In this paper , we report the results of constraining the dynamical dark energy with a divergence-free parameterization , w ( z ) = w _ { 0 } + w _ { a } \left ( \frac { \ln ( 2 + z ) } { 1 + z } - \ln 2 \right ) , in the presence of spatial curvature and massive neutrinos , with the 7-yr WMAP temperature and polarization data , the power spectrum of LRGs derived from SDSS DR7 , the Type Ia supernova data from Union2 sample , and the new measurements of H _ { 0 } from HST , by using a MCMC global fit method .
Our focus is on the determinations of the spatial curvature , \Omega _ { k } , and the total mass of neutrinos , \sum m _ { \nu } , in such a dynamical dark energy scenario , and the influence of these factors to the constraints on the dark energy parameters , w _ { 0 } and w _ { a } .
We show that \Omega _ { k } and \sum m _ { \nu } can be well constrained in this model ; the 95 \% CL limits are : -0.0153 < \Omega _ { k } < 0.0167 and \sum m _ { \nu } < 0.56 eV .
Comparing to the case in a flat universe , we find that the error in w _ { 0 } is amplified by 25.51 \% , and the error in w _ { a } is amplified by 0.14 \% ; comparing to the case with a zero neutrino mass , we find that the error in w _ { 0 } is amplified by 12.24 \% , and the error in w _ { a } is amplified by 1.63 \% .