Abstract
Recent studies have shown that the primordial non-Gaussianity affects clustering of dark matter halos through a scale-dependent bias and various constraints on the non-Gaussianity through this scale-dependent bias have been placed. Here we introduce the cross-correlation between the CMB lensing potential and the galaxy angular distribution to effectively extract information about the bias from the galaxy distribution. Then, we estimate the error of non-linear parameter, f_NL, for the on-going CMB experiments and galaxy surveys, such as Planck and Hyper Suprime-Cam (HSC). We found that for the constraint on f_NL with Planck and HSC, the wide field galaxy survey is preferable to the deep one, and the expected error on f_NL can be as small as: \Delta f_NL ~ 20 for b_0 = 2 and \Delta f_NL ~ 10 for b_0 = 4, where b_0 is the linear bias parameter. It is also found that future wide field galaxy survey could achieve \Delta f_NL ~ 5 with CMB prior from Planck if one could observe highly biased objects at higher redshift (z ~ 2).
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