The distant galaxy cluster XLSSJ022403.9-041328 on the L X –T X –M scaling relations using Chandra and XMM–Newton observations
We present a very detailed analysis of Chandra and XMM–Newton observations of XLSSJ022403.9-041328 galaxy cluster of z=1, which was detected during the XMM-Newton Large Scale Structure survey. To define the “luminosity-temperature-mass”, L X –T X –M, scaling relations we built temperature, surface brightness, density, and mass profiles. The total gravitational mass of this cluster was taken within the scaled radius, R500, was determined under the assumption of hydrostatic equilibrium for intercluster gas and spherical symmetry of a cluster.
The temperature of XLSSJ022403.9-041328 was found to be 4.5±0.7 keV from the Chandra data, and 3.8±0.3 from the XMM–Newton data. The total gravitational mass is equal to 1.44±0.23×1014M⊙ at the corresponding radius, while the fraction of gas is equal to 15 % of a total mass. These values were used to define the XLSSJ022403.9-041328 galaxy cluster at the L X –T X –M g scaling relations, and for all of these cases we got agreement which fitting well with self-similar model. This research permits us to use L X –T X –M relations for galaxy clusters at a highest redshift in the cosmological probes.
KeywordsCosmology: observations Large scale structure of Universe Dark matter Galaxies X-rays: galaxies: clusters XLSSJ022403-041328
The authors wish to thank all staff members involved in the Chandra and XMM–Newton projects. The HEASARC on-line data archive at NASA/GSFC was used extensively in this research. This work was partially supported in frame of the Target Program of Space Science Research of the National Academy of Science of Ukraine (2012–2016).
- Andreon, S., Pierre, M., XMM-LSS collaboration: SAIt Mem. Suppl. 3 188 (2003) Google Scholar
- Arnaud, K.: In: Jacoby, G.H., Barnes, J. (eds.) Astronomical Data Analysis Software and Systems V, XSPEC: The First Ten Years, PASP, vol. 101, p. 17 (1996) Google Scholar
- Bergé, J., Pacaud, F., Réfrégier, A., et al.: Astron. Astrophys. 385, 695 (2008) Google Scholar
- Metzler, C., Evrard, A.: astro-ph/9710324 (1997)