Primordial non-Gaussianity with Angular correlation function: Integral constraint and validation for DES

Abstract

Local primordial non-Gaussianity (PNG) is a promising observable of the underlying physics of inflation, characterised by $f_{\mathrm{NL}}^{\mathrm{loc}}$. We present the methodology to measure $f_{\mathrm{NL}}^{\mathrm{loc}}$ from the Dark Energy Survey (DES) data using the 2-point angular correlation function (ACF) with scale-dependent bias. One of the focuses of the work is the integral constraint. This condition appears when estimating the mean number density of galaxies from the data and is key in obtaining unbiased $f_{\mathrm{NL}}^{\mathrm{loc}}$ constraints. The methods are analysed for two types of simulations: $\sim 246$ GOLIAT-PNG N-body small area simulations with $f_{\mathrm{NL}}$ equal to -100 and 100, and 1952 Gaussian ICE-COLA mocks with $f_{\mathrm{NL}}=0$ that follow the DES angular and redshift distribution. We use the ensemble of GOLIAT-PNG mocks to show the importance of the integral constraint when measuring PNG, where we recover the fiducial values of $f_{\mathrm{NL}}$ within the $1\sigma$ when including the integral constraint. In contrast, we found a bias of $\Delta f_{\mathrm{NL}}\sim 100$ when not including it. For a DES-like scenario, we forecast a bias of $\Delta f_{\mathrm{NL}}\sim 23$, equivalent to $1.8\sigma$, when not using the IC for a fiducial value of $f_{\mathrm{NL}}=100$. We use the ICE-COLA mocks to validate our analysis in a realistic DES-like setup finding it robust to different analysis choices: best-fit estimator, the effect of IC, BAO damping, covariance, and scale choices. We forecast a measurement of $f_{\mathrm{NL}}$ within $\sigma (f_{\mathrm{NL}})=31$ when using the DES-Y3 BAO sample, with the ACF in the $1\mathrm{deg}<\theta <20\mathrm{deg}$ range.

Version after MNRAS reviewer comments. Improved discussion in Section 7. 16 pages, 11 figures

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• PNG-UNITsims: Halo clustering response to primordial non-Gaussianities as a function of mass
• Constraining primordial non-Gaussianity by combining next-generation galaxy and 21 cm intensity mapping surveys
• The full-sky Spherical Fourier-Bessel power spectrum in general relativity
• Angular correlation functions of bright Lyman-break galaxies at $3\lesssim \mathbf{z}\lesssim 5$
• Beyond the two-point correlation: constraining primordial non-gaussianity with density perturbation moments