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Pulsar Timing Array Constraints on Primordial Black Holes with NANOGrav 11-Year Data Set
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abstract
The detection of binary black hole coalescences by LIGO/Virgo has aroused the interest in primordial black holes (PBHs), because they could be both the progenitors of these black holes and a compelling candidate of dark matter (DM). PBHs are formed soon after the enhanced scalar perturbations re-enter horizon during radiation dominated era, which would inevitably induce gravitational waves as well. Searching for such scalar induced gravitational waves (SIGWs) provides an elegant way to probe PBHs. We perform the first direct search for the signals of SIGWs accompanying the formation of PBHs in North American Nanohertz Observatory for Gravitational waves (NANOGrav) 11-year data set. No statistically significant detection has been made, and hence we place a stringent upper limit on the abundance of PBHs at $95\%$ confidence level. In particular, less than one part in a million of the total DM mass could come from PBHs in the mass range of $[2 \times 10^{-3}, 7\times 10^{-1}] \Msun$.
Forward citations
Cited by 8 Pith papers
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Observable Gravitational Wave Strain at Second Order
At second order, the gravitational-wave strain measured by geodesic observers exchanging light pulses is the transverse-traceless metric perturbation in the Newton gauge (h_N^(2)).
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Under the FIRAS μ-distortion variance cap, power-law and heavy log-normal PDF tails can yield seed-relevant PBH abundances, while Gaussian and ordinary exponential tails cannot.
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Implications for Pulsar Timing Arrays of Sub-solar Black Hole Detections: From LVK to Einstein Telescope and Cosmic Explorer
A Bayesian analysis shows that a future sub-solar PBH detection would make the primordial SIGW interpretation of PTA data favored over the SMBH interpretation, but this preference is driven by the detection prior.
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On the Gauge Invariance of Secondary Gravitational Waves
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In holographic QCD models, a stronger external magnetic field shifts the gravitational-wave peak from the first-order confinement transition to lower frequencies, with signals potentially visible to IPTA and SKA.
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Pre-Big-Bang Cosmology Cannot Explain NANOGrav 15-year Signal
Pre-Big Bang string cosmology cannot explain the NANOGrav 15-year signal; a power-law spectrum is preferred by a Bayes factor of about 468.
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