Kamionkowski, Marc and Verde, Licia and Jimenez, Raul (2009) The void abundance with non-gaussian primordial perturbations. Journal of Cosmology and Astroparticle Physics, 2009 (01). 010. ISSN 1475-7516. http://resolver.caltech.edu/CaltechAUTHORS:KAMjcap09
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We use a Press-Schechter-like calculation to study how the abundance of voids changes in models with non-Gaussian initial conditions. While a positive skewness increases the cluster abundance, a negative skewness does the same for the void abundance. We determine the dependence of the void abundance on the non-Gaussianity parameter fnl for the local-model bispectrum—which approximates the bispectrum in some multi-field inflation models—and for the equilateral bispectrum, which approximates the bispectrum in single-field slow-roll inflation and in string-inspired DBI models of inflation. We show that the void abundance in large-scale-structure surveys currently being considered should probe values as small as fnl ≾ 10 and fnleq ≾ 30, over distance scales ~ 10 Mpc.
|Additional Information:||© 2009 IOP Publishing Limited and SISSA. Received 2 September 2008, accepted for publication 29 November 2008. Published 8 January 2009. MK thanks Andrew Benson for useful suggestions and the Aspen Center for Physics for hospitality. This work was supported at Caltech by DoE DE-FG03-92-ER40701 and the Gordon and Betty Moore Foundation. LV thanks M. LoVerde for providing the curves of figure 3(a,b) of ref.  in table form. LV is supported by FP7-PEOPLE-2007-4-3 IRG n 202182 and CSIC I3 grant 200750I034. RJ is supported by grants from the Spanish Science Ministry and The European Union (FP7).|
|Group:||TAPIR, Moore Center for Theoretical Cosmology and Physics|
|Subject Keywords:||inflation, physics of the early universe, superclusters and voids, power spectrum|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Archive Administrator|
|Deposited On:||10 Jan 2009 09:46|
|Last Modified:||11 Dec 2016 00:55|
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