 [Deg.] 13 0 2 4 6 8 10 12 B −15 10$^{−14}$ 10$^{−13}$ 10$^{−12}$ 10$^{−11}$ 10$^{−10}$ 10 −9 10  [Deg.] 23 38 40 42 44 46 48 50 B −15 10$^{−14}$ 10$^{−13}$ 10$^{−12}$ 10$^{−11}$ 10$^{−10}$ 10 −9 10 FIG. 8: Figures show the predictions of η$_{B}$ for M$_{3}$ ≃ 1TeV and δ$_{N}$$_{3}$$_{η}$ = 10 − $^{5}$. Left-figure shows η$_{B}$ as a function of θ$_{13}$ . Right-figure shows η$_{B}$ as a function of θ$_{23}$ . The horizontal dotted lines in both figures correspond to the phenomenologically acceptable current measurement, and the horizontal thick line represents the best-fit value η$_{B}$ = 6 . 2 × 10 − 10 of current measurement from WMAP [25]. And the vertical dotted lines represent the experimental bounds in 1 σ of the mixing angles θ$_{13}$ and θ$_{23}$ in neutrino oscillations. approximately given $^{4}$, for x ≪ 1, by As can be seen in Eqs. (44,45), since the lepton asymmetries in µ and τ flavors are equal but opposite in sign to the first order, i.e. ε µ 3 ≈ − ε τ $_{3}$, satisfying ε µ 3 + ε τ 3 = − ε e $_{3}$, and the wash-out parameters in µ and τ are almost equal K µ 3 ≈ K τ 3 ≫ K e $_{3}$, the effects of wash-out factor related with N$_{3}$ can play a crucial role in a successful leptogenesis according to the size of δ$_{N}$$_{3}$$_{η}$ . In strong wash-out regime K α 3 > 1 ( α = e, µ, τ ), given the initial thermal abundance of N$_{3}$ and the condition for K α $_{3}$, the resulting baryon-to-photon ratio η$_{B}$ including lepton flavor effects can be approximately given as ε e 3 = bx $^{2}$g2 ν 32 aπ ( x sin φ + a sin 2 φ ) , ε µ 3 ≃ bxg 2 ν 64 aπ { 4 $_{a}$√$_{3 cos}$$_{φ}$ − x $_{[}$√$_{3 + 2}$$_{a}$$_{cos}$$_{φ}$$_{(}$ √$_{3 cos}$$_{φ}$ + sin φ )] } , ε τ 3 ≃ bxg 2 ν 64 aπ {− 4 $_{a}$√$_{3 cos}$$_{φ}$ + x $_{[}$√$_{3 + 2}$$_{a}$$_{cos}$$_{φ}$$_{(}$ √$_{3 cos}$$_{φ}$ − sin φ )] } . (45) η$_{B}$ ≃ 4 × $_{10}$− $^{3}$ε e 3 ( 1 K e 3 ) 1 . 16 . (46) 22 4 Due to Im[ H 3 $_{j}$] = 0 for ϕ 1 , 2 = 0, the relation ε µ 3 + ε τ 3 = − ε e 3 is satisfied if they are considered to the order of x $^{3}$.