On the mass segregation of stars and brown dwarfs in Taurus
Article first published online: 18 JAN 2011
© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS
Monthly Notices of the Royal Astronomical Society
Volume 412, Issue 4, pages 2489–2497, April 2011
How to Cite
Parker, R. J., Bouvier, J., Goodwin, S. P., Moraux, E., Allison, R. J., Guieu, S. and Güdel, M. (2011), On the mass segregation of stars and brown dwarfs in Taurus. Monthly Notices of the Royal Astronomical Society, 412: 2489–2497. doi: 10.1111/j.1365-2966.2010.18070.x
- Issue published online: 8 APR 2011
- Article first published online: 18 JAN 2011
- Accepted 2010 November 23. Received 2010 November 12; in original form 2010 September 1
- methods: data analysis;
- brown dwarfs;
- stars: low-mass;
- galaxies: star clusters: individual: Taurus
We use the new minimum spanning tree (MST) method to look for mass segregation in the Taurus association. The method computes the ratio of MST lengths of any chosen subset of objects, including the most massive stars and brown dwarfs, to the MST lengths of random sets of stars and brown dwarfs in the cluster. This mass segregation ratio (ΛMSR) enables a quantitative measure of the spatial distribution of high- and low-mass stars, and brown dwarfs to be made in Taurus.
We find that the most massive stars in Taurus are inversely mass segregated with ΛMSR= 0.70 ± 0.10 (ΛMSR= 1 corresponds to no mass segregation), which differs from the strong mass segregation signatures found in more dense and massive clusters such as Orion. The brown dwarfs in Taurus are not mass segregated, although we find evidence that some low-mass stars are, with an ΛMSR= 1.25 ± 0.15. Finally, we compare our results to previous measures of the spatial distribution of stars and brown dwarfs in Taurus, and briefly discuss their implications.