期刊
PHYSICAL REVIEW D
卷 99, 期 4, 页码 -出版社
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevD.99.043536
关键词
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资金
- U.S. Department of Energy [DE-FG02-13ER41958]
- NASA ATP [NNX15AK22G]
- Simons Foundation
- Kavli Institute for Cosmological Physics at the University of Chicago [NSF PHY-1125897]
- Kavli Foundation
- Japan Society for the Promotion of Science (JSPS) [JP17H06359, JP18K13565]
- NASA [NNX15AK22G, 806105] Funding Source: Federal RePORTER
Primordial black holes (PBHs) cannot be produced abundantly enough to be the dark matter in canonical single-field inflation under slow roll. This conclusion is robust to local non-Gaussian correlations between long-and short-wavelength curvature modes, which we show have no effect in slow roll on local primordial black hole abundances. For the prototypical model which evades this no-go, ultra-slow roll (USR), these squeezed non-Gaussian correlations have at most an order-unity effect on the variance of PBH-producing curvature fluctuations for models that would otherwise fail to form sufficient PBHs. Moreover, the transition out of USR, which is necessary for a successful model, suppresses even this small enhancement unless it causes a large increase in the inflaton kinetic energy in a fraction of an e-fold, which we call a large and fast transition. Along the way we apply the in-in formalism, the delta N formalism, and gauge transformations to compute non-Gaussianities and illuminate different aspects of the physical origin of these results. Local non-Gaussianity in the squeezed limit does not weaken the Gaussian conclusion that PBHs as dark matter in canonical single-field inflation require a complicated and fine-tuned potential shape with an epoch where slow roll is transiently violated.
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