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• W2010356064 abstract "A consensus is emerging that interacting galaxies show depressed nuclear gas metallicities compared to isolated star-forming galaxies. Simulations suggest that this nuclear underabundance is caused by interaction-induced inflow of metal-poor gas and that this inflow concurrently flattens the radial metallicity gradients in strongly interacting galaxies. We present metallicities of over 300 H ii regions in a sample of 16 spirals that are members of strongly interacting galaxy pairs with mass ratio near unity. The deprojected radial gradients in these galaxies are about half of those in a control sample of isolated, late-type spirals. Detailed comparison of the gradients with simulations shows remarkable agreement in gradient distributions, the relationship between gradients and nuclear underabundances, and the shape of profile deviations from a straight line. Taken together, this evidence conclusively demonstrates that strongly interacting galaxies at the present day undergo nuclear metal dilution due to gas inflow, as well as significant flattening of their gas-phase metallicity gradients, and that current simulations can robustly reproduce this behavior at a statistical level." @default.
• W2010356064 created "2016-06-24" @default.
• W2010356064 creator A5016073168 @default.
• W2010356064 creator A5027796962 @default.
• W2010356064 creator A5033229802 @default.
• W2010356064 date "2010-10-20" @default.
• W2010356064 modified "2023-10-15" @default.
• W2010356064 title "GAS-PHASE OXYGEN GRADIENTS IN STRONGLY INTERACTING GALAXIES. I. EARLY-STAGE INTERACTIONS" @default.
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• W2010356064 doi "https://doi.org/10.1088/0004-637x/723/2/1255" @default.
• W2010356064 hasPublicationYear "2010" @default.
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