0.08 0.1 0.12 0.14 0.16 0.18 0.2 GLYPH<CapOmega> h 2 75 100 125 150 175 200 225 250 m$^{N}$ GLYPH<OverTilde> GLYPH<LParen1> GeV GLYPH<RParen1> FIG. 13: Ω h 2 vs m$_{˜}$ $_{N}$. The solid lines from left to right are for Ω h 2 = 0.094 and 0.129 respectively. The Z ′ -ino mass is equal to the Bino mass since the new U (1) gauge coupling is the same as the hypercharge gauge coupling. in the original condensate that drives inflation is lost. However, the neutrino Yukawa, h , is way too small to allow acceptable thermal dark matter. Note that ˜ N would dominate the universe right after the end of inflation if it had no gauge interactions. In order to calculate the relic abundance of the RH sneutrino, it is necessary to know the masses of the additional gauge boson Z ′ and its SUSY partner ˜ Z ′ , the new Higgsino masses, Higgs VEVs which break the new U (1) gauge symmetry, the RH sneutrino mass, the new gauge coupling, and the charge assignments for the additional U (1). Assuming that the new gauge symmetry is broken around 2 TeV, and the existence of two new Higgs superfields to maintain the theory anomaly free. The primary diagrams responsible to provide the right amount of relic density are medi- ated by ˜ Z ′ in the t -channel. In Fig. (13), we show the relic density values for smaller masses of sneutrino. In the case of a larger sneutrino mass in this model, the correct dark matter abundance can be obtained by annihilation via Z ′ pole [716, 738]. A sneutrino mass in the 1 − 2 TeV range provides a good fit to the PAMELA data and a reasonable fit to the ATIC data [739]. Since the dark matter candidate, the RH sneutrino, interacts with quarks via the Z ′ boson, it is possible to see it via the direct detection experiments. The detection cross sections are not small as the interaction diagram involves Z ′ in the t -channel. The typical cross section is about 2 × 10 − 8 pb for a Z ′ mass around 2 TeV, makes it possible to probe 165