Clumpy streams in a smooth dark halo: the case of Palomar 5

By means of direct N-body simulations and simplified numerical models, we study the formation and characteristics of the tidal tails around Palomar 5, along its orbit in the Milky Way potential. Unlike previous findings, we are able to reproduce the substructures observed in the stellar streams of t...

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Bibliographic Details
Published in:arXiv.org 2012-09
Main Authors: Mastrobuono-Battisti, Alessandra, Paola Di Matteo, Montuori, Marco, Haywood, Misha
Format: Article
Language:English
Subjects:
Clumps
Computer simulation
Dark matter
Globular clusters
Mathematical models
Star clusters
Stellar orbits
Substructures
Online Access:Get full text
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Summary:By means of direct N-body simulations and simplified numerical models, we study the formation and characteristics of the tidal tails around Palomar 5, along its orbit in the Milky Way potential. Unlike previous findings, we are able to reproduce the substructures observed in the stellar streams of this cluster, without including any lumpiness in the dark matter halo. We show that overdensities similar to those observed in Palomar 5 can be reproduced by the epicyclic motion of stars along its tails, i.e. a simple local accumulation of orbits of stars that escaped from the cluster with very similar positions and velocities. This process is able to form stellar clumps at distances of several kiloparsecs from the cluster, so it is not a phenomenon confined to the inner part of Palomar 5's tails, as previously suggested. Our models can reproduce the density contrast between the clumps and the surrounding tails found in the observed streams, without including any lumpiness in the dark halo, suggesting new upper limits on its granularity.
ISSN:2331-8422
DOI:10.48550/arxiv.1209.0466