Chandra observations of A2029:: The dark matter profile down to below 0.01rvir in an unusually relaxed cluster

We have used a high spatial resolution Chandra observation to examine the core mass distribution of the unusually regular cD cluster A2029. This bright, nearby system is especially well suited for analysis of its mass distribution under the assumption of hydrostatic equilibrium; it exhibits an undisturbed, symmetric X-ray morphology and a single-phase intracluster medium (ICM). From the deprojected temperature and density profiles, we estimate the total mass and the contributions of the gas and dark matter (DM) components from less than 3 to similar to3' (<4.4-260 h(70)(-1) kpc, 0.001-0.1r(vir)). The gas density pro le is not adequately described by a single-beta model fit because of an increase in the density at the center (r<17 h(70)(-1) kpc, <12&DPRIME;), but it is well fitted by either a double-β model, or a cusped β model. The temperature data increase as a function of radius and are well fitted by a Bertschinger & Meiksin profile and may be approximated by a power-law T(r)∝ r(α T), with α(T)=0.27±0.01. Using the fitted profiles to obtain smooth functions of density and temperature, we employed the equation of hydrostatic equilibrium to compute the total enclosed mass as a function of radius. We report a total mass of 9.15±0.25x10(13) h(70)(-1) M-circle dot within 260 h(70)(-1) kpc, using the chosen parameterization of gas density and temperature. The mass profile is remarkably well described down to 0.002r(vir) by the Navarro, Frenk, & White (NFW) profile, or a Hernquist profile, over two decades of radius and three decades of mass. For the NFW model, we measure a scale radius r(s)=540+/-90 h(70)(-1) kpc (approximate to0.2r(vir)) and concentration parameter c=4.4+/-0.9. The mass profile is also well approximated by a simple power-law fit [M (