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@ARTICLE{Bartolo:405621,
      author       = {Bartolo, Nicola and Domcke, Valerie and Figueroa, Daniel G.
                      and Garcia-Bellido, Juan and Peloso, Marco and Pieroni,
                      Mauro and Ricciardone, Angelo and Sakellariadou, Mairi and
                      Sorbo, Lorenzo and Tasinato, Gianmassimo},
      title        = {{P}robing non-{G}aussian {S}tochastic {G}ravitational
                      {W}ave {B}ackgrounds with {LISA}},
      reportid     = {PUBDB-2018-02233, DESY-18-086. CERN-TH-2018-130.
                      UMN-TH-3720-18. IFT-UAM-CSIC-18-58. KCL-PH-TH-2018-22.
                      ACFI-T18-08. arXiv:1806.02819},
      year         = {2018},
      abstract     = {The stochastic gravitational wave background (SGWB)
                      contains a wealth of information on astrophysical and
                      cosmological processes. A major challenge of upcoming years
                      will be to extract the information contained in this
                      background and to disentangle the contributions of different
                      sources. In this paper we provide the formalism to extract,
                      from the correlation of three signals in the Laser
                      Interferometer Space Antenna (LISA), information about the
                      tensor three-point function, which characterizes the
                      non-Gaussian properties of the SGWB. Compared to the
                      two-point function, the SGWB three-point function has a
                      richer dependence on the gravitational wave momenta and
                      chiralities, and a larger number of signal channels. It can
                      be used therefore as a powerful discriminator between
                      different models. We provide LISA's response functions to a
                      general SGWB three-point function. As examples, we study in
                      full detail the cases of an equilateral and squeezed SGWB
                      bispectra, and provide the explicit form of the response
                      functions, ready to be convoluted with any theoretical
                      prediction of the bispectrum to obtain the observable
                      signal. We further derive the optimal estimator to compute
                      the signal-to-noise ratio. Our formalism covers general
                      shapes of non-Gaussianity, and can be extended straightaway
                      to other detector geometries. Finally, we provide a short
                      overview of models of the early universe that can give rise
                      to non-Gaussian SGWB.},
      cin          = {T},
      cid          = {I:(DE-H253)T-20120731},
      pnm          = {611 - Fundamental Particles and Forces (POF3-611)},
      pid          = {G:(DE-HGF)POF3-611},
      experiment   = {EXP:(DE-MLZ)NOSPEC-20140101},
      typ          = {PUB:(DE-HGF)25 / PUB:(DE-HGF)29},
      eprint       = {1806.02819},
      howpublished = {arXiv:1806.02819},
      archivePrefix = {arXiv},
      SLACcitation = {$\%\%CITATION$ = $arXiv:1806.02819;\%\%$},
      doi          = {10.3204/PUBDB-2018-02233},
      url          = {https://bib-pubdb1.desy.de/record/405621},
}