Chandra Observations of Abell 2029: The Dark Matter Profile Down to <0.01 R_vir in an Unusually Relaxed Cluster

Details Chandra Observations of Abell 2029: The Dark Matter Profile Down to <0.01 R_vir in an Unusually Relaxed Cluster Chandra Observations of Abell 2029: The Dark Matter Profile Down to <0.01 R_vir in an Unusually Relaxed Cluster

2002-09-11

arxiv.org/abs/astro-ph/0209205v2

Astrophys.J. 586 (2003) 135-142

Astronomy and Astrophysics

Astrophysics

ApJ Accepted Version; to appear in 2003 March 20 Issue; 8 pages, emulateapj5, 3 figures (2 color)

Scientific paper

10.1086/367556

We have used a high resolution Chandra observation to examine the core mass distribution of the unusually regular cD cluster Abell 2029. This system is especially well-suited for analysis of its mass distribution under the assumption of hydrostatic equilibrium: it exhibits an undisturbed X-ray morphology and a single-phase ICM. We estimate the total mass, and the contributions of the gas and dark matter components from <3 arcsec to ~3 arcmin (<4.4-260 kpc, 0.001-0.1 r_vir). The gas density is well fitted by either a double beta-model, or a ``cusped'' beta-model. The temperature data are increasing, and can be approximated by a power-law, with alpha_T = 0.27+/-0.01. Fitting smooth functions to density and T, we obtain a mass profile, which is remarkably well described down to 0.002 r_vir by the NFW model, for which we measure r_scale = 540+/-90 kpc (~0.2 r_vir) and c = 4.4 +/- 0.9. The mass profile is also approximated by a power-law fit with alpha_m = 1.81+/-0.04 (corresponding to a logarithmic density slope of -1.19+/-0.04). The density profile is too shallow to be fitted with a Moore et al. model. The consistency with NFW at <0.01 r_vir is incompatible with SIDM, and contrasts with the results from rotation curves of LSB and dwarf galaxies. This suggests that while CDM may adequately describe clusters, it does not currently account properly for small halos. Using the cD light, we observe a total M/L_V ~ 12 at r < 20 kpc, rising to > 100 beyond 200 kpc. The consistency with an NFW halo model and the large M/L suggest the cluster is DM-dominated down to <~ 0.005 r_vir. We observe a gas mass fraction = 0.139+/-0.004 at the limit of our observations, finding an upper limit to Omega_m <= 0.29+/-0.03 (abridged).

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