2006PASJ...58..695H

We present results from an XMM-Newton observation of the non-cooling flow cluster Abell 1060. The large effective area of XMM-Newton enabled us to investigate the nature of this cluster in unprecedented detail. >From the observed surface brightness distribution, we found that the gravitational mass distribution is well described by the Navarro-Frenk-White (1997, ApJ, 490, 493) profile, but with a central density slope of ∼1.5. We established that the temperature of a region ∼7' southeast of the center is higher than the azimuthally averaged temperature of the same radius by ∼20%. Since the pressure of this region already reaches equilibrium with the environment, the temperature structure can be interpreted as having been produced between 4 x 10⁷ yr (the sound-crossing time) and 3 x 10⁸ yr (the thermal conduction time) ago. We found that a high-metallicity blob located at ∼1'.5 northeast of NGC 3311 is more extended, and its iron mass of 1.9 x 10⁷ M_☉ is larger by an order of magnitude than that estimated from our Chandra observation. The amount of iron can still be considered as being injected solely from the elliptical galaxy NGC 3311.