  The asymptotic quasinormal frequencies of the brane-localized
$(4+n)$-dimensional black hole are computed. Since the induced metric on the
brane is not an exact vacuum solution of the Einstein equation defined on the
brane, the real parts of the quasinormal frequencies $ \omega$ do not approach
to the well-known value $T_H \ln 3$ but approach to $T_H \ln k_n$, where $k_n$
is a number dependent on the extra dimensions. For the scalar perturbation
$Re(\omega / T_H) = \ln 3$ is reproduced when $n = 0$. For $n \neq 0$, however,
$Re(\omega / T_H)$ is smaller than $\ln 3$. It is shown also that when $n > 4$,
$Im(\omega / T_H)$ vanishes in the scalar perturbation. For the gravitational
perturbation it is shown that $Re(\omega / T_H) = \ln 3$ is reproduced when $n
= 0$ and $n = 4$. For different $n$, however, $Re(\omega / T_H)$ is smaller
than $\ln 3$. When $n = \infty$, for example, $Re(\omega / T_H)$ approaches to
$\ln (1 + 2 \cos \sqrt{5} \pi) \approx 0.906$. Unlike the scalar perturbation
$Im(\omega / T_H)$ does not vanish regradless of the number of extra
dimensions.
