http://arxiv.org/abs/1801.07868
The post-reionization ${\rm HI}$ 21-cm signal is an excellent candidate for precision cosmology, this however requires accurate modelling of the expected signal. Sarkar et al. (2016) have simulated the real space ${\rm HI}$ 21-cm signal, and have modelled the ${\rm HI}$ power spectrum as $P_{{\rm HI}}(k)=b^2 P(k)$ where $P(k)$ is the dark matter power spectrum and $b(k)$ is a (possibly complex) scale dependent bias for which fitting formulas have been provided. This paper extends these simulations to incorporate redshift space distortion and predict the expected redshift space ${\rm HI}$ 21-cm power spectrum $P^s_{{\rm HI}}(k_{\perp},k_{\parallel})$ using two different prescriptions for the ${\rm HI}$ distributions and peculiar velocities. We model $P^s_{{\rm HI}}(k_{\perp},k_{\parallel})$ assuming that it is the product of $P_{{\rm HI}}(k)=b^2 P(k)$ with a Kaiser enhancement term and a Finger of God (FoG) damping which has $\sigma_p$ the pair velocity dispersion as a free parameter. Considering several possibilities for the bias and the damping profile, we find that the models with a scale dependent bias and a Lorentzian damping profile best fit the simulated $P^s_{{\rm HI}}(k_{\perp},k_{\parallel})$ over the entire range $1 \le z \le 6$. The best fit value of $\sigma_p$ falls approximately as $(1+z)^{-m}$ with $m=2$ and $1.2$ respectively for the two different prescriptions. The model predictions are consistent with the simulations for $k < 0.3 \, {\rm Mpc}^{-1}$ over the entire $z$ range for the monopole $P^s_0(k)$, and at $z \le 3$ for the quadrupole $P^s_2(k)$. At $z \ge 4$ the models underpredict $P^s_2(k)$ at large $k$, and the fit is restricted to $k < 0.15 \, {\rm Mpc}^{-1}$.
D. Sarkar and S. Bharadwaj
Thu, 25 Jan 18
19/67
Comments: 14 pages, 7 figures, 2 Tables, accepted for publication in MNRAS main journal