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We employ the Planck 2013 CMB temperature anisotropy and lensing data, andbaryon acoustic oscillation (BAO) data to constrain a phenomenological $w$CDMmodel, where dark matter and dark energy interact. We assume time-dependentequation of state parameter for dark energy, and treat dark matter and darkenergy as fluids whose energy-exchange rate is proportional to the dark-matterdensity. The CMB data alone leave a strong degeneracy between the interactionrate and the physical CDM density parameter today, $\omega_c$, allowing a largeinteraction rate $|\Gamma| \sim H_0$. However, as has been known for a while,the BAO data break this degeneracy. Moreover, we exploit the CMB lensingpotential likelihood, which probes the matter perturbations at redshift $z \sim2$ and is very sensitive to the growth of structure, and hence one of the toolsfor discerning between the $\Lambda$CDM model and its alternatives. However, wefind that in the non-phantom models ($w_{\mathrm{de}}>-1$), the constraintsremain unchanged by the inclusion of the lensing data and consistent with zerointeraction, $-0.14 < \Gamma/H_0 < 0.02$ at 95\% CL. On the contrary, in thephantom models ($w_{\mathrm{de}}<-1$), energy transfer from dark energy to darkmatter is moderately favoured over the non-interacting model; $-0.57 <\Gamma/H_0 < -0.10$ at 95\% CL with CMB+BAO, while addition of the lensing datashifts this to $-0.46 < \Gamma/H_0 < -0.01$.

Distinguishing interacting dark energy from wCDM with CMB, lensing, and baryon acoustic oscillation data