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We present redshift space two-point ($\xi$), three-point ($\zeta$) andreduced three-point (Q) correlations of Ly$\alpha$ absorbers (Voigt profilecomponents having HI column density, $N_{\rm HI}>10^{13.5}$cm$^{-2}$) overthree redshift bins spanning $1.7< z<3.5$ using high-resolution spectra of 292quasars. We detect positive $\xi$ up to 8 $h^{-1}$ cMpc in all three redshiftbins. The strongest detection of $\zeta =1.81\pm 0.59$ (with Q$=0.68\pm 0.23$),is in $z=1.7-2.3$ bin at $1-2h^{-1}$ cMpc. The measured $\xi$ and $\zeta$values show an increasing trend with $N_{\rm HI}$, while Q remains relativelyindependent of $N_{\rm HI}$. We find $\xi$ and $\zeta$ to evolve strongly withredshift. Using simulations, we find that $\xi$ and $\zeta$ seen in real spacemay be strongly amplified by peculiar velocities in redshift space. Simulationssuggest that while feedback, thermal and pressure smoothing effects influencethe clustering of Ly$\alpha$ absorbers at small scales, i.e $<0.5h^{-1}$ cMpc,the HI photo-ionization rate ($\Gamma_{\rm HI}$) has a strong influence at allscales. The strong redshift evolution of $\xi$ and $\zeta$ (for a fixed $N_{\rmHI}$-cutoff) is driven by the redshift evolution of the relationship between$N_{\rm HI}$ and baryon overdensity. Our simulation using best-fitted$\Gamma_{\rm HI}(z)$ measurements produces consistent clustering signals withobservations at $z\sim 2$ but under-predicts the clustering at higherredshifts. One possible remedy is to have higher values of $\Gamma_{\rm HI}$ athigher redshifts. Alternatively the discrepancy could be related tonon-equilibrium and inhomogeneous conditions prevailing during HeIIreionization not captured by our simulations.

monthly notices of the royal astronomical society

Measurement of redshift-space two- and three-point correlation of  Ly$\alpha$ absorbers at $1.7< z <3.5$: Implications on evolution of the  physical properties of IGM