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http://hdl.handle.net/20.500.12386/27413
Titolo: | Revisiting the role of the thermally pulsating asymptotic-giant-branch phase in high-redshift galaxies | Autori: | Capozzi, Diego Maraston,Claudia Daddi, Emanuele Renzini, Alvio STRAZZULLO, VERONICA Gobat, Raphael |
Data pubblicazione: | 2016 | Rivista: | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | Numero: | 456 | Fascicolo: | 1 | Da pagina:: | 790 | Abstract: | We study the debated contribution from thermally pulsing asymptotic-giant-branch (TP-AGB) stars in evolutionary population synthesis models. We investigate the spectral energy distributions (SEDs) of a sample of 51 spectroscopically confirmed, high-z (1.3 < zspec < 2.7), galaxies using three evolutionary population synthesis models with strong, mild and light TP-AGB. Our sample is the largest of spectroscopically confirmed galaxies on which such models are tested so far. Galaxies were selected as passive, but we model them using a variety of star formation histories in order not to be dependent on this pre-selection. We find that the observed SEDs are best fitted with a significant contribution of TP-AGB stars or with substantial dust attenuation. Without including reddening, TP-AGB-strong models perform better and deliver solutions consistent within 1σ from the best-fitted ones in the vast majority of cases. Including reddening, all models perform similarly. Using independent constraints from observations in the mid- and far-IR, we show that low/negligible dust attenuation, I.e. E(B - V) ≲ 0.05, should be preferred for the SEDs of passively selected galaxies. Given that TP-AGB-light models give systematically older ages for passive galaxies, we suggest number counts of passive galaxies at higher redshifts as a further test to discriminate among stellar population models. | URI: | http://hdl.handle.net/20.500.12386/27413 | URL: | http://arxiv.org/abs/1511.05573v1 https://academic.oup.com/mnras/article/456/1/790/1070731 |
ISSN: | 0035-8711 | DOI: | 10.1093/mnras/stv2692 | Bibcode ADS: | 2016MNRAS.456..790C | Fulltext: | open |
È visualizzato nelle collezioni: | 1.01 Articoli in rivista |
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