Volume 652, August 2021
|Number of page(s)||5|
|Section||Letters to the Editor|
|Published online||19 August 2021|
Letter to the Editor
[α/Fe] traced by H II regions from the CALIFA survey
The connection between morphology and chemical abundance patterns
Instituto de Astronomía, Universidad Nacional Autonóma de México, AP 70-264, 04510 CDMX, Mexico
2 Universidad Nacional Autónoma de México, Instituto de Astronomía, AP 106, Ensenada, 22800 BC, Mexico
3 Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany
4 Instituto de Astrofísica de Andalucía (IAA/CSIC), Glorieta de la Astronomía s/n Aptdo. 3004, 18080 Granada, Spain
5 Departamento de Física Teórica y del Cosmos, Universidad de Granada, 18071 Granada, Spain
Accepted: 4 August 2021
Context. Differential enrichment between α and Fe-peak elements is known to be strongly connected with the shape of the star formation history (SFH), the star formation efficiency (SFE), the inflow and outflow of material, and even the shape of the initial mass function (IMF). However, beyond the Local Group, detailed explorations are mostly limited to early-type galaxies due to the lack of a good proxy for [α/Fe] in late-type ones, limiting our understanding of the chemical enrichment process.
Aims. We intent to extend the explorations of [α/Fe] to late-type galaxies in order to understand the details of the differential enrichment process.
Methods. We compare the gas-phase oxygen abundance with the luminosity-weighted stellar metallicity in an extensive catalogue of ∼25 000 H II regions extracted from the Calar Alto Legacy Integral Field Area (CALIFA) survey, an exploration that uses the integral-field spectroscopy of ∼900 galaxies and covers a wide range of masses and morphologies. This way, we define [O/Fe] as the ratio between both parameters, proposing it as an indirect proxy of the [α/Fe] ratio. This procedure is completely different from the one adopted to estimate [α/Fe] from high-resolution spectroscopic data for stars in our Galaxy.
Results. We illustrate how the [O/Fe] parameter describes the chemical enrichment process in spiral galaxies, finding that: (i) it follows the decreasing pattern with [Fe/H] reported for the [α/Fe] ratio and (ii) its absolute scale depends on the stellar mass and the morphology. We reproduce both patterns using two different chemical evolution models, considering that galaxies with different stellar masses and morphologies present either different SFHs, SFEs, and inflow and outflow rates or a different maximum stellar mass cut for the IMF. We will explore the differential chemical enrichment using this new proxy galaxy by galaxy and region by region in further studies.
Key words: galaxies: abundances / galaxies: evolution / galaxies: fundamental parameters / ISM: abundances / stars: abundances
© ESO 2021
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