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Hemispherical anomaly from asymmetric initial states
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy.
KTH Royal Inst Technol, Nordita, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden.;Stockholm Univ, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden..
2016 (English)In: PHYSICAL REVIEW D, ISSN 2470-0010, Vol. 94, no 4, 043009Article in journal (Refereed) Published
Abstract [en]

We investigate if the hemispherical asymmetry in the CMB is produced from "asymmetric" excited initial conditions. We show that in the limit where the deviations from the Bunch-Davies vacuum are large and the scale of new physics is maximally separated from the inflationary Hubble parameter, the primordial power spectrum is modulated only by position-dependent dipole and quadrupole terms. Requiring the dipole contribution in the power spectrum to account for the observed power asymmetry, A = 0.07 +/- 0.022, we show that the amount of quadrupole terms is roughly equal to A(2). The mean local bispectrum, which gets enhanced for the excited initial state, is within the 1 sigma bound of Planck 2015 results for a large field model, f(NL) similar or equal to 4.17, but is reachable by future CMB experiments. The amplitude of the local non-Gaussianity modulates around this mean value, depending on the angle that the correlated patches on the 2d CMB surface make with the preferred direction. The amount of variation is minimized for the configuration in which the short and long wavelength modes are around the preferred pole and vertical bar(k(3)) over right arrow vertical bar approximate to vertical bar(k) over right arrow (l approximate to 10)vertical bar << vertical bar(k(1)) over right arrow vertical bar approximate to vertical bar(k(2)) over right arrow vertical bar approximate to vertical bar(k) over right arrow (l approximate to 2500)vertical bar with f(NL)(min) approximate to 3.64. The maximum occurs when these modes are at the antipode of the preferred pole, f(NL)(max) approximate to 4.81. The difference of non-Gaussianity between these two configurations is as large as similar or equal to 1.17, which can be used to distinguish this scenario from other scenarios that try to explain the observed hemispherical asymmetry.

Place, publisher, year, edition, pages
2016. Vol. 94, no 4, 043009
National Category
Astronomy, Astrophysics and Cosmology
URN: urn:nbn:se:uu:diva-305563DOI: 10.1103/PhysRevD.94.043009ISI: 000383048000001OAI: oai:DiVA.org:uu-305563DiVA: diva2:1038833
Available from: 2016-10-20 Created: 2016-10-19 Last updated: 2016-10-20Bibliographically approved

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