hierarchy between S$_{D}$ and δ$_{L}$ . In Fig. 10, we give the FSR and VIB contributions to the gamma-ray spectrum for three different DM mass cases ( m$_{D}$ = 2 . 5 , 4 and 6 TeV). Here we have fixed the triplet mass m$_{δ}$$_{L}$ = 1 TeV and the DM lifetime τ$_{D}$ = 0 . 9 × 10 26 s. We can see that with m$_{D}$ increasing, the VIB contribution becomes more significant relative to FSR. For a low m$_{D}$ = 2 . 5 TeV, the contribution from VIB relative to that of FSR is only ∼ 7%. But for a larger m$_{D}$ = 6 TeV, the contribution can reach ∼ 20% which is non-negligible. We have discussed the DM cascade decay induced by tiny soft C -violating interactions in an extension of a left-right symmetric model in which the DM particle is identified as a gauge singlet scalar. In this scenario, the DM particle may decay favorably into leptonic final states through the intermediate SU (2)$_{L}$ triplets. We have explored the parameter space which can well explain the current PAMELA and Fermi-LAT or ATIC experimental data. It is shown that this scenario predicts significant associating signals in the flux of high energy neutrinos and gamma-rays, which is due to the correlated couplings to neutrinos and the extra contributions from the charged components of the triplet. We have found that the predicted neutrino-induced muon flux is dominated by the contribution from the neutrinos directly from the triplet decay. The gamma-ray radiation from the charged triplet scalars through VIB process can be significant in the case that the triplets are much lighter that the DM particle. This work is supported in part by the National Basic Research Program of China (973 Program) under Grants No. 2010CB833000; the National Nature Science Foundation of China (NSFC) under Grants No. 10975170, No. 10821504 and No. 10905084; and the Project of Knowledge Innovation Program (PKIP) of the Chinese Academy of Science. [1] O. Adriani et al. [PAMELA Collaboration], Nature 458 , 607 (2009) [arXiv:0810.4995 [astro- ph]]; Phys. Rev. Lett. 102 , 051101 (2009) [arXiv:0810.4994 [astro-ph]]. 23 Acknowledgments IV. CONCLUSIONS