XMM—Newton observations of the Perseus cluster — II. Evidence for gas motions in the core

By E. Churazov, W. Forman, C. Jones, R. Sunyaev, H. Böhringer. 2003

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The 5–9 keV spectrum of the inner ∼100 kpc of the Perseus cluster measured by XMM–Newton can be well described by an optically thin plasma emission model as predicted by the apec code, without any need for invoking a strong Ni overabundance or the effects of resonant scattering. For the strongest 6.7-keV line of He-like iron, the optical depth of the cluster, calculated using observed density, temperature and abundance profiles, is of the order of 3. The lack of evidence for resonant scattering effects implies gas motion in the core with a range in velocities of at least half of the sound velocity. If this motion has the character of small-scale turbulence, then its dissipation would provide enough energy to compensate for radiative cooling of the gas. The activity of the supermassive black hole at the centre of the cluster may be the driving force of the gas motion.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/dd17886207843318a1c255ea320f2d904a538547

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Citations in the corpus

Energy, momentum and mass outflows and feedback from thick accretion discs around rotating black holes (2013, background): “…BH angular velocity H and the BH magnetic flux BH. SMBH ‘feedback’ in galaxy clusters is believed to play an important role in keeping the cluster gas hot and preventing catastrophic star formation (Ciotti & Ostriker 2001; Brüggen & Kaiser 2002; Ruszkowski & Begelman 2002; Churazov et al. 2004).”
Compressible turbulence in galaxy clusters: physics and stochastic particle re-acceleration (2007, background): “…challenges, indications of some level (at least 10–20% of the thermal energy) of turbulence in the ICM comes from gas–pressure maps in the X–rays (Schuecker et al. 2004), and also from the lack of resonant scattering from X–ray spectra (Churazov et al. 2004; Gastaldello & Molendi 2004).”
X-ray spectroscopy of galaxy clusters: studying astrophysical processes in the largest celestial laboratories (2009, methodology): “Note that the spatial scales of turbulence probed in the cores of elliptical galaxies by RGS are much smaller than those probed in Perseus (Churazov et al. 2004) or Coma (Schuecker et al. 2004).”
Turbulent Motions and Shocks Waves in Galaxy Clusters simulated with AMR (2009, methodology): “Additional evidences of turbulent motions inside nearby galaxy clusters came from the observation of pseudo-pressure fluctuations in Abell 754 using XMM (Henry et al.2004) and from the non detection of resonant scattering in the Perseus cluster (Churazov et al.2004).”
Evolving turbulence and magnetic fields in galaxy clusters (2005, background): “The presence of long Hα filaments observed by Fabian et al. (2003, 2005) in the core of the Perseus cluster may not be inconsistent with various evidence for random motions in this cluster core (Churazov et al. 2004; Rebusco et al. 2005).”
Massive and refined - II. The statistical properties of turbulent motions in massive galaxy clusters with high spatial resolution (2010, background): “…of a number of nearby clusters, based on pseudo– pressure maps of cluster cores and on the lack of evidence for resonant scattering e ﬀ ects in the X-ray spectra, provided hints of turbulence in the ICM (e.g. Schuecker et al. 2004; Henry et al. 2004; Churazov et al. 2004; Ota et al. 2007).”
Heating Hot Atmospheres with Active Galactic Nuclei (2007, unknown): “Outflows from central AGN may create a similar level of turbulence, as suggested by observations of the Perseus cluster (Churazov et al. 2004), so that the source of turbulence in cool cores is unclear.”