SDSS-IV MaNGA: drivers of stellar metallicity in nearby galaxies
The distribution of stellar metallicities within and across galaxies is an excellent relic of the chemical evolution across cosmic time. We present a detailed analysis of spatially resolved stellar populations based on >2.6 million spatial bins from 7439 nearby galaxies in the Sloan Digital Sky S...
| Autores: | , , , , , , , , , , , , , , |
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| Formato: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2021 |
| País: | España |
| Recursos: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/261389 |
| Acesso em linha: | http://hdl.handle.net/10261/261389 |
| Access Level: | acceso abierto |
| Palavra-chave: | Techniques: spectroscopic Galaxies: abundances Galaxies: evolution Galaxies: statistics Galaxies: stellar content |
| Resumo: | The distribution of stellar metallicities within and across galaxies is an excellent relic of the chemical evolution across cosmic time. We present a detailed analysis of spatially resolved stellar populations based on >2.6 million spatial bins from 7439 nearby galaxies in the Sloan Digital Sky Survey-IV (SDSS-IV) Mapping Nearby Galaxies at APO (MaNGA) survey. To account for accurate inclination corrections, we derive an equation for morphology-dependent determination of galaxy inclinations. Our study goes beyond the well-known global mass-metallicity relation and radial metallicity gradients by providing a statistically sound exploration of local relations between stellar metallicity [Z/H], stellar surface mass density Σ∗, and galactocentric distance in the global mass-morphology plane. We find a significant resolved mass density-metallicity relation Σ ZR for galaxies of all types and masses above 109.8 M⊙. Different radial distances make an important contribution to the spread of the relation. Particularly, in low- and intermediate-mass galaxies, we find that at fixed Σ∗ metallicity increases with radius independently of morphology. For high masses, this radial dependence is only observed in high Σ∗ regions of spiral galaxies. This result calls for a driver of metallicity, in addition to Σ∗ that promotes chemical enrichment in the outer parts of galaxies more strongly than in the inner parts. We discuss gas accretion, outflows, recycling, and radial migration as possible scenarios. |
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