Detalles de publicación
PP 019010
The MUSE Atlas of Disks (MAD): Resolving Star Formation Rates and Gas Metallicities on < 100pc Scales
(1)Department of Physics, ETH,
(2)Leibniz-Institut fur Astrophysik Potsdam (AIP),
(3)Subaru Telescope, National Astronomical Observatory of Japan,
(4)Leiden Observatory,
(5) Instituto de Astrofísica e Ciências do Espaco,
(6) Instituto de Astrofísica de Canarias,
(7) Departamento de Astrofísica, Universidad de La Laguna,
(8) Dept. of Physics & Astronomy, University of Victoria,
(9)Astronomy Centre, Department of Physics and Astronomy, University of Sussex,
(10)Jeremiah Horrocks Institute, University of Central Lancashire,
(11)Univ Lyon, Univ Lyon1, Ens de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon,
(12)Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA
We study the physical properties of the ionized gas in local disks using the sample of 38 nearby ∼ 108.5−11.2M Star-Forming Main Sequence (SFMS) galaxies observed so far as part of the MUSE Atlas of Disks (MAD). Specifically, we use all strong emission lines in the MUSE wavelength range 4650-9300 ˚A to investigate the resolved ionized gas properties on ∼ 100 pc scales. This spatial resolution enables us to disentangle Hii
regions from the Diffuse Ionized Gas (DIG) in the computation of gas metallicities and Star Formation Rates (SFRs) of star forming regions. The gas metallicities generally decrease with radius. The metallicity of the Hii
regions is on average ∼0.1 dex higher than that of the DIG, but the metallicity radial gradient in both components is similar. The mean metallicities within the inner galaxy cores correlate with the total stellar mass of the galaxies. On our < 100 pc scales, we find two correlations previously reported at kpc scales: a spatially resolved MassMetallicity Relation (RMZR) and a spatially resolved SFMS (RSFMS). We find no secondary dependency of the RMZR with the SFR density. We find that both resolved relations have a local origin, as they do not depend on the total stellar mass. The observational results of this paper are consistent with the inside-out scenario for the growth of galactic disks.
regions from the Diffuse Ionized Gas (DIG) in the computation of gas metallicities and Star Formation Rates (SFRs) of star forming regions. The gas metallicities generally decrease with radius. The metallicity of the Hii
regions is on average ∼0.1 dex higher than that of the DIG, but the metallicity radial gradient in both components is similar. The mean metallicities within the inner galaxy cores correlate with the total stellar mass of the galaxies. On our < 100 pc scales, we find two correlations previously reported at kpc scales: a spatially resolved MassMetallicity Relation (RMZR) and a spatially resolved SFMS (RSFMS). We find no secondary dependency of the RMZR with the SFR density. We find that both resolved relations have a local origin, as they do not depend on the total stellar mass. The observational results of this paper are consistent with the inside-out scenario for the growth of galactic disks.