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Integrated Sachs-Wolfe effect in massive bigravity

We study the integrated Sachs-Wolfe (ISW) effect in ghost-free, massive bigravity. We focus on the infinite-branch bigravity (IBB) model which exhibits viable cosmic expansion histories and stable linear perturbations, while the cosmological constant is set to zero and the late-time accelerated expa...

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Bibliographic Details
Main Authors: Enander, Jonas (Author) , Akrami, Yashar (Author) , Mörtsell, Edvard (Author) , Renneby, Malin (Author) , Solomon, Adam R. (Author)
Format: Article (Journal)
Language:English
Published: 20 April 2015
In: Physical review. D, Particles, fields, gravitation, and cosmology
Year: 2015, Volume: 91, Issue: 8
ISSN:1550-2368
DOI:10.1103/PhysRevD.91.084046
Online Access:Verlag, lizenzpflichtig, Volltext: https://doi.org/10.1103/PhysRevD.91.084046
Verlag, lizenzpflichtig, Volltext: https://link.aps.org/doi/10.1103/PhysRevD.91.084046
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Author Notes:Jonas Enander, Yashar Akrami, Edvard Mörtsell, Malin Renneby, and Adam R. Solomon
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Summary:We study the integrated Sachs-Wolfe (ISW) effect in ghost-free, massive bigravity. We focus on the infinite-branch bigravity (IBB) model which exhibits viable cosmic expansion histories and stable linear perturbations, while the cosmological constant is set to zero and the late-time accelerated expansion of the Universe is due solely to the gravitational interaction terms. The ISW contribution to the CMB auto-correlation power spectrum is predicted, as well as the cross-correlation between the CMB temperature anisotropies and large-scale structure. We use ISW amplitudes as inferred from the WMAP 9-year temperature data together with galaxy and AGN data provided by the WISE mission in order to compare the theoretical predictions to the observations. The ISW amplitudes in IBB are found to be larger than the corresponding ones in the standard ΛCDM model by roughly a factor of 1.5, but are still consistent with the observations.
Item Description:Gesehen am 13.07.2020
Physical Description:Online Resource
ISSN:1550-2368
DOI:10.1103/PhysRevD.91.084046

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