  In this paper, we report the results of constraining the holographic dark
energy model with spatial curvature and massive neutrinos, based on a Markov
Chain Monte Carlo global fit technique. The cosmic observational data include
the full WMAP 7-yr temperature and polarization data, the type Ia supernova
data from Union2.1 sample, the baryon acoustic oscillation data from SDSS DR7
and WiggleZ Dark Energy Survey, and the latest measurements of $H_0$ from HST.
To deal with the perturbations of dark energy, we adopt the parameterized
post-Friedmann method. We find that, for the simplest holographic dark energy
model without spatial curvature and massive neutrinos, the phenomenological
parameter $c<1$ at more than $4\sigma$ confidence level. The inclusion of
spatial curvature enlarges the error bars and leads to $c<1$ only in about
$2.5\sigma$ range; in contrast, the inclusion of massive neutrinos does not
have significant influence on $c$. We also find that, for the holographic dark
energy model with spatial curvature but without massive neutrinos, the
$3\sigma$ error bars of the current fractional curvature density $\Omega_{k0}$
are still in order of $10^{-2}$; for the model with massive neutrinos but
without spatial curvature, the $2\sigma$ upper bound of the total mass of
neutrinos is $\sum m_{\nu} < 0.48$ eV. Moreover, there exists clear degeneracy
between spatial curvature and massive neutrinos in the holographic dark energy
model, which enlarges the upper bound of $\sum m_{\nu}$ by more than 2 times.
In addition, we demonstrate that, making use of the full WMAP data can give
better constraints on the holographic dark energy model, compared with the case
using the WMAP ``distance priors''.
