The mass-metallicity relation of interacting galaxies

We study the mass-metallicity relation of galaxies in pairs and in isolation taken from the Sloan Digital Sky Survey-Data Release 4 (SDSS-DR4) using the stellar masses and oxygen abundances derived by Tremonti et al. Close galaxy pairs, defined by projected separation rp < 25 kpc h-1 and radi...

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Autores principales: Michel-Dansac, L., Lambas, D.G., Alonso, M.S., Tissera, P.
Formato: JOUR
Materias:
Galaxies: abundances
Galaxies: evolution
Galaxies: formation
Galaxies: interactions
Acceso en línea:http://hdl.handle.net/20.500.12110/paper_17453933_v386_n1_pL82_MichelDansac
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Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
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spelling todo:paper_17453933_v386_n1_pL82_MichelDansac2023-10-03T16:31:58Z The mass-metallicity relation of interacting galaxies Michel-Dansac, L. Lambas, D.G. Alonso, M.S. Tissera, P. Galaxies: abundances Galaxies: evolution Galaxies: formation Galaxies: interactions We study the mass-metallicity relation of galaxies in pairs and in isolation taken from the Sloan Digital Sky Survey-Data Release 4 (SDSS-DR4) using the stellar masses and oxygen abundances derived by Tremonti et al. Close galaxy pairs, defined by projected separation rp < 25 kpc h-1 and radial velocity ΔV < 350 km s-1, are morphologically classified according to the strength of the interaction signs. We find that only for pairs showing signs of strong interactions, the mass-metallicity relation differs significantly from that of galaxies in isolation. In such pairs, the mean gas-phase oxygen abundances of galaxies with low stellar masses (M* ≲ 109 M⊙ h-1) exhibit an excess of 0.2 dex. Conversely, at larger masses (M* ≳ 1010 M⊙ h-1) galaxies have a systematically lower metallicity, although with a smaller difference (-0.05 dex). Similar trends are obtained if g-band magnitudes are used instead of stellar masses. In minor interactions, we find that the less massive member is systematically enriched, while a galaxy in interaction with a comparable stellar mass companion shows a metallicity decrement with respect to galaxies in isolation. We argue that metal-rich starbursts triggered by a more massive component, and inflows of low-metallicity gas induced by comparable or less massive companion galaxies, provide a natural scenario to explain our findings. © 2008 The Authors. Journal compilation © 2008 RAS. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_17453933_v386_n1_pL82_MichelDansac
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Galaxies: abundances
Galaxies: evolution
Galaxies: formation
Galaxies: interactions
spellingShingle Galaxies: abundances
Galaxies: evolution
Galaxies: formation
Galaxies: interactions
Michel-Dansac, L.
Lambas, D.G.
Alonso, M.S.
Tissera, P.
The mass-metallicity relation of interacting galaxies
topic_facet Galaxies: abundances
Galaxies: evolution
Galaxies: formation
Galaxies: interactions
description We study the mass-metallicity relation of galaxies in pairs and in isolation taken from the Sloan Digital Sky Survey-Data Release 4 (SDSS-DR4) using the stellar masses and oxygen abundances derived by Tremonti et al. Close galaxy pairs, defined by projected separation rp < 25 kpc h-1 and radial velocity ΔV < 350 km s-1, are morphologically classified according to the strength of the interaction signs. We find that only for pairs showing signs of strong interactions, the mass-metallicity relation differs significantly from that of galaxies in isolation. In such pairs, the mean gas-phase oxygen abundances of galaxies with low stellar masses (M* ≲ 109 M⊙ h-1) exhibit an excess of 0.2 dex. Conversely, at larger masses (M* ≳ 1010 M⊙ h-1) galaxies have a systematically lower metallicity, although with a smaller difference (-0.05 dex). Similar trends are obtained if g-band magnitudes are used instead of stellar masses. In minor interactions, we find that the less massive member is systematically enriched, while a galaxy in interaction with a comparable stellar mass companion shows a metallicity decrement with respect to galaxies in isolation. We argue that metal-rich starbursts triggered by a more massive component, and inflows of low-metallicity gas induced by comparable or less massive companion galaxies, provide a natural scenario to explain our findings. © 2008 The Authors. Journal compilation © 2008 RAS.
format JOUR
author Michel-Dansac, L.
Lambas, D.G.
Alonso, M.S.
Tissera, P.
author_facet Michel-Dansac, L.
Lambas, D.G.
Alonso, M.S.
Tissera, P.
author_sort Michel-Dansac, L.
title The mass-metallicity relation of interacting galaxies
title_short The mass-metallicity relation of interacting galaxies
title_full The mass-metallicity relation of interacting galaxies
title_fullStr The mass-metallicity relation of interacting galaxies
title_full_unstemmed The mass-metallicity relation of interacting galaxies
title_sort mass-metallicity relation of interacting galaxies
url http://hdl.handle.net/20.500.12110/paper_17453933_v386_n1_pL82_MichelDansac
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