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tokens: we take the average over contributions from all pairs of cells (and the third associated cell that is uniquely determined by the triangular condition) that fall into that bin. We do not look at the bispectrum bins unless at least some combination of the wave numbers in that bin satisfies a triangular condition. To avoid counting equivalent triplets multiple times, we impose a condition k 1 > k 2 > k 3 . Fig. A1 shows the average nonlinear and linear power spectra of matter particles from Quijote simulations. We rescaled the linear power spectrum to have a matching amplitude at small wave numbers. The two are reasonably close for large-scale modes (up to k ∼ 0.1 h Mpc −1 after which the additional power in the nonlinear power spectrum becomes visible. The partial erasure of the BAO signal is also visible by eye. Fig. A2 shows the average bispectrum of matter particles from Quijote simulations at z = 0 as a function of the longest wave number. Features in the shape of this three-dimensional function provide additional opportunities for the standard ruler test. Figure A1. Non-linear power spectrum at z = 0 (blue) and a linear power spectrum (black) of Quijote matter particles. The linear power spectrum is measured from particles at z = 99 and rescaled to have a matching amplitude on large scales. Figure A2. Bispectrum of Quijote matter particles at z = 0 as a function of the largest wave number k 1 . Multiple points at the same abscissa show all bispectrum bins that share that value of k 1 but have different values of k 2 and k 3 . We multiply the bispectrum by a factor of k 1 k 2 k 3 . This factor is proportional to the number of fundamental triangles in the bin and separates different points for better visibility. To estimate the covariance of these measurements, , by computing the sample covariance over 8,000 Quijote simulations, X i l are the power spectrum and bispectrum measurements, where the first index goes over the bins and the second index goes over simulations. N sim is the number of simulations. Fig. A3 shows the correlation matrix of these measurements defined as We ordered the measurements so that the first 50 elements are binned P ( k ) up to k max = 0.5 h Mpc −1 . They are followed by binned B ( k 1 , k 2 , k 3 ) arranged in such a way that the bispectrum bin with smaller k 1 goes first (smaller k 2 when k 1 are equal, and smaller k 3 when both k 1 and k 2 are equal). The first 150 bins arranged in this way accommodate all bispectra up to k 1, max = 0.1 h Mpc −1 . The correlation between power spectra at high wave numbers is clearly visible in this plot. The bispectrum measurements are also correlated between themselves and the power spectra but to a lesser extent. Figure A3. Correlation coefficient of the power spectrum (first 50 bins, goes up to k max = 0.5 h Mpc −1 ) and the bispectrum (last 150 bins, goes up to k 1, max = 0.1 h Mpc −1 ) measurements. Colourmap is adjusted in such a way that red, blue, and white cells