Hostname: page-component-6bf8c574d5-8gtf8 Total loading time: 0 Render date: 2025-02-18T00:17:15.146Z Has data issue: false hasContentIssue false
  • English
  • Français

SDSS-IV MaNGA: Testing the Metallicity Distribution across the Merging Sequence

Published online by Cambridge University Press:  03 March 2020

Jorge K. Barrera-Ballesteros ,
Li-hwai Lin ,
Bu-Ching Hsieh ,
Hsi-An Pan ,
Sebastian Sánchez  and
Timothy Heckman
Jorge K. Barrera-Ballesteros
Affiliation:
Dept. of Physics and Astronomy, Johns Hopkins University, 3400 N Charles St., Baltimore, MD21218, USA email: [email protected]
Li-hwai Lin
Affiliation:
Academia Sinica, Institute of Astronomy & Astrophysics (ASIAA), P.O. Box Box 23-141, Taipei10617, Taiwan
Bu-Ching Hsieh
Affiliation:
Academia Sinica, Institute of Astronomy & Astrophysics (ASIAA), P.O. Box Box 23-141, Taipei10617, Taiwan
Hsi-An Pan
Affiliation:
Academia Sinica, Institute of Astronomy & Astrophysics (ASIAA), P.O. Box Box 23-141, Taipei10617, Taiwan
Sebastian Sánchez
Affiliation:
Instituto de Astronomía, Universidad Nacional Autonoma deMexico
Timothy Heckman
Affiliation:
Dept. of Physics and Astronomy, Johns Hopkins University, 3400 N Charles St., Baltimore, MD21218, USA email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Interactions and mergers have been known as key scenarios to enhance global star formation rates and to lower the metal content of galaxies. However, little is known on how interactions affect the spatial distribution of gas metallicities. Thanks to the SDSS-IV MaNGA survey we are able to statistically constrain the impact of interactions across the optical distributions of galaxies. In this study, we compare the radial distribution of the ionized gas metallicity from a sample of 329 interacting objects – covering different interaction stages – with a statistical robust control sample. Our results suggest that galaxies close to coalesce tend to have flat, lower metallicities than non-interacting star-forming galaxies.

Keywords

Galaxy: evolutiongalaxies: interactionsgalaxies: abundances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium A30: Astronomy in Focus XXX , August 2018 , pp. 263 - 264
Copyright
© International Astronomical Union 2020

References

Ellison, S., Patton, D., Simmard, L., & McConnachie, W. 2008, ApJ, 135, 1877 CrossRefGoogle Scholar