Open AccessThe relationship between the optical Hα filaments and the X‐ray emission in the core of the Perseus cluster
Author(s) -
Fabian A. C.,
Sanders J. S.,
Crawford C. S.,
Conselice C. J.,
Gallagher J. S.,
Wyse R. F. G.
Publication year - 2003
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2003.06856.x
Subject(s) - physics , astrophysics , intracluster medium , nebula , laminar flow , galaxy cluster , bubble , cluster (spacecraft) , galaxy , core (optical fiber) , cooling flow , astronomy , stars , optics , mechanics , computer science , thermodynamics , programming language
NGC 1275 in the centre of the Perseus cluster of galaxies, Abell 426, is surrounded by a spectacular filamentary Hα nebula. Deep Chandra X‐ray imaging has revealed that the brighter outer filaments are also detected in soft X‐rays. This can be due to conduction and mixing of the cold gas in the filaments with the hot, dense intracluster medium. We show the correspondence of the filaments in both wavebands and draw attention to the relationship of two prominent curved north‐west filaments to an outer, buoyant radio bubble seen as a hole in the X‐ray image. There is a strong resemblance in the shape of the hole and the disposition of the filaments to the behaviour of a large air bubble rising in water. If this is a correct analogy, then the flow is laminar and the intracluster gas around this radio source is not turbulent. We obtain a limit on the viscosity of this gas.