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Carbon and oxygen in H ii regions of the Magellanic Clouds: abundance discrepancy and chemical evolution

Abstract We present C and O abundances in the Magellanic Clouds derived from deep spectra of H ii regions. The data have been taken with the Ultraviolet-Visual Echelle Spectrograph at the 8.2-m Very Large Telescope. The sample comprises five H ii regions in the Large Magellanic Cloud (LMC) and four...

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Published in:Monthly notices of the Royal Astronomical Society 2017-06, Vol.467 (3), p.3759-3774
Main Authors: Toribio San Cipriano, L., Domínguez-Guzmán, G., Esteban, C., García-Rojas, J., Mesa-Delgado, A., Bresolin, F., Rodríguez, M., Simón-Díaz, S.
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cited_by cdi_FETCH-LOGICAL-c267t-926450c4d423db57c463273303628703a1012ba737d658da9188b533279842013
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container_issue 3
container_start_page 3759
container_title Monthly notices of the Royal Astronomical Society
container_volume 467
creator Toribio San Cipriano, L.
Domínguez-Guzmán, G.
Esteban, C.
García-Rojas, J.
Mesa-Delgado, A.
Bresolin, F.
Rodríguez, M.
Simón-Díaz, S.
description Abstract We present C and O abundances in the Magellanic Clouds derived from deep spectra of H ii regions. The data have been taken with the Ultraviolet-Visual Echelle Spectrograph at the 8.2-m Very Large Telescope. The sample comprises five H ii regions in the Large Magellanic Cloud (LMC) and four in the Small Magellanic Cloud (SMC). We measure pure recombination lines (RLs) of C ii and O ii in all the objects, permitting to derive the abundance discrepancy factors (ADFs) for O2+, as well as their O/H, C/H and C/O ratios. We compare the ADFs with those of other H ii regions in different galaxies. The results suggest a possible metallicity dependence of the ADF for the low-metallicity objects; but more uncertain for high-metallicity objects. We compare nebular and B-type stellar abundances and we find that the stellar abundances agree better with the nebular ones derived from collisionally excited lines (CELs). Comparing these results with other galaxies we observe that stellar abundances seem to agree better with the nebular ones derived from CELs in low-metallicity environments and from RLs in high-metallicity environments. The C/H, O/H and C/O ratios show almost flat radial gradients, in contrast with the spiral galaxies where such gradients are negative. We explore the chemical evolution analysing C/O versus O/H and comparing with the results of H ii regions in other galaxies. The LMC seems to show a similar chemical evolution to the external zones of small spiral galaxies and the SMC behaves as a typical star-forming dwarf galaxy.
doi_str_mv 10.1093/mnras/stx328
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title Carbon and oxygen in H ii regions of the Magellanic Clouds: abundance discrepancy and chemical evolution
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