N. Chandrachani Devi, T. Roy Choudhury, Anjan A. Sen
We study the formation of galaxy clusters in the presence of thawing class of
scalar field dark energy. We consider cases where the scalar field has
canonical as well non canonical kinetic term in its action. We also consider
various forms for the potential of the scalar field e.g, linear, quadratic,
inverse quadratic, exponential as well as Pseudo-Nambu-Goldstone Boson (PNGB)
type. Moreover we investigate situation where dark energy is homogeneous as
well as situation where dark energy takes part in the virialization process. We
use the Sheth-Torman formalism while calculating the number density of galaxy
clusters. Our results show that cluster number density for different dark
energy models have significant deviation from the corresponding value for the
\Lambda CDM case. The deviation is more for higher redshifts. Moreover the
tachyon type scalar field with linear potential has the highest deviation from
the \Lambda CDM case. For the total cluster number counts, different dark
energy models can have substantial deviation from \Lambda CDM and this
deviation is most significant around $z \sim 0.5 \sim 1$ for all the models we
considered.
View original:
http://arxiv.org/abs/1112.0728
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