XMM-Newton Observations of the Perseus Cluster. I. The Temperature and Surface Brightness Structure

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

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In Astronomy and Astrophysics

Citations in the corpus

On the X-ray, optical emission line and black hole mass properties of local Seyfert galaxies ! (2006, result): “The hard luminosity is in agreement with Churazov et al. (2003).”
Reflections of Active Galactic Nucleus Outbursts in the Gaseous Atmosphere of M87 (2003, methodology): “The gas temperature map was calculated as described by Churazov et al. (1996; see also Churazov et al. 2003 for this method applied to XMM-Newton data for the Perseus Cluster).”
Constraining the population of cosmic ray protons in cooling flow clusters with γ-ray and radio observations: Are radio mini-halos of hadronic origin? (2003, unknown): “.. . . . . . . . . . ASCA GIS 7.2 4.5 (f) (a) Irwin & Bregman (2000), (b) Lima Neto et al. (2001), (c) Churazov et al. (2003), (d) Voigt et al. (2002), (e) Johnstone et al. (2002), (f) White (2000), (g) Matsushita et al. (2002), (h) Arnaud et al. (2001), (i) Sun et al. (2002). where we again…”
FERMI DISCOVERY OF GAMMA-RAY EMISSION FROM NGC 1275 (2009, methodology): “…andXMM-Newton observations with excellent angular resolution to resolvethe nucleus revealed that non-thermal nucleus emission is well represented by a simple power-law function of Γ = 1.65 (Churazov et al. 2003; Balmaverde et al. 2006; Molendi& Gastaldello 2009), with some hints of flux variations.”
A deeper X‐ray study of the core of the Perseus galaxy cluster: the power of sound waves and the distribution of metals and cosmic rays (2007, methodology): “This hard component has been confirmed with XMM–Newton data (Molendi, private communication).”
STIRRING UP THE POT: CAN COOLING FLOWS IN GALAXY CLUSTERS BE QUENCHED BY GAS SLOSHING? (2009, background): “…(“cold fronts”), concentric with respect to the brightness peak of the cluster (e.g., Mazzotta et al. 2001; Markevitch et al. 2001, 2003b; Churazov et al. 2003; Ascasibar & Markevitch 2006, hereafter AM06; for a review of observations and simulations see Markevitch & Vikhlinin 2007).”
XMM—Newton observations of the Perseus cluster — II. Evidence for gas motions in the core (2003, methodology): “The low equivalent width region to the West of the cluster center is apparently the result of higher gas temperature in this region (see Churazov et al. 2003), since in the abundance map this feature is absent.”
A deep Chandra observation of the Perseus cluster: shocks and ripples (2003, background): “3 D I S C U S S I O N The swirl seen in the gross temperature structure is probably due to some angular momentum remaining from the merger history of the Perseus cluster (Fabian et al. 2000; Churazov et al. 2003; Motl et al. 2003).”
Filaments, Bubbles, and Weak Shocks in the Gaseous Atmosphere of M87 (2006, background): “The solution for emissivities minimizing the 2 deviation from the observed surface brightness in the set of annuli can be easily found (see, e.g., Churazov et al. 2003).”
Improved constraints on dark energy from Chandra X-ray observations of the largest relaxed galaxy clusters (2007, background): “2006; Rafferty et al. 2006) and/or ‘sloshing’ of the X-ray emitting gas within the central potentials (e.g. Churazov et al. 2003; Markevitch et al. 2003; Ascasibar & Markevitch 2006).”
A Fundamental plane of black hole activity (2003, unknown): “…Nagar et al. (2002); (30) Barth, Ho & Sargent (2002); (31) Terashima & Wilson (2003); (32) Allen et al. (2001); (33) Hereudeau & Simien (1998); (34) Churazov et al. (2003); (35) Fabbiano et al. (1992); (36) Shih et al. (2003); (37) Loewenstein et al. (2001); (38)Merritt & Ferrarese (2001); (39) Di…”
X-ray Spectroscopy of Cooling Clusters (2005, background): “Some may be cooler, denser groups that have fallen to the center, whereas others may be cooled gas that already was present in the core of the cluster but is oscillating because of a merger in the cluster outskirts (Churazov et al. 2003).”