The Dark Side of the Universe after Planck
  Recently released Planck data implies a smaller Hubble constant $H_0$ than
that from Hubble Space Telescope project (HST) and a larger percentage of the
matter components $\Omega_m$ compared to Supernova Legacy Survey (SNLS) in
$\Lambda$CDM model. In this paper we found that even though the tension on
$H_0$ between Planck and HST can be relaxed if the dark radiation is introduced
($\Delta N_{\rm eff}=0.536_{-0.224}^{+0.229}$ at $68\%$ CL from the datasets of
Planck+WMAP Polarization (WP)+baryon acoustic oscillation (BAO)+the combination
of supernova Union2.1 compilation of 580 SNe (Union2.1)+HST), $\Omega_m$ from
Planck is still not nicely compatible with that from SNLS. The tensions between
Planck and other astrophysical datasets can be significantly relaxed in $w$CDM
model, and the combination of these datasets prefers a phantom-like dark energy
at more than $95\%$ CL: $w=-1.15\pm 0.07$ and $w=-1.16\pm 0.06$ at $68\%$ CL
from Planck+WP+BAO+Union2.1+HST and Planck+WP+BAO+SNLS+HST respectively. From
the statistical point of view, there is no evidence for a time-evolving
equation of state ($\Delta \chi^2=-0.3$ compared to a constant equation of
state for the combination of Planck+WP+BAO+SNLS+HST).
