Castillo Morales, María ÁfricaSchindler, S.2023-06-202023-06-2020021. Fukazawa, Y. 1997, Ph.D. thesis, Univ. Tokyo. 2. Allen S.W. & Fabian A.C., Mon. Not. R. Astr. Soc. 297, 57 (1998). 3. Arnaud M. & Evrard A.E., Mon. Not. R. Astr. Soc. 305, 631 (1999). 4. Ettori S. & Fabian A.C., Mon. Not. R. Astr. Soc. 305, 834 (1999). 5. Horner D.J., et al, Astrophys. J. 520, 78 (1999). 6. Jones C. & Forman W.R., Astrophys. J. 511, 65 (1999). 7. Mohr J.J., et al, Astrophys. J. 517, 627 (1999). 8. Schindler S., Astron. Astrophys. 349, 435 (1999). 9. Schindler S., et al, Astron. Astrophys submitted (2001). 10. Neumann D.M.& Arnaud M., Astron. Astrophys. 348, 711 (1999). 11. Stanford S.A., et al, Astrophysical Journal in press, astro-ph/0012250. 12. Cavaliere A. & Fusco-Fermiano F., Astron. Astrophys. 49, 137 (1976). 13. Peres C.B., et al, Mon. Not. R. Astr. Soc. 298, 416 (1998). 14. Allen S.W. & Fabian A.C., Mon. Not. R. Astr. Soc. 286, 583 (1997). 15. White D.A, et al, Mon. Not. R. Astr. Soc. 292, 419 (1997). 16. Markevitch M., et al, Astrophys. J. 503, 77 (1998). 17. White D.A, Mon. Not. R. Astr. Soc. 312, 663 (2000). 18. Irwin, J.A & Bregman, J.N., Astrophys. J. 538, 543 (2000). 19. Evrard A., et al, Astrophys. J. 469, 494 (1996). 20. Matsumoto H., et al, Publ. Astr. Soc. Japan. 52, 153 (2000). 21. Reiprich T.H. & Böhringer H., Proceedings of the Workshop ‘Diffuse thermal and relativistic plasma in galaxy cluster’. Ringberg Castle, Germany, April 19-23, 1999, p.157.1-58381-108-7https://hdl.handle.net/20.500.14352/60926Workshop on Tracing Cosmic Evolution with Galaxy Clusters (2001. Sesto Pusteria, Italy). We would like to thank the organizers of the meeting for the financial support. We thank Javier Campania for the help printing the poster.We present the analysis of baryonic and non-baryonic matter distributions in a sample of eleven nearby clusters (0.03 < z < 0.09) with temperatures between 4.4 and 9.4 keV. These galaxy clusters have been studied in detail using X-ray data and global physical properties have been determined. Correlations between these quantities have been analysed and compared with the results for distant clusters. We found an interesting dependence between the relative gas extent (expressed as the ratio of gas mass fractions at r(500) and 0.5 x r(500)) and the total cluster mass. The extent of the gas relative to the extent of the dark matter tends to be larger in less massive clusters. This dependence might give us some hints about non-gravitational processes in clusters.engbook parthttp://arxiv.org/pdf/astro-ph/0106201v1.pdfopen access52Astronomy and astrophysicsAstrofísicaAstronomía (Física)