Unequal-mass galaxy merger remnants: spiral-like morphology but elliptical-like kinematics

Details Unequal-mass galaxy merger remnants: spiral-like morphology but elliptical-like kinematics Unequal-mass galaxy merger remnants: spiral-like morphology but elliptical-like kinematics

2004-03-12

arxiv.org/abs/astro-ph/0403307v1

Astron.Astrophys. 418 (2004) L27

Astronomy and Astrophysics

Astrophysics

4 pages, 3 figures, Accepted for publication in A&A Letters

Scientific paper

10.1051/0004-6361:20040114

It is generally believed that major galaxy mergers with mass ratios in the range 1:1-3:1 result in remnants that have properties similar to elliptical galaxies, and minor mergers below 10:1 result in disturbed spiral galaxies. The intermediate range of mass ratios 4:1-10:1 has not been studied so far. Using N-body simulations, we show that such mergers can result in very peculiar systems, that have the morphology of a disk galaxy with an exponential profile, but whose kinematics is closer to that of elliptical systems. These objects are similar to those recently observed by Jog & Chitre (2002). We present two cases with mass ratios 4.5:1 and 7:1, and show that the merging causes major heating and results in the appearance of elliptical-type kinematics, while surprisingly the initial spiral-like mass profile is conserved.

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