The MUSE Atlas of Disks (MAD): resolving star formation rates and gas metallicities on <100 pc scales†. Issue 4 (21st January 2019)

• Record Type: Journal Article
• Authors: Erroz-Ferrer, Santiago; Carollo, C Marcella; den Brok, Mark; Onodera, Masato; Brinchmann, Jarle; Marino, Raffaella A; Monreal-Ibero, Ana; Schaye, Joop; Woo, Joanna; Cibinel, Anna; Debattista, Victor P; Inami, Hanae; Maseda, Michael; Richard, Johan; Tacchella, Sandro; Wisotzki, Lutz
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 484:Issue 4(2019)
• Page Start: 5009
• Page End: 5027
• Publication Date: 2019-01-21
• Subjects: galaxies: abundances -- galaxies: general -- galaxies: spiral -- galaxies: star formation -- ISM: H ii regions; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stz194
• Languages: English
• ISSNs: 0035-8711

Abstract

Abstract: We study the physical properties of the ionized gas in local discs using the sample of 38 nearby ∼10 8.5–11.2 M⊙ 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 Å to investigate the resolved ionized gas properties on ∼100 pc scales. This spatial resolution enables us to disentangle H ii 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 H ii 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 mass–metallicity relation (RMZR) and a spatially resolved SFMS (RSFMS). We find no secondary dependence 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.