BINGO: A code for the efficient computation of the scalar bi-spectrum

TL;DR

BINGO is a new Fortran code designed for efficient and accurate numerical computation of the scalar bi-spectrum and non-Gaussianity parameter f_{NL} in single field inflation models, accommodating arbitrary wavevector configurations.

Contribution

The paper introduces BINGO, a novel computational tool that accurately calculates the scalar bi-spectrum and f_{NL} for various inflationary scenarios, including deviations from slow roll.

Findings

BINGO accurately reproduces spectral dependence in power law inflation.

The code matches analytical results in slow roll and Starobinsky models.

BINGO can distinguish inflationary models based on non-Gaussianity features.

Abstract

We present a new and accurate Fortran code, the BI-spectra and Non-Gaussianity Operator (BINGO), for the efficient numerical computation of the scalar bi-spectrum and the non-Gaussianity parameter f_{NL} in single field inflationary models involving the canonical scalar field. The code can calculate all the different contributions to the bi-spectrum and the parameter f_{NL} for an arbitrary triangular configuration of the wavevectors. Focusing firstly on the equilateral limit, we illustrate the accuracy of BINGO by comparing the results from the code with the spectral dependence of the bi-spectrum expected in power law inflation. Then, considering an arbitrary triangular configuration, we contrast the numerical results with the analytical expression available in the slow roll limit, for, say, the case of the conventional quadratic potential. Considering a non-trivial scenario involving deviations from slow roll, we compare the results from the code with the analytical results that have recently been obtained in the case of the Starobinsky model in the equilateral limit. As an immediate application, we utilize BINGO to examine of the power of the non-Gaussianity parameter f_{NL} to discriminate between various inflationary models that admit departures from slow roll and lead to similar features in the scalar power spectrum. We close with a summary and discussion on the implications of the results we obtain.