Probing turbulence in the Coma galaxy cluster

By P. Schuecker, A. Finoguenov, Francesco Miniati, H. Böhringer, U. Briel. 2004

236 citations recorded by the source corpus.

Spatially-resolved gas pressure maps of the Coma galaxy cluster are obtained from a mosaic of XMM-Newton observations in the scale range between a resolution of 20 kpc and an extent of 2.8 Mpc. A Fourier analysis of the data reveals the presence of a scale-invariant pressure fluctuation spectrum in the range between 40 and 90 kpc and is found to be well described by a projected Kolmogorov/Oboukhov-type turbulence spectrum. Deprojection and integration of the spectrum yields the lower limit of ∼10 percent of the total intracluster medium pressure in turbulent form. The results also provide observational constraints on the viscosity of the gas.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/35aa4d426068d05ff3531cff138c816ea5046198

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Citations in the corpus

RESIDUAL GAS MOTIONS IN THE INTRACLUSTER MEDIUM AND BIAS IN HYDROSTATIC MEASUREMENTS OF MASS PROFILES OF CLUSTERS (2009, methodology): “In particular, Schuecker et al. (2004) use the Fourier analysis of fluctuations in the projected gas presure map of the Coma Cluster measured withXMM-Newton and find a Kolmogorov-like spectrum.”
X-ray surface brightness and gas density fluctuations in the Coma cluster (2011, methodology): “For now, turbulence remains a plausible contributor to the observed surface brightness fluctuations, as well as pressure fluctuations (Schuecker et al. 2004) in Coma.”
Magnetic Fields in the Large-Scale Structure of the Universe (2011, methodology): “For example, Schuecker et al. (2004) analyzed gas pressure maps that were constructed from XMM-Newton X-ray data.”
Astrophysical magnetic fields and nonlinear dynamo theory (2004, background): “From analysis of pressure fluctuations as revealed in X-ray observations it has been argued [555] that the integral turbulent scale in the Coma cluster 35 is close to 100 kpc, and they assume a turbulent speed of 250 km s−1 at that scale.”
Cluster Mergers and Non-Thermal Phenomena: A Statistical Magneto-Turbulent Model (2004, result): “In particular the turbulent energy is found to be ∼15 per cent of that of the thermal energy, in agreement with recent numerical simulations (Sunyaev, Norman & Bryan 2003) and with very recent observational claims (Schuecker et al. 2004).”
Formation of Galaxy Clusters (2012, background): “Currently, there are only indirect indications for turbulent motions in the ICM of the realclusters from fluctuations of gas density measured in X–ray observations (e.g., Churazovet al. 2012, Schuecker et al. 2004).”
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).”
X-ray spectroscopy of galaxy clusters: studying astrophysical processes in the largest celestial laboratories (2009, methodology): “An investigation of the presence of stochastic turbulence has been performed by means of a spectral reduction of deepXMM-Newton observations of the Coma galaxy cluster by Schuecker et al. (2004).”
Evolving turbulence and magnetic fields in galaxy clusters (2005, background): “From analysis of pressure fluctuations as revealed in X-ray observations, Schuecker et al. (2004) argue that the integral turbulent scale in the Coma cluster is close to 100 kpc, and they assume a turbulent speed of 250 km s−1 at that scale.”
Compressible turbulence in galaxy clusters: physics and stochastic particle re-acceleration (2007, background): “A related issue is the discovery of non–thermal emission in the hard X–ray band detected in a few galaxy clusters (e.g., Fusco–Femiano et al. 2004; Rephaeli, Gruber, Arieli 2006). c© 0000 RAS The most spectacular example of non–thermal emission from galaxy clusters is that of giant radio halos.”
X-Ray and Sunyaev-Zel’dovich Effect Measurements of the Gas Mass Fraction in Galaxy Clusters (2006, result): “Recent numerical simulations suggest that this provides about 10% of the total pressure support in clusters (Faltenbacher et al. 2005; Rasia et al. 2006; Lau et al. 2006) and similar results are obtained using XMM-Newton observations of the Coma cluster (Schuecker et al. 2004).”
Moving mesh cosmology: numerical techniques and global statistics (2011, background): “It is widely appreciated that the intracluster medium of galaxy clusters is partially supported by subsonic turbulence (Schuecker et al. 2004), which is created by curved accretion shocks around the haloes, and more importantly, by the hierarchical infall of structures.”
Chaotic cold accretion on to black holes (2013, background): “In fact, such a level of velocity fluctuations seems to be very common in gaseous haloes (e.g. Schuecker et al. 2004; Rebusco et al. 2006; Churazov et al. 2012; de Plaa et al. 2012; Sanders & Fabian 2013; and even higher in the ISM; Vazquez-Semadeni 2012) and can be confirmed by the upcoming…”
Shocking results without shocks: Subsonic turbulence in smoothed particle hydrodynamics and moving-mesh simulations (2011, methodology): “For example, Schuecker et al. (2004) analysed pressure fluctuations in the Coma cluster, finding them to be well described by a Kolmogorov power spectrum with a lower limit of 10% of the total ICM pressure being in turbulent form.”
Cosmic ray transport in galaxy clusters: implications for radio halos, gamma-ray signatures, and cool core heating (2010, background): “…is 13 The following papers provide insight into cluster turbulence: Bryan & Norman (1998); Roettiger et al. (1999b); Inogamov & Sunyaev (2003); Schuecker et al. (2004); Faltenbacher et al. (2005); Dolag et al. (2005); Subramanian et al. (2006); Schekochihin & Cowley (2006); Vazza et al.…”