Redshift space distortion of 21 cm line at 1 < |$z$| < 5 with cosmological hydrodynamic simulations.

We measure the scale dependence and redshift dependence of 21 cm line emitted from the neutral hydrogen gas at redshift 1 < |$z$| < 5 using full cosmological hydrodynamic simulations by taking the ratios between the power spectra of H  i –dark matter (DM) cross-correlation and DM autocorrelation. The neutral hydrogen distribution is computed in full cosmological hydrodynamic simulations including star formation and supernova feedback under a uniform ultraviolet background radiation. We find a significant scale dependence of H  i bias at |$z$| > 3 on scales of k ≳ 1 h  Mpc−1, but it is roughly constant at lower redshift |$z$| < 3. The redshift evolution of H  i bias is relatively slow compared to that of QSOs at similar redshift range. We also measure a redshift space distortion (RSD) of H  i gas to explore the properties of H  i clustering. Fitting to a widely applied theoretical prediction, we find that the constant bias is consistent with that measured directly from the real space power spectra, and the velocity dispersion is marginally consistent with the linear perturbation prediction. Finally, we compare the results obtained from our simulation and the Illustris simulation, and conclude that the detailed astrophysical effects do not affect the scale dependence of H  i bias very much, which implies that the cosmological analysis using 21 cm line of H  i will be robust against the uncertainties arising from small-scale astrophysical processes such as star formation and supernova feedback. [ABSTRACT FROM AUTHOR]