The properties of the dark matter halo distribution in non-Gaussian scenarios

Details The properties of the dark matter halo distribution in non-Gaussian scenarios The properties of the dark matter halo distribution in non-Gaussian scenarios

Oct 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009nuphs.194...22c&link_type=abstract

Nuclear Physics B Proceedings Supplements, Volume 194, p. 22-27.

Physics

Nuclear Physics

1

Scientific paper

The description of halo abundance and clustering for non-Gaussian initial conditions has recently received renewed interest, motivated by the forthcoming large galaxy and cluster surveys, which can potentially detect primordial non-Gaussianity of the local form with a non-Gaussianity parameter |f| of order unity. This is particularly exciting because, while the simplest single-field slow-roll models of inflation predict a primordial |f|≪1, this signal sources extra contributions to the effective f of large-scale structures that are expected to be above the predicted detection threshold [C. Carbone, L. Verde, and S. Matarrese, ApJL 684 (2008) L1]. We present tests on N-body simulations of analytical formulae describing the halo abundance and clustering for non-Gaussian initial conditions. In particular, when we calibrate the analytic non-Gaussian mass function of [S. Matarrese, L. Verde, L. and R. Jimenez, ApJL 541 (2000) 10] and [M. LoVerde, A. Miller, S. Shandera and L. Verde, JCAP 04 (2008) 014] and the analytic description of halo clustering for non-Gaussian initial conditions on N-body simulations, we find excellent agreement between the simulations and the analytic predictions if we make the substitutions δ→δ×q and δ→δ×q where q≃0.75, in the density threshold for gravitational collapse and in the non-Gaussian fractional correction to the halo bias, respectively. We discuss the implications of these corrections on present and forecasted primordial non-Gaussianity constraints. We confirm that the non-Gaussian halo bias offers a robust and highly competitive test of primordial non-Gaussianity.

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