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|Title:||Resolving the age bimodality of galaxy stellar populations on kpc scales||Authors:||ZIBETTI, Stefano
GALLAZZI, Anna Rita
García Benito, R.
de Lorenzo-Cáceres, A.
Marino, R. A.
Sánchez, S. F.
van de Ven, G.
Walcher, C. J.
|Issue Date:||2017||Journal:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY||Number:||468||Issue:||2||First Page:||1902||Abstract:||Galaxies in the local Universe are known to follow bimodal distributions in the global stellar population properties. We analyse the distribution of the local average stellar population ages of 654 053 sub-galactic regions resolved on ∼1 kpc scales in a volume-corrected sample of 394 galaxies, drawn from the Calar Alto Legacy Integral Field Area (CALIFA) DR3 integral-field-spectroscopy survey and complemented by Sloan Digital Sky Survey (SDSS) imaging. We find a bimodal local-age distribution, with an old and a young peak primarily due to regions in early-type galaxies and star-forming regions of spirals, respectively. Within spiral galaxies, the older ages of bulges and interarm regions relative to spiral arms support an internal age bimodality. Although regions of higher stellar mass surface density, μ<SUB>*</SUB>, are typically older, μ<SUB>*</SUB> alone does not determine the stellar population age and a bimodal distribution is found at any fixed μ<SUB>*</SUB>. We identify an 'old ridge' of regions of age ∼9 Gyr, independent of μ<SUB>*</SUB>, and a 'young sequence' of regions with age increasing with μ<SUB>*</SUB> from 1-1.5 to 4-5 Gyr. We interpret the former as regions containing only old stars, and the latter as regions where the relative contamination of old stellar populations by young stars decreases as μ<SUB>*</SUB> increases. The reason why this bimodal age distribution is not inconsistent with the unimodal shape of the cosmic-averaged star formation history is that (I) the dominating contribution by young stars biases the age low with respect to the average epoch of star formation, and (II) the use of a single average age per region is unable to represent the full time extent of the star formation history of 'young sequence' regions.||URI:||http://hdl.handle.net/20.500.12386/27949||URL:||https://academic.oup.com/mnras/article/468/2/1902/2962445||ISSN:||0035-8711||DOI:||10.1093/mnras/stx251||Bibcode ADS:||2017MNRAS.468.1902Z||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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checked on Jan 23, 2021
checked on Jan 23, 2021
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