TY - JOUR

T1 - High accuracy Power Spectra at high redshift in Dynamical Dark Energy simulations

AU - Casarini, L.

AU - Macciò, A. V.

AU - Bonometto, S. A.

PY - 2009/10

Y1 - 2009/10

N2 - Accurate predictions on non-linear power spectra, at various redshift z, will be a basic tool to interpret cosmological data from next generation mass probes. We need then high precision simulations, exploring the functional space of w (a) DE state equations, for the admitted cosmological parameter ranges. A procedure was however suggested, making recourse to suitable w = const. auxiliary models, and yielding a ∼1% precision at z = 0. The precision of this procedure, however, worsens at higher z. Here we follow a different criterion for high z. Our N-body gravitational simulations then show that auxiliary w = const. models still meet given w (a) model spectra within 1% at z = 0, but are much better at higher redshift, where they approach a permil precision.

AB - Accurate predictions on non-linear power spectra, at various redshift z, will be a basic tool to interpret cosmological data from next generation mass probes. We need then high precision simulations, exploring the functional space of w (a) DE state equations, for the admitted cosmological parameter ranges. A procedure was however suggested, making recourse to suitable w = const. auxiliary models, and yielding a ∼1% precision at z = 0. The precision of this procedure, however, worsens at higher z. Here we follow a different criterion for high z. Our N-body gravitational simulations then show that auxiliary w = const. models still meet given w (a) model spectra within 1% at z = 0, but are much better at higher redshift, where they approach a permil precision.

UR - http://www.scopus.com/inward/record.url?scp=71149088937&partnerID=8YFLogxK

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U2 - 10.1016/j.nuclphysbps.2009.07.018

DO - 10.1016/j.nuclphysbps.2009.07.018

M3 - Article

AN - SCOPUS:71149088937

VL - 194

SP - 185

EP - 189

JO - Nuclear and Particle Physics Proceedings

JF - Nuclear and Particle Physics Proceedings

SN - 2405-6014

IS - C

ER -