Formation of the Small Magellanic Cloud: ancient major merger as a solution to the kinematical differences between old stars and HI gas
Kenji Bekki, Masashi Chiba

TL;DR
This paper proposes that an ancient major merger between gas-rich dwarf irregulars explains the Small Magellanic Cloud's current kinematic differences between old stars and HI gas, supported by simulations showing distinct stellar and gas dynamics.
Contribution
It introduces a novel merger scenario that accounts for the SMC's kinematic properties, supported by simulations of dwarf-dwarf mergers resulting in a spheroidal stellar component and rotating HI disk.
Findings
Simulations produce a spheroidal stellar component with little rotation.
Simulations generate a rotating extended HI gas disk.
The model explains the observed kinematic differences in the SMC.
Abstract
Recent observations of the Small Magellanic Cloud (SMC) have revealed that the HI gas shows a significant amount of rotation (V_c 60 km/s), while no or little rotation is evident for the old stellar populations. We suggest that this unique kinematical difference between these components in the SMC can be caused by a major merger event which occurred in the early stage of the SMC formation. Our simulations show that dissipative dwarf-dwarf merging can transform two gas-rich dwarf irregulars into a new dwarf, which consists of a spheroidal stellar component and a rotating extended HI disk. The remnant of this dwarf-dwarf merging shows significantly different kinematics between stars and gas, in the sense that a gas disk rotates rapidly while a stellar component shows little rotation. We thus suggest that the simulated dwarf having a dynamically hot spheroid and an extended gas disk…
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