dc.contributor.author | Masi, C. De | |
dc.contributor.author | Vincenzo, F. | |
dc.contributor.author | Matteucci, F. | |
dc.contributor.author | Rosani, G. | |
dc.contributor.author | Barbera, La | |
dc.contributor.author | Pasquali, A. | |
dc.contributor.author | Spitoni, E. | |
dc.date.accessioned | 2020-03-27T01:07:09Z | |
dc.date.available | 2020-03-27T01:07:09Z | |
dc.date.issued | 2019-02 | |
dc.identifier.citation | Masi , C D , Vincenzo , F , Matteucci , F , Rosani , G , Barbera , L , Pasquali , A & Spitoni , E 2019 , ' Is the IMF in ellipticals bottom-heavy? Clues from their chemical abundances ' , Monthly Notices of the Royal Astronomical Society , vol. 483 , no. 2 , sty3127 , pp. 2217–2235 . https://doi.org/10.1093/mnras/sty3127 | |
dc.identifier.issn | 0035-8711 | |
dc.identifier.other | PURE: 13877220 | |
dc.identifier.other | PURE UUID: af3a95f2-47eb-47ea-b843-e50d11edb30a | |
dc.identifier.other | ArXiv: http://arxiv.org/abs/1805.06841v1 | |
dc.identifier.other | Scopus: 85067049803 | |
dc.identifier.uri | http://hdl.handle.net/2299/22513 | |
dc.description | © 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. | |
dc.description.abstract | We tested the implementation of different initial mass functions (IMFs) in our model for the chemical evolution of ellipticals, with the aim of reproducing the observed relations of [Fe/H] and [Mg/Fe] abundances with galaxy mass in a sample of early-type galaxies selected from the SPIDER-SDSS catalogue. Abundances in the catalogue were derived from averaged spectra, obtained by stacking individual spectra according to central velocity dispersion, as a proxy of galaxy mass. We tested IMFs already used in a previous work, as well as two new models, based on low-mass tapered (‘bimodal’) IMFs, where the IMF becomes either (1) bottom-heavy in more massive galaxies, or (2) is time-dependent, switching from top-heavy to bottom-heavy in the course of galactic evolution. We found that observations could only be reproduced by models assuming either a constant, Salpeter IMF, or a time-dependent distribution, as other IMFs failed. We further tested the models by calculating their M/L ratios. We conclude that a constant, time-independent bottom-heavy IMF does not reproduce the data, especially the increase of the [α/Fe] ratio with galactic stellar mass, whereas a variable IMF, switching from top to bottom-heavy, can match observations. For the latter models, the IMF switch always occurs at the earliest possible considered time, i.e. tswitch = 0.1 Gyr. | en |
dc.format.extent | 19 | |
dc.language.iso | eng | |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | |
dc.subject | astro-ph.GA | |
dc.title | Is the IMF in ellipticals bottom-heavy? Clues from their chemical abundances | en |
dc.contributor.institution | School of Physics, Astronomy and Mathematics | |
dc.description.status | Peer reviewed | |
rioxxterms.version | VoR | |
rioxxterms.versionofrecord | https://doi.org/10.1093/mnras/sty3127 | |
rioxxterms.type | Journal Article/Review | |
herts.preservation.rarelyaccessed | true | |