The clustering and evolution of Hα emitters at z ∼ 1 from HiZELS?

The clustering properties of a well-defined sample of 734 Hα emitters at z = 0.845 ± 0.015, obtained as part of the Hi-z Emission Line Survey (HiZELS), are investigated. The spatial correlation function of these Hα emitters is very well-described by the power law ξ = (r/r0) −1.8, with a real-space correlation, r0, of 2.7±0.3 h−1 Mpc. The correlation length r0 increases strongly with Hα luminosity (LHα) , from r0 ∼ 2 h−1 Mpc for the most quiescent galaxies (star-formation rates of ∼ 4Myr−1), up to r0> 5 h−1 Mpc for the brightest galax-ies in Hα. The correlation length also increases with increasing rest-frame K-band (MK) luminosity, but the r0-LHα correlation maintains its full statistical significance at fixed MK. At z = 0.84, star-forming galaxies classified as irregulars or mergers are much more clustered than discs and non-mergers, respectively; however, once the samples are matched in LHα and MK, the differences vanish, implying that the clustering is independent of morphological type at z ∼ 1 just as in the local Universe. The typical Hα emitters found at z = 0.84 reside in dark-matter haloes of ≈ 1012 M, but those with the highest SFRs reside in more massiv