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Mass Distribution in Galaxy Cluster Cores

  • Authors: M. T. Hogan, B. R. McNamara, F. Pulido, P. E. J. Nulsen, H. R. Russell, A. N. Vantyghem, A. C. Edge, and R. A. Main

2017 The Astrophysical Journal 837 51.

  • Provider: AAS Journals

Caption: Figure 7.

Percentage difference (see Equation (9)) in mass between our ISONFWMASS profiles and a singular NFW fit where a constant mass equivalent to the isothermal component at 10 kpc is accounted for in fitting. The vertical dotted lines correspond to the R2500 for each color-coded cluster. We see that systematic differences in the resultant mass profiles are ≲10% out to at least R2500, beyond which the fits diverge. The sharp transition at r ≈ 10 kpc is due to the artificial truncation of the isothermal component in the singular NFW fit. For a full description see Section 4.5.2.

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