Hartmann, Markus, Debattista, Victor P., Seth, Anil, Cappellari, Michele and Quinn, Thomas R. (2011) Constraining the role of star cluster mergers in nuclear cluster formation: simulations confront integral-field data. Monthly Notices of the Royal Astronomical Society, 418 (4). pp. 2697-2714. ISSN 00358711
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Official URL: http://dx.doi.org/10.1111/j.1365-2966.2011.19659.x
We present observations and dynamical models of the stellar nuclear clusters (NCs) at the centres of NGC 4244 and M33. We then compare these to an extensive set of simulations testing the importance of purely stellar dynamical mergers on the formation and growth of NCs. Mergers of star clusters are able to produce a wide variety of observed properties, including densities, structural scaling relations, shapes (including the presence of young discs) and even rapid rotation. None the less, difficulties remain, most notably that the second-order kinematic moment inline image of the models is too centrally peaked to match observations. This can be partially remedied by the merger of star clusters on to a pre-existing nuclear disc, but the line-of-sight velocity V is still more slowly rising than in NGC 4244. Our results therefore suggest that purely stellar dynamical mergers cannot form NCs and that gas dissipation is a necessary ingredient for at least ∼50 per cent of a NC’s mass. The negative vertical anisotropy found in NGC 4244, however, requires at least 10 per cent of the mass to have been accreted as stars, since gas dissipation and in situ star formation leads to positive vertical anisotropy.
|Uncontrolled Keywords (separate with ;):||galaxies: evolution; galaxies: kinematics and dynamics; galaxies: structure|
|Subjects:||Physical sciences > Physics|
|Schools:||College of Science and Technology > School of Physical Sciences and Computing > Jeremiah Horrocks Institute|
|Deposited By:||Helen Cooper|
|Deposited On:||20 Mar 2012 17:28|
|Last Modified:||09 Aug 2016 15:15|
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