Estimates of maximum energy density of cosmological gravitational-wave backgrounds

Giblin, John T.; Thrane, E.

doi:10.1103/physrevd.90.107502

Cited by 47 publications

(43 citation statements)

References 44 publications

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“…These include unresolved compact binary coalescences of both black holes and neutron stars [1][2][3][4][5], rotating neutron stars [6][7][8], supernovae [9][10][11][12], cosmic strings [13][14][15][16], inflationary models [17][18][19][20][21][22][23][24], phase transitions [25][26][27], and the pre-Big Bang scenario [28][29][30][31]. The variety of mechanisms potentially contributing to the background provides the opportunity to study a number of different environments within the Universe.…”

mentioning

confidence: 99%

Upper Limits on the Stochastic Gravitational-Wave Background from Advanced LIGO’s First Observing Run

Abbott¹,

Abbott²,

Abbott³

et al. 2017

Phys. Rev. Lett.

247

268

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A wide variety of astrophysical and cosmological sources are expected to contribute to a stochastic gravitational-wave background. Following the observations of GW150914 and GW151226, the rate and mass of coalescing binary black holes appear to be greater than many previous expectations. As a result, the stochastic background from unresolved compact binary coalescences is expected to be particularly loud. We perform a search for the isotropic stochastic gravitational-wave background using data from Advanced LIGO's first observing run. The data display no evidence of a stochastic gravitational-wave signal. We constrain the dimensionless energy density of gravitational waves to be Ω0 < 1.7 × 10 −7 with 95% confidence, assuming a flat energy density spectrum in the most sensitive part of the LIGO band (20 − 86 Hz). This is a factor of ∼33 times more sensitive than previous measurements. We also constrain arbitrary power-law spectra. Finally, we investigate the implications of this search for the background of binary black holes using an astrophysical model for the background. The recent detections of binary black hole (BBH) coalescences by Advanced LIGO [32,33] suggest that the Universe may be rich with coalescing BBHs. While events like GW150914 and GW151226 are loud enough to be clearly detected, we expect there to be many more events that are too far away to be individually resolved and that contribute to the background. Since this BBH population originates from sources that are too distant to be individually detected, the stochastic search probes a distinct population of binaries compared to nearby sources [34]. The background from these binaries provides complementary information to individually resolved binary coalescences [35].In this Letter, we report on the search for an isotropic background using data from Advanced LIGO's first observing run O1. We search for the background by crosscorrelating data streams from the two separate LIGO detectors and looking for a coherent signal. We find no evidence for the background and place the best upper limits to date on the energy density of the background in the LIGO frequency band. We also update the impli-

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confidence: 99%

Upper Limits on the Stochastic Gravitational-Wave Background from Advanced LIGO’s First Observing Run

Abbott¹,

Abbott²,

Abbott³

et al. 2017

Phys. Rev. Lett.

247

268

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“…By approximating the source as a Gaussian of width σ peaked at wavenumber k * , Ref. [123] estimates the peak amplitude as…”

Section: A Efficiency Of Preheatingmentioning

confidence: 99%

Constraining axion inflation with gravitational waves from preheating

et al. 2020

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We study gravitational wave production from gauge preheating in a variety of inflationary models, detailing its dependence on both the energy scale and the shape of the potential. We show that gauge preheating generically leads to a large gravitational wave background that contributes significantly to the effective number of relativistic degrees of freedom in the early Universe, N eff . We demonstrate that the efficiency of gravitational wave production is correlated with the tensor-to-scalar ratio, r.In particular, we show that efficient gauge preheating in models whose tensor-to-scalar ratio would be detected by next-generation cosmic microwave background experiments (r 10 −3 ) will either be detected through its contribution to N eff or ruled out. Furthermore, we show that bounds on N eff provide the most sensitive probe of the possible axial coupling of the inflaton to gauge fields regardless of the potential.

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“…Astrophysical sources are reviewed in [4]. Cosmological sources of the SGWB include cosmic string networks [5][6][7][8], inflation [9][10][11][12][13][14][15][16], phase transitions [17][18][19], and the pre-Big-Bang scenario [20][21][22][23]. For reviews of search methods for the SGWB, see [24,25].…”

Section: Introductionmentioning

confidence: 99%

Identification and mitigation of narrow spectral artifacts that degrade searches for persistent gravitational waves in the first two observing runs of Advanced LIGO

Covas¹,

Effler²,

Goetz³

et al. 2018

Phys. Rev. D

138

157

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Searches are under way in Advanced LIGO and Virgo data for persistent gravitational waves from continuous sources, e.g. rapidly rotating galactic neutron stars, and stochastic sources, e.g. relic gravitational waves from the Big Bang or superposition of distant astrophysical events such as mergers of black holes or neutron stars. These searches can be degraded by the presence of narrow spectral artifacts (lines) due to instrumental or environmental disturbances. We describe a variety of methods used for finding, identifying and mitigating these artifacts, illustrated with particular examples. Results are provided in the form of lists of line artifacts that can safely be treated as non-astrophysical. Such lists are used to improve the efficiencies and sensitivities of continuous and stochastic gravitational wave searches by allowing vetoes of false outliers and permitting data cleaning.

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Estimates of maximum energy density of cosmological gravitational-wave backgrounds

Cited by 47 publications

References 44 publications

Upper Limits on the Stochastic Gravitational-Wave Background from Advanced LIGO’s First Observing Run

Upper Limits on the Stochastic Gravitational-Wave Background from Advanced LIGO’s First Observing Run

Constraining axion inflation with gravitational waves from preheating

Identification and mitigation of narrow spectral artifacts that degrade searches for persistent gravitational waves in the first two observing runs of Advanced LIGO

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