Journal
ADVANCES IN SPACE RESEARCH
Volume 53, Issue 6, Pages 950-962Publisher
ELSEVIER SCI LTD
DOI: 10.1016/j.asr.2013.06.001
Keywords
Galaxies: evolution; Galaxies: interactions; Galaxies: individual: NGC 3626, NGC 1533; Method: numerical
Categories
Funding
- ASI-INAF [1/009/10/0]
- INAF/PRIN
Ask authors/readers for more resources
We are investigating the co-evolution of galaxies within groups combining multi-wavelength photometric and 2D kinematical observations. Here we focus on S0s showing star formation in ring/arm-like structures. We use smooth particle hydrodynamical simulations (SPH) with chemo-photometric implementation which provide dynamical and morphological information together with the spectral energy distribution (SED) at each evolutionary stage. As test cases, we simulate the evolution of two such S0s: NGC 1533 and NGC 3626. The merging of two halos with mass ratio 2:1, initially just composed of DM and gas, well match their observed SEDs, their surface brightness profiles and their overall kinematics. The residual star formation today rejuvenating the ring/arm like structures in these S0s is then a mere consequence of a major merger, i.e. this is a phase during the merger episode. The peculiar kinematical features, e.g. gasstars counter rotation in NGC 3626, depends on the halos initial impact parameters. Furthermore, our simulations allow to follow, in a fully consistent way, the transition of these S0s through the green valley in the NUV-r vs. M-r colour magnitude diagram, which they cross in about 3-5 Gyrs, before reaching their current position in the red sequence. We conclude that a viable mechanism driving the evolution of S0s in groups is of gravitational origin. (C) 2013 COSPAR. Published by Elsevier Ltd. All rights reserved.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available