http://arxiv.org/abs/1701.03375
The squeezed-limit bispectrum, which is generated by nonlinear gravitational evolution as well as inflationary physics, measures the correlation of three wavenumbers, in the configuration where one wavenumber is much smaller than the other two. Since the squeezed-limit bispectrum encodes the impact of a large-scale fluctuation on the small-scale power spectrum, it can be understood as how the small-scale power spectrum “responds” to the large-scale fluctuation. Viewed in this way, the squeezed-limit bispectrum can be calculated using the response approach even in the cases which do not submit to perturbative treatment. To illustrate this point, we apply this approach to the cross-correlation between the large-scale quasar density field and small-scale Lyman-$\alpha$ forest flux power spectrum. In particular, using separate universe simulations which implement changes in the large-scale density, velocity gradient, and primordial power spectrum amplitude, we measure how the Lyman-$\alpha$ forest flux power spectrum responds to the local, long-wavelength quasar overdensity, and equivalently their squeezed-limit bispectrum. We perform a Fisher forecast for the ability of future experiments to constrain local non-Gaussianity using the bispectrum of quasars and the Lyman-$\alpha$ forest. Combining with quasar and Lyman-$\alpha$ forest power spectra to constrain the biases, we find that for DESI the expected $1-\sigma$ constraint is ${\rm err}[f_{\rm NL}]\sim60$. Ability for DESI to measure $f_{\rm NL}$ through this channel is limited primarily by the aliasing and instrumental noise of the Lyman-$\alpha$ forest flux power spectrum. The combination of response approach and separate universe simulations provides a novel technique to explore the constraints from the squeezed-limit bispectrum between different observables.
C. Chiang, A. Cieplak, F. Schmidt, et. al.
Fri, 13 Jan 17
4/44
Comments: 19 pages, 3 figures
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