The clustering of H β plus [O III] and [O II] emitters since z ∼ 5: dependencies with line luminosity and stellar mass

We investigate the clustering properties of similar to 7000 H beta + [O III] and [O II] narrowband-selected emitters at z similar to 0.8-4.7 from the High-z Emission Line Survey. We find clustering lengths, r(0), of 1.5-4.0 h(-1) Mpc and minimum dark matter halo masses of 10(10.7-12.1) M-circle dot for our z = 0.8-3.2 H beta + [O III] emitters and r(0) similar to 2.0-8.3 h(-1) Mpc and halo masses of 10(11.5-12.6) M-circle dot for our z = 1.5-4.7 [O II] emitters. We find r(0) to strongly increase both with increasing line luminosity and redshift. By taking into account the evolution of the characteristic line luminosity, L-star (z), and using our model predictions of halo mass given r(0), we find a strong, redshift-independent increasing trend between L/L-star (z) and minimum halo mass. The faintest H beta + [O III] emitters are found to reside in 10(9.5) M-circle dot haloes and the brightest emitters in 10(13.0) M-circle dot haloes. For [O II] emitters, the faintest emitters are found in 10(10.5) M-circle dot haloes and the brightest emitters in 10(12.6) M-circle dot haloes. A redshift-independent stellar mass dependency is also observed where the halo mass increases from 10(11) to 10(12.5) M-circle dot for stellar masses of 10(8.5) to 10(11.5) M-circle dot, respectively. We investigate the interdependencies of these trends by repeating our analysis in a L-line - M-star grid space for our most populated samples (H beta + [O III] z = 0.84 and [O II] z = 1.47) and find that the line luminosity dependency is stronger than the stellar mass dependency on halo mass. For L > L-star emitters at all epochs, we find a relatively flat trend with halo masses of 10(12.5-13) M-circle dot, which may be due to quenching mechanisms in massive haloes that is consistent with a transitional halo mass predicted by models.