Speaker
Description
Aims. Cold gas ( $T \sim 10^4$ K) filamentary structures with H$\alpha$ emissions were found around central regions of some
cool-core galaxy clusters. We wish to compare the results
between the observation of the Perseus cluster and our simulation
in order to interpret velocity structures of observed filaments.
Methods. We perform hydrodynamic simulations to trace gas
motions in the Perseus cluster.
Results. In our simulation, filaments with a chaotic velocity
structure dominate the population, while those with a uniform
velocity structure are secondary. The simulation also produces
an overall low velocity dispersion.
Conclusions. The cold gas motions present chaotic more
often, whereas observations suggest an uniform structure. On
the other hand, the velocity dispersion in the simulation is
consistent with the observation results.
| Section | Galaxy/Extragalactic |
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