Details

Autor(en) / Beteiligte

• Bartalucci, I.
• Arnaud, M.
• Pratt, G.W.
• Le Brun, A. M. C.

Titel

Resolving the hydrostatic mass profiles of galaxy clusters at z ∼ 1 with XMM-Newton and Chandra

Ist Teil von

• Astronomy and astrophysics (Berlin), 2018-09, Vol.617, p.A64

Ort / Verlag

Heidelberg: EDP Sciences

Erscheinungsjahr

2018

Quelle

EZB-FREE-00999 freely available EZB journals

Beschreibungen/Notizen

• We present a detailed study of the integrated total hydrostatic mass profiles of the five most massive M500SZ < 5 × 1014 M⊙ ( M 500 SZ > 5 × 10 14   M ⊙ ) $\left( {M_{500}^{{\rm{SZ}}} > 5 \times {{10}^{14}}\,{M_ \odot }} \right)$ galaxy clusters selected at z ∼ 1 via the Sunyaev–Zel’dovich effect. These objects represent an ideal laboratory to test structure formation models where the primary driver is gravity. Optimally exploiting spatially-resolved spectroscopic information from XMM-Newton and Chandra observations, we used both parametric (forward, backward) and non-parametric methods to recover the mass profiles, finding that the results are extremely robust when density and temperature measurements are both available. Our X-ray masses at R500 are higher than the weak lensing masses obtained from the Hubble Space Telescope (HST), with a mean ratio of 1.39−0.35+0.47 1.39 − 0.35 + 0.47 $1.39^{+0.47}_{-0.35}$ . This offset goes in the opposite direction to that expected in a scenario where the hydrostatic method yields a biased, underestimated, mass. We investigated halo shape parameters such as sparsity and concentration, and compared to local X-ray selected clusters, finding hints for evolution in the central regions (or for selection effects). The total baryonic content is in agreement with the cosmic value at R500. Comparison with numerical simulations shows that the mass distribution and concentration are in line with expectations. These results illustrate the power of X-ray observations to probe the statistical properties of the gas and total mass profiles in this high mass, high-redshift regime.