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-Argüello</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. Velázquez</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.

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