Monte Carlo Modeling of Non-Gravitational Heating Processes in Galaxy Clusters | Zendy

Mamoru Shimizu | Zendy; Tetsu Kitayama | Zendy; Shin Sasaki | Zendy; Yasushi Suto | Zendy

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Monte Carlo Modeling of Non-Gravitational Heating Processes in Galaxy Clusters

Author(s) -

Mamoru Shimizu,

Tetsu Kitayama,

Shin Sasaki,

Yasushi Suto

Publication year - 2004

Publication title -

publications of the astronomical society of japan

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 1.99

H-Index - 110

eISSN - 2053-051X

pISSN - 0004-6264

DOI - 10.1093/pasj/56.1.1

Subject(s) - physics , astrophysics , protogalaxy , supernova , galaxy , hydrostatic equilibrium , redshift , gravitation , galaxy formation and evolution , galaxy cluster , dark matter , cooling flow , gravitational energy , astronomy , halo , galaxy merger

We consider non-gravitational heating effects on galaxy clusters on the basisof the Monte-Carlo modeling of merging trees of dark matter halos combined withthe thermal evolution of gas inside each halo. Under the assumption ofhydrostatic equilibrium and the isothermal gas profiles, our model takesaccount of the metallicity evolution, metallicity-dependent cooling of gas,supernova energy feedback, and heating due to jets of radio galaxies in aconsistent manner. The observed properties of galaxy clusters can be explainedin models with higher non-gravitational heating efficiency than that in theconventional model. Possibilities include jet heating by the Fanaroff-RileyType II radio galaxies, and the enhanced star formation efficiency and/orsupernova energy feedback, especially at high redshifts.Comment: 29 pages, 12 figures. To appear in PASJ, February 25, 200

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