The effects of the interaction on the kinematics, stellar population and metallicity of AM2322-821 with Gemini/GMOS

• Published in: arXiv.org
• Main Authors: Krabbe, A C, Pastoriza, M G, Winge, C, Rodrigues, I, Dors, O L, Ferreiro, D L
• Format: Paper Journal Article
• Language: English
• Published: Ithaca Cornell University Library, arXiv.org 23.05.2011
• Subjects: Abundance; Computer simulation; Diagnostic systems; Galactic rotation; Galaxy distribution; Kinematics; Mathematical models; Metallicity; Oxygen; Photoionization; Physics - Cosmology and Nongalactic Astrophysics; Radial velocity; Spiral galaxies; Stars & galaxies; Stellar populations; Velocity distribution
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.1105.4581

We present an observational study about the impacts of the interactions in the kinematics, stellar populations, and oxygen abundances of the components of the galaxy pair AM\,2322-821. A fairly symmetric rotation curve for the companion (AM\,2322B) galaxy with a deprojected velocity amplitude of 110 km s\(^{-1}\) was obtained, and a dynamical mass of \( 1.1 - 1.3 \times 10^{10} M_{\sun}\) within a radius of 4 kpc was estimated using this deprojected velocity. Asymmetries in the radial velocity field were detected for the companion, very likely due the interaction between the galaxies. The interaction between the main and companion galaxies was modelled using numerical N-body/hydrodynamical simulations, with the result indicating that the current stage of the system would be about 90 Myr after perigalacticum. The spatial variation in the distribution of the stellar-population components in both galaxies was analysed using the stellar population synthesis code {\sc STARLIGHT}. The companion galaxy is dominated by a very young (t \( \leq 1\times10^{8}\) yr) population, with the fraction of this population to the total flux at \(\lambda\, 5\,870\, \AA\), increasing outwards in the galaxy disc. On the other hand, the stellar population of AM\,2322A is heterogeneous along the slit positions observed. Spatial profiles of oxygen abundance in the gaseous phase were obtained using the diagnostic diagram R23 vs. [OIII]/[OII], where we compared the observed values with the ones obtained from photoionization models. Such gradients of oxygen abundance are significantly flatter for this pair of galaxies than in typical isolated spiral galaxies. This metallicity distribution is interpreted as the gradients having been destroyed by interaction-induced gas flows from the outer parts to the centre of the galaxy