Astrophysics and Space Science

, Volume 349, Issue 1, pp 415–421

The Chandra X-ray galaxy clusters at z<1.4: constraints on the evolution of LXTMg relations

Original Article

DOI: 10.1007/s10509-013-1630-z

Cite this article as:
Babyk, I. & Vavilova, I. Astrophys Space Sci (2014) 349: 415. doi:10.1007/s10509-013-1630-z


We analyzed the luminosity-temperature-mass of gas (LXTMg) relations for a sample of 21 Chandra galaxy clusters. We used the standard approach (β−model) to evaluate these relations for our sample that differs from other catalogues since it considers galaxy clusters at higher redshifts (0.4<z<1.4). We assumed power-law relations in the form \(L_{X} \sim(1 +z)^{A_{L_{X}T}} T^{\beta_{L_{X}T}}\), \(M_{g} \sim(1 + z)^{A_{M_{g}T}} T^{\beta_{M_{g}T}}\), and \(M_{g} \sim(1 + z)^{A_{M_{g}L_{X}}} L^{\beta_{M_{g}L_{X}}}\). We obtained the following fitting parameters with 68 % confidence level: \(A_{L_{X}T} = 1.50 \pm0.23\), \(\beta_{L_{X}T} = 2.55 \pm0.07\); \(A_{M_{g}T} = -0.58 \pm0.13\) and \(\beta_{M_{g}T} = 1.77 \pm0.16\); \(A_{M_{g}L_{X}} \approx-1.86 \pm0.34\) and \(\beta_{M_{g}L_{X}} = 0.73 \pm0.15\), respectively. We found that the evolution of the MgT relation is small, while the MgLX relation is strong for the cosmological parameters Ωm=0.27 and ΩΛ=0.73. In overall, the clusters at high-z have stronger dependencies between LXTMg correlations, than those for clusters at low-z. For most of galaxy clusters (first of all, from MACS and RCS surveys) these results are obtained for the first time.


Galaxy clusters: general X-ray clusters 

Copyright information

© Springer Science+Business Media Dordrecht 2013

Authors and Affiliations

  1. 1.Main Astronomical Observatory of the NAS of UkraineKyivUkraine

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