The sense of rotation of subhaloes in cosmological dark matter haloes

Details The sense of rotation of subhaloes in cosmological dark matter haloes The sense of rotation of subhaloes in cosmological dark matter haloes

2005-12-06

arxiv.org/abs/astro-ph/0512156v2

Mon.Not.Roy.Astron.Soc.369:1253-1266,2006

Astronomy and Astrophysics

Astrophysics

16 pages, 9 figures, accepted by MNRAS; extended comparison with previous work (mistake corrected) and observations, typos cor

Scientific paper

10.1111/j.1365-2966.2006.10371.x

We present a detailed analysis of the velocity distribution and orientation of orbits of subhaloes in high resolution cosmological simulations of dark matter haloes. We find a trend for substructure to preferentially revolve in the same direction as the sense of rotation of the host halo: there is an excess of prograde satellite haloes. Throughout our suite of nine host haloes (eight cluster sized objects and one galactic halo) there are on average 59% of the satellites corotating with the host. Even when including satellites out to five virial radii of the host, the signal still remains pointing out the relation of the signal with the infall pattern of subhaloes. However, the fraction of prograde satellites weakens to about 53% when observing the data along a (random) line-of-sight and deriving the distributions in a way an observer would infer them. This decrease in the observed prograde fraction has its origin in the technique used by the observer to determine the sense of rotation, which results in a possible misclassification of non-circular orbits. We conclude that the existence of satellites on corotating orbits is another prediction of the cold dark matter structure formation scenario, although there will be difficulties to verify it observationally. Since the galactic halo simulation gave the same result as the cluster-sized simulations, we assume that the fraction of prograde orbits is independent of the scale of the system, though more galactic simulations would be necessary to confirm this.

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