constant model when the coupling is proportional to the energy density of DM and total dark sectors. The Press-Schechter formalism we employed is good enough for the purpose of this paper to illustrate how the interaction between dark sectors and the DE inhomogeneities influence cluster number counts, but it is still not easy to seek precise confrontations with observational data at the present moment. Recently in the uncoupled model, the statistical analysis was performed on the sensitivity of cluster counts to DE perturbations by employing a set of cosmological parameters using the Fisher matrix method. It was argued that the impact of DE fluctuations is large enough, which could already be detected by existing instruments[32]. It is of great interest to extend their analysis to examine the interaction between DE and DM effect and the DE inhomogeneities influence. Such a study is under way. This work has been supported partially by NNSF of China and the National Basic Research Program of China under grant 2010CB833000 and brazilian foundations CNPq and FAPESP. Acknowledgments [1] S. J. Perlmutter et al., Nature 391, 51 (1998); A. G. Riess et al., Astron. J. 116, 1009 (1998); S. J. Perlmutter et al., Astroph. J. 517, 565 (1999); J. L. Tonry et al., Astroph. J. 594, 1 (2003); A. G. Riess et al., Astroph. J. 607, 665 (2005); P. Astier et al., Astron. Astroph. 447, 31 (2005); A G. Riess et al., Astroph. J. 659, 98 (2007). [2] L. Amendola, Phys. Rev. D 62, 043511 (2000); L. Amendola and C. Quercellini, Phys. Rev. D 68, 023514 (2003); L. Amendola, S. Tsujikawa, and M. Sami, Phys. Lett. B 632, 155 (2006). [3] D. Pavon, W. Zimdahl, Phys. Lett. B 628, 206 (2005); S. Campo, R. Herrera, D. Pavon, Phys. Rev.D 78, 021302(R) (2008). [4] C. G. Boehmer, G. Caldera-Cabral, R. Lazkoz, and R. Maartens, Phys. Rev. D 78, 023505 (2008). [5] G. Olivares, F. Atrio-Barandela, and D. Pavon, Phys. Rev. D 74, 043521 (2006). [6] S. B. Chen, B. Wang, and J. L. Jing, Phys.Rev.D 78, 123503 (2008). [7] J. Valiviita, E. Majerotto, and R. Maartens, JCAP 07, 020 (2008), ArXiv:0804.0232. [8] J. -H. He, B. Wang, and E. Abdalla, Phys. Lett. B 671, 139 (2009), ArXiv:0807.3471. [9] P. Corasaniti, Phys.Rev.D 78, 083538 (2008); B. Jackson, A. Taylor, and A. Berera, Phys.Rev.D 79, 043526 (2009). [10] D. Pavon, B. Wang, Gen. Relav. Grav. 41,1,(2009); B. Wang, C.-Y. Lin, D. Pavon, and E. Abdalla, Phys. Lett. B 662, 1, (2008). [11] B. Wang, J. Zang, C.-Y. Lin, E. Abdalla, and S. Micheletti, Nucl. Phys. B 778, 69 (2007). [12] W. Zimdahl, Int. J. Mod. Phys. D 14, 2319 (2005). [13] Z. K. Guo, N. Ohta, and S. Tsujikawa, Phys. Rev. D 76, 023508 (2007). [14] C. Feng, B. Wang, E. Abdalla, and R. K. Su, Phys. Lett. B 665, 111 (2008), ArXiv:0804.0110. [15] J. Valiviita, R. Maartens, and E. Majerotto, ArXiv:0907.4987. [16] J. Q. Xia, ArXiv:0911.4820. [17] J.-H. He, B. Wang, and P. Zhang, Phys. Rev. D 80, 063530 (2009), ArXiv:0906.0677. [18] J.-H. He, B. Wang, JCAP 06, 010 (2008), ArXiv:0801.4233. [19] J. H. He, B. Wang, and Y. P. Jing, JCAP 07, 030 (2009) ArXiv:0902.0660. [20] C. G. Tsagas, A. Challinor, and R. Maartens, Phys.Rept. 465, 61(2008), ArXiv:0705.4397. [21] G. Caldera-Cabral, R. Maartens, and B. Schaefer, JCAP 07, 027 (2009). [22] O. Bertolami, F. Gil Pedro, and M. Le Delliou, Phys. Lett. B 654, 165 (2007). O. Bertolami, F. Gil Pedro, and M. Le Delliou, ArXiv:0705.3118. [23] E. Abdalla, L.Raul W. Abramo, L. Sodre Jr., and B. Wang, Phys. Lett. B673, 107 (2009); E. Abdalla, L. Abramo, J. Souza, ArXiv:0910.5236. [24] T. Multamaki, M. Manera,and E. Gaztanaga, MNRAS 344, 761 (2003). [25] P. Solevi, R. Mainini, S. A. Bonometto, A. V. Macci, A. Klypin, and S. Gottlber, ArXiv:astro-ph/0504124. [26] D.F. Mota, C. van de Bruck, Astron. Astrophys. 421, 71 (2004), ArXiv:astro-ph/0401504. 21