The scatter in the radial profiles of X-ray luminous galaxy clusters as diagnostic of the thermodynamical state of the ICM

Authors

  • F. Vazza,

    Corresponding author
    1. Jacobs University Bremen, Campus Ring 1, 28759, Bremen, Germany
    2. INAF/Istituto di Radioastronomia, via Gobetti 101, I-40129 Bologna, Italy
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  • M. Roncarelli,

    1. Dipartimento di Astronomia, Università di Bologna, via Ranzani 1, I-40127 Bologna, Italy
    2. Centre d’Etude Spatiale des Rayonnements, CNRS/Université de Toulouse, 9 avenue du Colonel Roche, BP44346, 31028 Toulouse Cedex 04, France
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  • S. Ettori,

    1. Istituto Nazionale di Astrofisica – Osservatorio Astronomico di Bologna, Via Ranzani 1, I-40127 Bologna, Italy
    2. INFN, Sezione di Bologna, viale Berti Pichat 6/2, I-40127 Bologna, Italy
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  • K. Dolag

    1. Max-Planck-Institut für Astrophysik, Garching, Germany
    2. University Observatory Munich, Scheinerstr. 1, D-81679 Munich, Germany
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E-mail: f.vazza@jacobs-university.de

ABSTRACT

We study the azimuthal scatter in the radial profiles of X-ray luminous galaxy clusters with two sets of high-resolution cosmological re-simulations obtained with the codes enzo and gadget2. The average gas profiles are computed for different angular sectors of the cluster projected volume and compared with the mean cluster profiles at each radius from the centre. We report that, in general, the level of azimuthal scatter is found to be ∼10 per cent for gas density, temperature and entropy inside R200, and ∼25 per cent for X-ray luminosity for the same volume. These values generally double approaching 2R200 from the cluster centre, and are generally found to be higher (by ∼20–40 per cent) in the case of perturbed systems. A comparison with the results from recent Suzaku observations is discussed, showing the possibility to simply interpret the large azimuthal scatter of observables in light of our simulated results.

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