Genesis of morpho-kinematic lopsidedness in minor merger of galaxies

Abstract

An $m=1$ lopsided asymmetry is common in disc galaxies. Here, we investigate the excitation of an $m=1$ lopsidedness in host galaxies during minor mergers while choosing a set of 1:10 merger models (with varying orbital configurations, morphology of the host galaxy) from the GalMer galaxy merger library. We show that a minor merger triggers a prominent $m=1$ lopsidedness in stars of the host galaxy. The strength of the $m=1$ lopsidedness undergoes a transient amplification phase after each pericenter passage of the satellite, in concordance with past findings of exciting an $m=1$ lopsidedness by tidal encounters. However, once the merger happens, and the post-merger remnant readjusts itself, the lopsidedness disappears in short time-scale ($\sim$ 500-850 Myr). Furthermore, a delayed merger can drive a prolonged ($\sim$2 Gyr) lopsidedness in the host galaxy. We demonstrate that the $m=1$ lopsidedness rotates with a well-defined pattern speed which is much slower than the $m=2$ bar pattern speed, and is retrograde with respect to the bar. This gives rise to a dynamical scenario where the Inner Lindblad resonance of the $m=1$ lopsidedness falls in between the corotation and the Outer Lindblad resonance of the $m=2$ bar mode. A kinematic lopsidedness also arises in the host galaxy; the resulting temporal variation closely follows that of the density lopsidedness. The minor merger also triggers a transient off-centred stellar disc-dark matter halo configuration due to the tidal encounter with the satellite.

19 pages, 1 table, 16 figures (including appendices), accepted for publication in MNRAS

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• SAMI-HI: the connection between global asymmetry in the ionised and neutral atomic hydrogen gas in galaxies
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