Property of Young Massive Clusters in a Galaxy-Galaxy Merger Remnant. (arXiv:1811.04547v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Matsui_H/0/1/0/all/0/1">Hidenori Matsui</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tanikawa_A/0/1/0/all/0/1">Ataru Tanikawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Saitoh_T/0/1/0/all/0/1">Takayuki R Saitoh</a>
We investigate the properties of young massive clusters (YMCs) in a
galaxy-galaxy merger remnant by analyzing the data obtained by a gas rich major
merger simulations in Matsui et al. 2012. We found that the YMCs are
distributed at a few $rm kpc$ and at $sim 10~{rm kpc}$ from the galactic
center, in other words, there are two components of their distribution. The
former are formed in filamentary and turbulent gas generated at a few $rm kpc$
from the center because of galaxy encounters, and the latter are formed in
tidal tails which are far from the center. The YMCs are much less concentrated
than galaxy stars. The mass function of the YMCs is $dN/dM propto M^{-2}$.
Most of YMCs are formed from the second encounter to the final coalescence
phase of the galactic cores, and their formation rate is especially high at
final coalescence phase. Most of them consists of single stellar population in
age, but YMCs with multi stellar populations in age are also formed. The
multiple populations are produced by the following process: a YMC captures
dense gas, and another generation stars form within the cluster. There are
several YMCs formed in an isolated disk before the encounter of galaxies. These
candidates contain stars with various age by capturing dense gas and forming
stars. YMCs in a merger remnant, have various orbits, but large fraction of
candidates have circular orbits.
We investigate the properties of young massive clusters (YMCs) in a
galaxy-galaxy merger remnant by analyzing the data obtained by a gas rich major
merger simulations in Matsui et al. 2012. We found that the YMCs are
distributed at a few $rm kpc$ and at $sim 10~{rm kpc}$ from the galactic
center, in other words, there are two components of their distribution. The
former are formed in filamentary and turbulent gas generated at a few $rm kpc$
from the center because of galaxy encounters, and the latter are formed in
tidal tails which are far from the center. The YMCs are much less concentrated
than galaxy stars. The mass function of the YMCs is $dN/dM propto M^{-2}$.
Most of YMCs are formed from the second encounter to the final coalescence
phase of the galactic cores, and their formation rate is especially high at
final coalescence phase. Most of them consists of single stellar population in
age, but YMCs with multi stellar populations in age are also formed. The
multiple populations are produced by the following process: a YMC captures
dense gas, and another generation stars form within the cluster. There are
several YMCs formed in an isolated disk before the encounter of galaxies. These
candidates contain stars with various age by capturing dense gas and forming
stars. YMCs in a merger remnant, have various orbits, but large fraction of
candidates have circular orbits.
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