Reconstructing the spectral shape of a stochastic gravitational wave background with LISA

Caprini, Chiara; Figueroa, Daniel G.; Flauger, Raphael; Nardini, Germano; Peloso, Marco; Pieroni, Mauro; Ricciardone, Angelo; Tasinato, Gianmassimo

doi:10.1088/1475-7516/2019/11/017

Cited by 240 publications

(316 citation statements)

References 154 publications

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“…To calculate the SNR for different reheating temperature T R , we used the strain sensitivity S n (f ) of a single channel of the LISA detector given in Eq. (2.4) in Caprini et al [93].…”

Section: Detection Of the Generated Gw Spectrum With The Lisamentioning

confidence: 88%

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Generation of helical magnetic field in a viable scenario of inflationary magnetogenesis

2018

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Generation of magnetic fields during inflation is a promising mechanism for the origin of the observed large scale magnetic fields in the universe. Among several attempts, a popular model is one where the inflaton and the electromagnetic field are coupled through a coupling function f leading to a term in the Lagrangian density of the form, f 2 F µν Fµν . A number of potential difficulties with such models have been raised in the literature. In our earlier work, we have suggested viable models of inflationary magnetogenesis which avoid these problems and at the same time can lead to either nonhelical or helical magnetic fields of astrophysical interest. Our models require a low energy scale for inflation and reheating (reheating temperature, TR < 10 4 GeV) and generate a blue spectrum of electromagnetic (EM) field which peaks around the horizon scale of reheating. We show here that the anisotropic stress associated with these EM fields naturally source the production of a stochastic background of Gravitational waves (GW) with frequencies in the range of tens of nano Hertz to milli Hertz. These two extremes of the range can be probed respectively by pulsar timing arrays (PTA) experiments and the upcoming Laser Interferometric Space Array (LISA). The peak value of the GW spectrum energy represented by dΩGW /d ln k is 10 −6 for the models which lead to nonhelical primordial fields and 2 × 10 −6 for the helical case for TR = 100 GeV. In this case the spectrum peaks at a frequency 30µHz for non helical case and at 40µHz for helical case. These values are obtained when the ratio of EM energy density to the cosmological density at reheating ∼ 1 and decrease approximately as 2 for smaller values. The amplitude is similar for a lower value of TR, but the frequency at which the GW spectrum peaks decreases as TR. The gravitational waves generated are unpolarized if the EM fields are nonhelical but are circularly polarised for helical primordial fields. If detected in future these gravitational waves will provide a unique probe of such models of inflationary magnetogenesis. * ramkishor@iucaa.in † kandu@iucaa.in ‡ trs@physics.du.ac.in

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“…To calculate the SNR for different reheating temperature T R , we used the strain sensitivity S n (f ) of a single channel of the LISA detector given in Eq. (2.4) in Caprini et al [93].…”

Section: Detection Of the Generated Gw Spectrum With The Lisamentioning

confidence: 88%

“…We now discuss the prospects of detection of the GW spectrum generated in our model with the LISA. For this, we calculate the signal to noise ratio (SNR) using the following definition [93],…”

Section: Detection Of the Generated Gw Spectrum With The Lisamentioning

confidence: 99%

Generation of helical magnetic field in a viable scenario of inflationary magnetogenesis

2018

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“…The strongest astrophysical background in the frequency region of terrestrial detectors is expected to be due to the coalescence of binary black holes and binary neutron star systems. To separate the cosmological and the astrophysical backgrounds the first step will be to use any distinct spectral dependence of the average (monopole) amplitude Ω GW [228]. However, the better angular resolution of 3G detectors will most probably allow to spot the anisotropies (directionality dependence) of the astrophysical background.…”

Section: Astrophysical Backgroundsmentioning

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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“…The previous expression is time-translationally invariant, since it depends only on the time difference (t 2 − t 1 ) appearing in the exponential term of eq (6).…”

Section: Characterization Of a Stationary Non-gaussian Sgwbmentioning

confidence: 99%

Probing a stationary non-Gaussian background of stochastic gravitational waves with pulsar timing arrays

Powell

Tasinato

2020

J. Cosmol. Astropart. Phys.

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We introduce the concept of stationary graviton non-Gaussianity (nG), an observable that can be probed in terms of 3-point correlation functions of a stochastic gravitational wave (GW) background. When evaluated in momentum space, stationary nG corresponds to folded bispectra of graviton nG. We determine 3-point overlap functions for testing stationary nG with pulsar timing array GW experiments, and we obtain the corresponding optimal signal-tonoise ratio. For the first time, we consider 3-point overlap functions including scalar graviton polarizations (which can be motivated in theories of modified gravity); moreover, we also calculate 3-point overlap functions for correlating pulsar timing array with ground based GW detectors. The value of the optimal signal-to-noise ratio depends on the number and position of monitored pulsars. We build geometrical quantities characterizing how such ratio depends on the pulsar system under consideration, and we evaluate these geometrical parameters using data from the IPTA collaboration. We quantitatively show how monitoring a large number of pulsars can increase the signal-to-noise ratio associated with measurements of stationary graviton nG. arXiv:1910.04758v1 [gr-qc]

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Reconstructing the spectral shape of a stochastic gravitational wave background with LISA

Cited by 240 publications

References 154 publications

Generation of helical magnetic field in a viable scenario of inflationary magnetogenesis

Generation of helical magnetic field in a viable scenario of inflationary magnetogenesis

Science case for the Einstein telescope

Probing a stationary non-Gaussian background of stochastic gravitational waves with pulsar timing arrays

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