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A detection of excess cosmic microwave background (CMB) B-mode polarizationon large scales allows the possibility of measuring not only the amplitude ofthese fluctuations but also their scale dependence, which can be parametrizedas the tensor tilt $n_T$. Measurements of this scale dependence will behindered by the secondary B-mode polarization anisotropy induced bygravitational lensing. Fortunately, these contaminating B modes can beestimated and removed with a sufficiently good estimate of the interveninggravitational potential and a good map of CMB E-mode polarization. We presentforecasts for how well these gravitational lensing B modes can be removed,assuming that the lensing potential can be estimated either internally from CMBdata or using maps of the cosmic infrared background (CIB) as a tracer. We findthat CIB maps are as effective as CMB maps for delensing at the noise levels ofthe current generation of CMB experiments, while the CMB maps themselves willultimately be best for delensing at polarization noise below $\Delta_P$=1$\mu$K-arcmin. At this sensitivity level, CMB delensing will be able to measure$n_T$ to an accuracy of 0.02 or better, which corresponds to the tensor tiltpredicted by the consistency relation for single-field slow-roll models ofinflation with $r=0.2$. However, CIB-based delensing will not be sufficient forconstraining $n_T$ in simple inflationary models.

Prospects for Delensing the Cosmic Microwave Background for Studying Inflation