We present the first hydrodynamic N-body simulations of primordial gas clouds responsible for the reionization process in dark energy cosmologies. We compare the cosmological constant scenario with a SUGRA quintessence model with marked dynamics in order to highlight effects due to the different acceleration histories imposed by the dark energy. We show that both the number density of gas clouds and their clumpiness keep a record of the expansion rate during evolution, similar to the non-linear dark matter profile at virialization, as was recently demonstrated by Dolag et al. Varying the shape of the primordial power spectrum, we show how this effect is mitigated by a running spectral index decreasing the power at small scales. Our results demonstrate that, in order to constrain the dark energy from large-scale structures, one must track its effects down to the distribution of luminous matter.

Early structure formation in quintessence models and its implications for cosmic reionisation from first stars / Maio, U.; Dolag, K.; Meneghetti, M.; Moscardini, L.; Yoshida, N.; Baccigalupi, C.; Bartelmann, M.; Perrotta, F.. - In: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. - ISSN 0035-8711. - 373:2(2006), pp. 869-878. [10.1111/j.1365-2966.2006.11090.x]

Early structure formation in quintessence models and its implications for cosmic reionisation from first stars

Baccigalupi, C.;Perrotta, F.
2006-01-01

Abstract

We present the first hydrodynamic N-body simulations of primordial gas clouds responsible for the reionization process in dark energy cosmologies. We compare the cosmological constant scenario with a SUGRA quintessence model with marked dynamics in order to highlight effects due to the different acceleration histories imposed by the dark energy. We show that both the number density of gas clouds and their clumpiness keep a record of the expansion rate during evolution, similar to the non-linear dark matter profile at virialization, as was recently demonstrated by Dolag et al. Varying the shape of the primordial power spectrum, we show how this effect is mitigated by a running spectral index decreasing the power at small scales. Our results demonstrate that, in order to constrain the dark energy from large-scale structures, one must track its effects down to the distribution of luminous matter.
2006
373
2
869
878
https://doi.org/10.1111/j.1365-2966.2006.11090.x
https://arxiv.org/abs/astro-ph/0607409
Maio, U.; Dolag, K.; Meneghetti, M.; Moscardini, L.; Yoshida, N.; Baccigalupi, C.; Bartelmann, M.; Perrotta, F.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/20.500.11767/17304
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