The velocity structure of Cygnus OB2. (arXiv:2005.10260v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Arnold_B/0/1/0/all/0/1">Becky Arnold</a> (1 and 2), <a href="http://arxiv.org/find/astro-ph/1/au:+Goodwin_S/0/1/0/all/0/1">Simon P. Goodwin</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Wright_N/0/1/0/all/0/1">Nick J. Wright</a> (3) ((1) University of Sheffield, (2) University of Massachusetts, (3) Keele University)
The kinematic structure of the Cygnus OB2 association is investigated. No
evidence of expansion or contraction is found at any scale within the region.
Stars that are within $sim$ 0.5 parsecs of one another are found to have more
similar velocities than would be expected by random chance, and so it is
concluded that velocity substructure exists on these scales. At larger scales
velocity substructure is not found. We suggest that bound substructures exist
on scales of $sim$ 0.5 parsecs, despite the region as a whole being unbound.
We further suggest that any velocity substructure that existed on scales > 0.5
parsecs has been erased. The results of this study are then compared to those
of other kinematic studies of Cygnus OB2.
The kinematic structure of the Cygnus OB2 association is investigated. No
evidence of expansion or contraction is found at any scale within the region.
Stars that are within $sim$ 0.5 parsecs of one another are found to have more
similar velocities than would be expected by random chance, and so it is
concluded that velocity substructure exists on these scales. At larger scales
velocity substructure is not found. We suggest that bound substructures exist
on scales of $sim$ 0.5 parsecs, despite the region as a whole being unbound.
We further suggest that any velocity substructure that existed on scales > 0.5
parsecs has been erased. The results of this study are then compared to those
of other kinematic studies of Cygnus OB2.
http://arxiv.org/icons/sfx.gif
