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Mass and metallicity scaling relations of high redshift star-forming galaxies selected by GRBs

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posted on 2018-05-01, 09:23 authored by M. Arabsalmani, P. Møller, D. A. Perley, W. Freudling, J. P. U. Fynbo, E. L. Floc'h, M. A. Zwaan, S. Schulze, N. R. Tanvir, L. Christensen, A. J. Levan, P. Jakobsson, D. Malesani, Z. Cano, S. Covino, V. D'Elia, P. Goldoni, A. Gomboc, K. E. Heintz, M. Sparre, A. D. U. Postigo, S. D. Vergani
We present a comprehensive study of the relations between gas kinematics, metallicity, and stellar mass in a sample of 82 GRB-selected galaxies using absorption and emission methods. We find the velocity widths of both emission and absorption profiles to be a proxy of stellar mass. We also investigate the velocity-metallicity correlation and its evolution with redshift and find the correlation derived from emission lines to have a significantly smaller scatter compared to that found using absorption lines. Using 33 GRB hosts with measured stellar mass and metallicitiy, we study the mass-metallicity relation for GRB host galaxies in a stellar mass range of $10^{8.2} M_{\odot}$ to $10^{11.1} M_{\odot}$ and a redshift range of $ z\sim 0.3-3.4$. The GRB-selected galaxies appear to track the mass-metallicity relation of star forming galaxies but with an offset of 0.15 towards lower metallicities. This offset is comparable with the average error-bar on the metallicity measurements of the GRB sample and also the scatter on the MZ relation of the general population. It is hard to decide whether this relatively small offset is due to systematic effects or the intrinsic nature of GRB hosts. We also investigate the possibility of using absorption-line metallicity measurements of GRB hosts to study the mass-metallicity relation at high redshifts. Our analysis shows that the metallicity measurements from absorption methods can significantly differ from emission metallicities and assuming identical measurements from the two methods may result in erroneous conclusions.

Funding

We acknowledge the financial support from UnivEarthS Labex program at Sorbonne Paris Cit´e (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02). The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013)/ERC Grant agreement no. EGGS-278202. AdUP acknowledge support from the Spanish research project AYA 2014-58381-P, a Ram´on y Cajal fellowship, and a 2016 BBVA Foundation Grant for Researchers and Cultural Creators.

History

Citation

Monthly Notices of the Royal Astronomical Society, 2018, 473(3), pp. 3312–3324,

Author affiliation

/Organisation/COLLEGE OF SCIENCE AND ENGINEERING/Department of Physics and Astronomy

Version

  • VoR (Version of Record)

Published in

Monthly Notices of the Royal Astronomical Society

Publisher

Oxford University Press (OUP), Royal Astronomical Society

issn

0035-8711

eissn

1365-2966

Copyright date

2018

Available date

2018-08-25

Publisher version

https://academic.oup.com/mnras/article/473/3/3312/4222621

Language

en

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