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We present an XMM-Newton observation of A1413, a hot (kT = 6.5 keV) galaxycluster at z=0.143. We construct gas and temperature profiles up to ~1700 kpc,equivalent to ~0.7 r_200. The gas distribution is well described by a betamodel in the outer regions, but is more concentrated in the inner ~250 kpc. Weintroduce a new parameterisation for the inner regions, allowing a steeper gasdensity distribution. The projected radial temperature profile declinesgradually towards the outer regions, by ~20% between 0.1 r_200 and 0.5 r_200,and is well described by a polytropic model with gamma = 1.07+/-0.01. We findthat neither projection nor PSF effects change substantially the form of thetemperature profile. Assuming hydrostatic equilibrium (HE) and sphericalsymmetry, we use the observed temperature profile and the new parametric formfor the gas density profile to produce the total mass distribution. The massprofile is remarkably well fitted with the Moore et al. (1999) parameterisationwith a concentration parameter in the range expected from numericalsimulations. There are several indications that beyond a density contrast delta\~600, the gas may no longer be in HE. There is an offset with respect toadiabatic numerical simulations in the virialised part of the cluster, in thatthe predicted mass for the cluster temperature is ~40% too high. The gasdistribution is peaked in the centre primarily as a result of the cusp in thedark matter profile. The X-ray gas to total mass ratio rises with increasingradius to f_gas ~ 0.2. These data strongly support the validity of the currentapproach for the modelling of the dark matter collapse, but confirm thatunderstanding the gas specific physics is essential. (Abridged)Comment: To appear in A&

The mass profile of A1413 observed with $\vec {XMM}$–$\vec {Newton}$: Implications for the M–T relation