The clustering of H$\beta$+[OIII] and [OII] emitters since $z\sim 5$: dependencies with line luminosity and stellar mass

Abstract

We investigate the clustering properties of $\sim 7000$ H$\beta$+[OIII] and [OII] narrowband-selected emitters at $z\sim 0.8-4.7$ from the High-$z$ Emission Line Survey. We find clustering lengths, $r_0$, of $1.5-4.0h^{-1}$ Mpc and minimum dark matter halo masses of $10^{10.7-12.1}{\mathrm{M}}_{\odot }$ for our $z=0.8-3.2$ H$\beta$+[OIII] emitters and $r_0\sim 2.0-8.3h^{-1}$ Mpc and halo masses of $10^{11.5-12.6}{\mathrm{M}}_{\odot }$ for our $z=1.5-4.7$ [OII] 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$\beta$+[OIII] emitters are found to reside in $10^{9.5}{\mathrm{M}}_{\odot }$ halos and the brightest emitters in $10^{13.0}{\mathrm{M}}_{\odot }$ halos. For [OII] emitters, the faintest emitters are found in $10^{10.5}{\mathrm{M}}_{\odot }$ halos and the brightest emitters in $10^{12.6}{\mathrm{M}}_{\odot }$ halos. A redshift-independent stellar mass dependency is also observed where the halo mass increases from $10^{11}{\mathrm{M}}_{\odot }$ to $10^{12.5}{\mathrm{M}}_{\odot }$ for stellar masses of $10^{8.5}{\mathrm{M}}_{\odot }$ to $10^{11.5}{\mathrm{M}}_{\odot }$, respectively. We investigate the interdependencies of these trends by repeating our analysis in a $L_{\text{line}}-{\mathrm{M}}_{\text{star}}$ grid space for our most populated samples (H$\beta$+[OIII] $z=0.84$ and [OII] $z=1.47$) 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 $10^{12.5-13}{\mathrm{M}}_{\odot }$ which may be due to quenching mechanisms in massive halos which is consistent with a transitional halo mass predicted by models.

arXiv comment19 pages, 11 figures, 4 tables, submitted to MNRAS

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