The mass-metallicity relation of interacting galaxies

Leo Michel-Dansac, Diego G. Lambas, M. Sol Alonso, Patricia Tissera

Resultado de la investigación: Letter

67 Citas (Scopus)

Resumen

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.

Idioma originalEnglish
PublicaciónMonthly Notices of the Royal Astronomical Society: Letters
Volumen386
N.º1
DOI
EstadoPublished - 1 may 2008

Huella dactilar

interacting galaxies
metallicity
galaxies
stellar mass
isolation
oxygen
gas
interactions
radial velocity
inflow
vapor phases
trends
metal

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Michel-Dansac, Leo ; Lambas, Diego G. ; Alonso, M. Sol ; Tissera, Patricia. / The mass-metallicity relation of interacting galaxies. En: Monthly Notices of the Royal Astronomical Society: Letters. 2008 ; Vol. 386, N.º 1.
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abstract = "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.",
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The mass-metallicity relation of interacting galaxies. / Michel-Dansac, Leo; Lambas, Diego G.; Alonso, M. Sol; Tissera, Patricia.

En: Monthly Notices of the Royal Astronomical Society: Letters, Vol. 386, N.º 1, 01.05.2008.

Resultado de la investigación: Letter

TY - JOUR

T1 - The mass-metallicity relation of interacting galaxies

AU - Michel-Dansac, Leo

AU - Lambas, Diego G.

AU - Alonso, M. Sol

AU - Tissera, Patricia

PY - 2008/5/1

Y1 - 2008/5/1

N2 - 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.

AB - 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.

KW - Galaxies: abundances

KW - Galaxies: evolution

KW - Galaxies: formation

KW - Galaxies: interactions

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