Primordial Stochastic Gravitational Wave Background Anisotropies: in-in Formalization and Applications

Abstract

Primordial non-Gaussianities of the scalar(tensor)-tensor-tensor type supporting a non-trivial squeezed component are known to induce anisotropies in the stochastic gravitational wave background. We derive the explicit form of such anisotropies by making use, for the first time in this context, of the in-in formalism for cosmological correlation functions. After illustrating the general method and using it for the minimal single-field slow-roll case, we apply it to multi-field models, providing both a tree-level and a one-loop example. First, we make contact with previous results on anisotropies due to the presence of an extra spin-2 field during inflation. Secondly, we calculate the 1-loop scalar-tensor-tensor three-point function in the context of so-called supersolid inflation. The corresponding gravitational wave anisotropy is induced atop a gravitational signal that may be sufficiently large for detection.

v2: 35 pages, 5 figures, minor modifications, version published in JCAP

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Cited by in corpus (8)

• Stochastic gravitational wave background phenomenology in a pulsar timing array
• Enhancing gravitational wave anisotropies with peaked scalar sources
• No time to derive: unraveling total time derivatives in in-in perturbation theory
• Gravitational waves in ultra-slow-roll and their anisotropy at two loops
• Probing parity-odd bispectra with anisotropies of GW $V$ modes
• On the response of the Einstein Telescope to Doppler anisotropies
• Antipodal Angular Correlations of Inflationary Stochastic Gravitational Wave Background
• Stochastic gravitational wave background anisotropies from inflation with non-Bunch-Davies states