Non-linear Structure Formation for Dark Energy Models with a Steep Equation of State. (arXiv:1911.02402v1 [astro-ph.CO])

Non-linear Structure Formation for Dark Energy Models with a Steep Equation of State. (arXiv:1911.02402v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Devi_N/0/1/0/all/0/1">N. Chandrachani Devi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jaber_Bravo_M/0/1/0/all/0/1">M. Jaber-Bravo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aguilar_Arguello_G/0/1/0/all/0/1">G. Aguilar-Arg&#xfc;ello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Valenzuela_O/0/1/0/all/0/1">O. Valenzuela</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Macorra_A/0/1/0/all/0/1">A. de la Macorra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Velazquez_H/0/1/0/all/0/1">H. Vel&#xe1;zquez</a>

We study the nonlinear regime of large scale structure formation considering
a dynamical dark energy (DE) component determined by a Steep Equation of State
parametrization (SEoS) $w(z)=w_0+w_ifrac{(z/z_T)^q}{1+(z/z_T)^q}$. In order to
perform the model exploration at low computational cost, we modified the public
code L-PICOLA. We incorporate the DE model by means of the first and
second-order matter perturbations in the Lagrangian frame and the expansion
parameter. We analyze deviations of SEoS models with respect to $Lambda$CDM in
the non-linear matter power spectrum ($P_k$), the halo mass function (HMF), and
the two-point correlation function (2PCF). On quantifying the nature of steep
(SEoS-I) and smooth transitions in DE field (CPL-lim), no signature of steep
transition is observed, rather found the overall impact of DE behaviors in
$P_k$ at level of $sim 2-3%$ and $sim 3-4%$ differences w.r.t $Lambda$CDM
at $z=0$ respectively. HMF shows the possibility to distinguish between the
models at the high mass ends. The best-fitted model assuming only background
and linear perturbations dubbed as SEoS-II largely deviates from $Lambda$CDM
and current observations on studying the nonlinear growth. This large deviation
in SEoS-II also quantified the combined effect of the dynamical DE and the
larger amount of matter contained, $Omega_{m0}$ and $H_{0}$ accordingly. 2PCF
results are relatively robust with $sim 1-2 %$ deviation for SEoS-I and
CPL-lim and a significant deviation for SEoS-II throughout $r$ from
$Lambda$CDM. Finally, we conclude that the search for viable DE models (like
the SEoS) must include non-linear growth constraints.

We study the nonlinear regime of large scale structure formation considering
a dynamical dark energy (DE) component determined by a Steep Equation of State
parametrization (SEoS) $w(z)=w_0+w_ifrac{(z/z_T)^q}{1+(z/z_T)^q}$. In order to
perform the model exploration at low computational cost, we modified the public
code L-PICOLA. We incorporate the DE model by means of the first and
second-order matter perturbations in the Lagrangian frame and the expansion
parameter. We analyze deviations of SEoS models with respect to $Lambda$CDM in
the non-linear matter power spectrum ($P_k$), the halo mass function (HMF), and
the two-point correlation function (2PCF). On quantifying the nature of steep
(SEoS-I) and smooth transitions in DE field (CPL-lim), no signature of steep
transition is observed, rather found the overall impact of DE behaviors in
$P_k$ at level of $sim 2-3%$ and $sim 3-4%$ differences w.r.t $Lambda$CDM
at $z=0$ respectively. HMF shows the possibility to distinguish between the
models at the high mass ends. The best-fitted model assuming only background
and linear perturbations dubbed as SEoS-II largely deviates from $Lambda$CDM
and current observations on studying the nonlinear growth. This large deviation
in SEoS-II also quantified the combined effect of the dynamical DE and the
larger amount of matter contained, $Omega_{m0}$ and $H_{0}$ accordingly. 2PCF
results are relatively robust with $sim 1-2 %$ deviation for SEoS-I and
CPL-lim and a significant deviation for SEoS-II throughout $r$ from
$Lambda$CDM. Finally, we conclude that the search for viable DE models (like
the SEoS) must include non-linear growth constraints.

http://arxiv.org/icons/sfx.gif

Comments are closed.