XMM - Newton Observation of the Cluster of Galaxies Abell 1060

We present results from the XMM-Newton observation of the non-cooling flow cluster A 1060. Large effective area of XMM-Newton enables us to investigate the nature of this cluster in unprecedented detail. From the observed surface brightness distribution, we have found that the gravitational mass distribution is well described by the NFW profile but with a central density slope of ∼1.5. We have undoubtedly detected a radial temperature decrease of as large as ∼30% from the center to the outer region (r ∼ 13 ′), which seems much larger than that expected from the temperature profile averaged over nearby clusters. We have established that the temperature of the 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 4×10 7 yr (the sound-crossing time) and 3×10 8 yr (the thermal conduction time) ago. We have found that the high-metallicity blob located at ∼ 1. ′ 5 northeast of NGC 3311 is more extended and its iron mass of 1.9 × 10 7 M ⊙ is larger by an order of magnitude than estimated from our Chandra observation. The amount of iron can still be considered as being injected solely from the elliptical galaxy NGC 3311.