A very deep Chandra observation of the Perseus cluster: shocks, ripples and conduction

Details A very deep Chandra observation of the Perseus cluster: shocks, ripples and conduction A very deep Chandra observation of the Perseus cluster: shocks, ripples and conduction

2005-10-17

arxiv.org/abs/astro-ph/0510476v2

Mon.Not.Roy.Astron.Soc.366:417-428,2006

Astronomy and Astrophysics

Astrophysics

13 pages, 14 figures, colour, accepted by MNRAS, includes minor changes suggested by referee, high quality version at http:/

Scientific paper

10.1111/j.1365-2966.2005.09896.x

We present the first results from a very deep Chandra X-ray observation of the core of the Perseus cluster of galaxies. A pressure map reveals a clear thick band of high pressure around the inner radio bubbles. The gas in the band must be expanding outward and the sharp front to it is identified as a shock front, yet we see no temperature jump across it; indeed there is more soft emission behind the shock than in front of it. We conclude that in this inner region either thermal conduction operates efficiently or the co-existing relativistic plasma seen as the radio mini-halo is mediating the shock. If common, isothermal shocks in cluster cores mean that we cannot diagnose the expansion speed of radio bubbles from temperature measurements alone. They can at times expand more rapidly than currently assumed without producing significant regions of hot gas. Bubbles may also be significantly more energetic. The pressure ripples found in earlier images are identified as isothermal sound waves. A simple estimate based on their amplitude confirms that they can be an effective distributed heat source able to balance radiative cooling. We see multiphase gas with about 10^9 Msun at a temperature of about 0.5 keV. Much, but not all, of this cooler gas is spatially associated with the optical filamentary nebula around the central galaxy, NGC 1275. A residual cooling flow of about 50 Msun/yr may be taking place. A channel is found in the pressure map along the path of the bubbles, with indications found of outer bubbles. The channel connects in the S with a curious cold front.

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