銀河団内ガス分布に対する新しいベータモデル

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  • New β Model of Intracluster Gas Distribution
  • New v model of intracluster gas distribution

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A new type of β model of intracluster gas distribution is established, which is well fitted to the observed X-ray surface brightness profile except for outermost region. It employs the exact King model of the self-gravitating system of collisionless particles instead of the widely used approximated analytical formula for the dark matter distribution. The small difference between the modelled and the observed X-ray surface brightness profiles would disappear if the infall of matter from the intercluster space is taken into account. The number of parameters of our model is the same as for the isothermal β model, but the agreement between our model and data points is satisfactory even when the fitting with the isothermal β model remaines a large central excess. In addition, the enhanced central mass concentration in our model is high enough to resolve the discrepancy between the X-ray and the lensing measurements of cluster mass. These facts suggest that most of the central excess might be no more than a ghost embossed by an inadequate fitting. Therefore the central excess would not necessarily be linked to the existence of cooling flow. It is also shown that the obtained values of β(our model)∼0.5support the theory of non-gravitational intracluster gas heatings comparable to those reached through gravitational collapse. On the other hand, the value of β∼0.6obtained for the isothermal β model is explained as showing the scarcity of matter in the space surrounding each cluster, brobably due to the infall of matter towards it over a long time.

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