10 prospects we have obtained from neutrino tele- scope should be considered in any explanations based on iDM. Other on-going indirect detection experiments and the Large Hadron Collider also have the capability to detect the DM signals. It is exciting and useful to think about all these exper- iments and achieve a complete picture of DM. stringent constraints to the hard DM annihilation channels such as W $^{+}$W $^{−}$, ZZ , t ¯ t and τ $^{+}$τ $^{−}$. For the soft channels such as b ¯ b and c ¯ c , the limits are loose. With the IceCube 80-strings plus DeepCore, it can discover or exclude such channels. If the DM annihilation products are light charged lep- tons e $^{+}$e $^{−}$, µ $^{+}$µ $^{−}$, light mesons or some new light bosons, there are no constraints from the neutrino detection. For neutrinos from DM annihilation in the Earth, the constraint is weaker than the one in the Sun. This is mainly due to the fact that Earth being a small gravitational system that cap- tures the DM. Moreover, the terrestrial iDM cap- ture rate is suppressed due to the inelastic cap- ture condition. Furthermore, the terrestrial iDM capture and annihilation do not reach equilibrium in most of its parameter space. The constraint is available only for small δ and iDM with mass of several tens of GeV where similar behaviors as the “resonance enhancement” in the eDM case occur. If the DAMA and CDMS II results are really in- duced by DM, we could expect the XENON 100 [36] or other direct detection experiments to give the similar observations in the immediate future. Nevertheless, the constraints and future detection We would like to thank Paul H. Frampton, Sourav Mandal and Matthew Sudano for useful discussions. The work of J.S. was supported by the World Premier International Research Center Ini- tiative (WPI initiative) MEXT, Japan and Grant- in-Aid for scientific research (Young Scientists (B) 21740169) from Japan Society for Promotion of Science (JSPS). The work of P.F.Y. and S.H.Z was supported by the Natural Sciences Foundation of China (Nos. 10775001, 10635030). P.F.Y. would like to acknowledge the hospitality of Institute for Physics and Mathematics of the Universe (IPMU) while the work was initiated. VI. ACKNOWLEDGEMENT [1] E. Komatsu et al. [WMAP Collaboration], Astro- phys. J. Suppl. 180 , 330 (2009) [arXiv:0803.0547 [astro-ph]]. [2] A. Borriello and P. Salucci, Mon. Not. Roy. As- tron. Soc. 323 , 285 (2001). [3] H. Hoekstra, H. Yee and M. Gladders, New As- tron. Rev. 46 , 767 (2002). [4] R. B. Metcalf, L. A. Moustakas, A. J. Bunker and I. R. Parry, Astrophys. J. 607 , 43 (2004); L. A. Moustakas and R. B. Metcalf, Mon. Not. Roy. Astron. Soc. 339 , 607 (2003) [5] R. Bernabei et al. [DAMA Collaboration], Eur. Phys. J. C 56 , 333 (2008) [arXiv:0804.2741 [astro- ph]]. [7] S. Chang, G. D. Kribs, D. Tucker-Smith and N. Weiner, Phys. Rev. D 79 , 043513 (2009) [arXiv:0807.2250 [hep-ph]]. [6] D. Tucker-Smith and N. Weiner, Phys. Rev. D 64 , 043502 (2001) [arXiv:hep-ph/0101138]. [8] Z. Ahmed et al. [The CDMS-II Collaboration and CDMS-II Collaboration], arXiv:0912.3592 [astro- ph.CO]. [9] M. Kadastik, K. Kannike, A. Racioppi and M. Raidal, arXiv:0912.3797 [hep-ph]; N. Bernal and A. Goudelis, arXiv:0912.3905 [hep-ph]; A. Bottino, F. Donato, N. Fornengo and [11] K. Schmidt-Hoberg and M. W. Winkler, JCAP 0909 , 010 (2009) [arXiv:0907.3940 [astro-ph.CO]]. [10] J. Angle et al. [XENON Collaboration], Phys. Rev. Lett. 100 , 021303 (2008) [arXiv:0706.0039 [astro-ph]]. S. Scopel, arXiv:0912.4025 [hep-ph]. D. Feld- man, Z. Liu and P. Nath, arXiv:0912.4217 [hep-ph]; M. Ibe and T. T. Yanagida, arXiv:0912.4221 [hep-ph]; R. Allahverdi, B. Dutta and Y. Santoso, arXiv:0912.4329 [hep-ph]; M. Endo, S. Shirai and K. Yonekura, arXiv:0912.4484 [hep-ph]; Q. H. Cao, I. Low and G. Shaughnessy, arXiv:0912.4510 [hep-ph]; Q. H. Cao, C. R. Chen, C. S. Li and H. Zhang, arXiv:0912.4511 [hep-ph]; K. Cheung and T. C. Yuan, arXiv:0912.4599 [hep-ph]; J. Hisano, K. Nakayama and M. Yamanaka, arXiv:0912.4701 [hep-ph]; X. G. He, T. Li, X. Q. Li, J. Tandean and H. C. Tsai, arXiv:0912.4722 [hep-ph]; I. Gogoladze, R. Khalid, S. Raza and Q. Shafi, arXiv:0912.5411 [hep-ph]; M. Aoki, S. Kane- mura and O. Seto, arXiv:0912.5536 [hep-ph]; R. Foot, arXiv:1001.0096 [hep-ph]. M. Asano and R. Kitano, arXiv:1001.0486 [hep-ph]. W. S. Cho, J. H. Huh, I. W. Kim, J. E. Kim and B. Kyae, arXiv:1001.0579 [hep-ph].