Cosmology and dark energy from joint gravitational wave-GRB observations

Belgacem, Enis; Dirian, Yves; Foffa, Stefano; Howell, E. J.; Maggiore, Michele; Regimbau, T.

doi:10.1088/1475-7516/2019/08/015

Cited by 118 publications

(224 citation statements)

References 119 publications

(343 reference statements)

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“…Combining the errors on Ξ 0 from each of the 169 events in Table 5 (taking into account the number of events per bin) we get an overall error ∆Ξ 0 0.7%. This agrees with the result obtained in [203], using the full catalogs corresponding to 10 yr of data, and performing a MCMC to take into account more precisely the degeneracies with H 0 , Ω M and w 0 (and using, conservatively, the current datasets on CMB, BAO and SNe), where it was found that Ξ 0 can be determined to an accuracy of 1%. Clearly, with respect to the size of the deviation of Ξ 0 from the GR value, which can be as large as 80%, this is a remarkable precision.…”

Section: G Detectors: Einstein Telescope and Cosmic Explorersupporting

confidence: 87%

“…We next compare the predictions for modified GW propagation of the RT model with the sensitivities of current and future GW detectors, elaborating on the analysis in [115,165,203,204] for ground-based detectors and in [191] Table 6. The events in a given realization of the mock catalog of joint GW-GRB detections for the HLVKI network, over 10 yr of simulated data.…”

Section: Comparison With the Sensitivity Of Current And Future Gw Detmentioning

confidence: 99%

“…The 'measured' luminosity distance is obtained from the redshift assuming ΛCDM as fiducial model, and scattering randomly the fiducial values of d gw L (z) according to a Gaussian distribution with a width equal to the error ∆d gw L (z) (from ref. [203]). In the last column we give the corresponding error on the measurement of δ(0) from each single source, assuming a 1% error on the electromagnetic luminosity distance.…”

Section: Comparison With the Sensitivity Of Current And Future Gw Detmentioning

confidence: 99%

“…However, since the peak of the Table 7. Number of event and mean value of the observational error ∆d gw L /d gw L in different redshift bins, for a specific realization of the catalog of joint GW-GRB detections, assuming 10 yr of data (from [203]). In the last column we give an estimate of the error on Ξ 0 from an individual source in the given frequency bin.…”

Section: G Detectors: Einstein Telescope and Cosmic Explorermentioning

confidence: 99%

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Gravity in the infrared and effective nonlocal models

Belgacem

Dirian

Finke

et al. 2020

J. Cosmol. Astropart. Phys.

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We provide a systematic and updated discussion of a research line carried out by our group over the last few years, in which gravity is modified at cosmological distances by the introduction of nonlocal terms, assumed to emerge at an effective level from the infrared behavior of the quantum theory. The requirement of producing a viable cosmology turns out to be very stringent and basically selects a unique model, in which the nonlocal term describes an effective mass for the conformal mode. We discuss how such a specific structure could emerge from a fundamental local theory of gravity, and we perform a detailed comparison of this model with the most recent cosmological datasets, confirming that it fits current data at the same level as ΛCDM.Most notably, the model has striking predictions in the sector of tensor perturbations, leading to a very large effect in the propagation of gravitational wave (GWs) over cosmological distances. At the redshifts relevant for the next generation of GW detectors such as Einstein Telescope, Cosmic Explorer and LISA, this leads to deviations from GR that could be as large as 80%, and could be verified with the detection of just a single coalescing binary with electromagnetic counterpart. This would also have potentially important consequences for the search of the counterpart since, for a given luminosity distance to the source, as inferred through the GW signal, the actual source redshift could be significantly different from that predicted by ΛCDM. At the redshifts relevant for advanced LIGO/Virgo/Kagra the effect is smaller, but still potentially observable over a few years of runs at target sensitivity. arXiv:2001.07619v1 [astro-ph.CO] 21 Jan 2020 4 Conclusions 66 A Difficulties of alternative nonlocal models 68 -1 -2 The Lichnerowicz operator is defined by E µν,ρσ ≡ 1 2, where 2 = η µν ∂µ∂ν is the flat-space d'Alembertian. We use the signature ηµν = (−, +, +, +) and MTW [14] sign conventions. 3 We assume here 3 + 1 spacetime dimensions. See [13] for the corresponding equations in d + 1 spacetime dimensions, with d generic.

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Section: G Detectors: Einstein Telescope and Cosmic Explorersupporting

confidence: 87%

Section: Comparison With the Sensitivity Of Current And Future Gw Detmentioning

confidence: 99%

Section: Comparison With the Sensitivity Of Current And Future Gw Detmentioning

confidence: 99%

Section: G Detectors: Einstein Telescope and Cosmic Explorermentioning

confidence: 99%

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Gravity in the infrared and effective nonlocal models

Belgacem

Dirian

Finke

et al. 2020

J. Cosmol. Astropart. Phys.

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“…The corresponding detection rates will be impressive, of order 10 5 − 10 6 BH-BH and 7 × 10 4 NS-NS coalescences per year for a single detector such as ET [27][28][29]; depending on the network of electromagnetic facilities operating at the time of 3G detectors, over a few years one might collect O(10 2 − 10 3 ) NS-NS GW events with observed electromagnetic counterpart [29]. The signal-to-noise ratio of many of these events will be huge.…”

mentioning

confidence: 99%

Science case for the Einstein telescope

Maggiore

Broeck

Bartolo

et al. 2020

J. Cosmol. Astropart. Phys.

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The Einstein Telescope (ET), a proposed European ground-based gravitationalwave detector of third-generation, is an evolution of second-generation detectors such as Advanced LIGO, Advanced Virgo, and KAGRA which could be operating in the mid 2030s. ET will explore the universe with gravitational waves up to cosmological distances. We discuss its main scientific objectives and its potential for discoveries in astrophysics, cosmology and fundamental physics. 1 1 Prepared for submission to the ESFRI Roadmap, on behalf of the ET steering committee.

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