On the dynamics of the Small Magellanic Cloud through high-resolution ASKAP H I observations

Di Teodoro, E. M. et al., 2019, Monthly Notices of the Royal Astronomical Society, 483, 392 | View on ADS (2019MNRAS.483..392D) | Access via DOI


We use new high-resolution H I data from the Australian Square Kilometre Array Pathfinder to investigate the dynamics of the Small Magellanic Cloud (SMC). We model the H I gas component as a rotating disc of non-negligible angular size, moving into the plane of the sky, and undergoing nutation/precession motions. We derive a high-resolution (̃10 pc) rotation curve of the SMC out to R̃ 4 kpc. After correcting for asymmetric drift, the circular velocity slowly rises to a maximum value of V_c̃eq 55 {km s}^{-1} at R̃eq 2.8 kpc and possibly flattens outwards. In spite of the SMC undergoing strong gravitational interactions with its neighbours, its H I rotation curve is akin to that of many isolated gas-rich dwarf galaxies. We decompose the rotation curve and explore different dynamical models to deal with the unknown 3D shape of the mass components (gas, stars, and dark matter). We find that, for reasonable mass-to-light ratios, a dominant dark matter halo with mass M_DM(R<4 kpc) ̃eq 1-1.5 × 10^9 M_☉ is always required to successfully reproduce the observed rotation curve, implying a large baryon fraction of 30 per cent-40 per cent. We discuss the impact of our assumptions and the limitations of deriving the SMC kinematics and dynamics from H I observations.


This publication has been tagged as:

Magellanic Clouds/HI

18 total citations As at 1 Apr, 2021

Citations by month:
As at 31 Mar, 2021

Team log-in

Log-in to access the team wiki.

Contact the GASKAP team at gaskap[at]

Site design by Marc White, Research School of Astronomy & Astrophysics, Australian National University.
Site & content copyright © 2019, the GASKAP team.
Powered by Django.
Designed with Bootstrap.