion timescale and the mass of gas cleared out of the dust by a
supernova remnant, regulating the dust growth and destruction rate,
respectively. Two models with a different current balance between destruction
and accretion, i.e. with equilibrium and dominion of accretion over
destruction, can equally reproduce the observed dust profile of M74. This
outlines the degeneracy between these parameters in shaping the interstellar
dust content in galaxies. Our methods will be extended to more DustPedia
galaxies to shed more light on the relative roles of dust production and
destruction.
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