For odd parity, in asymptotic flat and dS spacetime, the perturbation frequency (Re(o>)) becomes smaller and the decay rate ([absolute value of (Im([omega]))]) decreases when b increases.
Caption: FIGURE 2: The effective potential for odd parity gravitational perturbation in asymptotically flat spacetime, with [r.sub.h] = 1, l = 2 (a) and with [r.sub.h] = 1, b = 5 (b).
Caption: FIGURE 3: The temporal evolution of odd parity gravitational perturbation in asymptotically flat phantom BH, with [r.sub.h] = 1, l = 2 (a) and with [r.sub.h] =1, b = 5 (b).
Caption: FIGURE 4: Calculated quasinormal frequencies of odd parity gravitational perturbation for [r.sub.h] = 1 in asymptotically flat spacetime.
Caption: FIGURE 5: The effective potential for odd parity gravitational perturbation in dS spacetime with [r.sub.h] = 1, [r.sub.c] = 10, l = 2 (a) and with [r.sub.h] = 1, [r.sub.c] = 10, b = 5 (b).
Caption: FIGURE 6: The temporal evolution of odd parity gravitational perturbation for dS phantom BH with [r.sub.h] = 1, l = 2 (a), and with [r.sub.h] = 1, b = 5 (b).
Caption: FIGURE 7: Calculated quasinormal frequencies of odd parity gravitational perturbation with [r.sub.h] = 1, [r.sub.c] = 10 in dS spacetime.
Caption: FIGURE 8: The effective potential for odd parity gravitational perturbation in AdS spacetime with [r.sub.h] =1, l = 2 (a) and with [r.sub.h] = 1, b = 1 (b).
