English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

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 $10^{10.7 - 12.1}\rm{M}_\odot$ forour $z = 0.8 - 3.2$ H$\beta$+[OIII] emitters and $r_0 \sim 2.0 - 8.3h^{-1}$ Mpcand halo masses of $10^{11.5 - 12.6}\rm{M}_\odot$ for our $z = 1.5 - 4.7$ [OII]emitters. We find $r_0$ to strongly increase both with increasing lineluminosity and redshift. By taking into account the evolution of thecharacteristic line luminosity, $L^\star(z)$, and using our model predictionsof halo mass given $r_0$, we find a strong, redshift-independent increasingtrend between $L/L^\star(z)$ and minimum halo mass. The faintestH$\beta$+[OIII] emitters are found to reside in $10^{9.5}\rm{M}_\odot$ halosand the brightest emitters in $10^{13.0}\rm{M}_\odot$ halos. For [OII]emitters, the faintest emitters are found in $10^{10.5} \rm{M}_\odot$ halos andthe brightest emitters in $10^{12.6}\rm{M}_\odot$ halos. A redshift-independentstellar mass dependency is also observed where the halo mass increases from$10^{11}\rm{M}_\odot$ to $10^{12.5} \rm{M}_\odot$ for stellar masses of$10^{8.5}\rm{M}_\odot$ to $10^{11.5}\rm{M}_\odot$, respectively. We investigatethe interdependencies of these trends by repeating our analysis in a$L_\textrm{line} - \rm{M}_\textrm{star}$ grid space for our most populatedsamples (H$\beta$+[OIII] $z = 0.84$ and [OII] $z = 1.47$) and find that theline luminosity dependency is stronger than the stellar mass dependency on halomass. For $L > L^\star$ emitters at all epochs, we find a relatively flat trendwith halo masses of $10^{12.5 - 13}\rm{M}_\odot$ which may be due to quenchingmechanisms in massive halos which is consistent with a transitional halo masspredicted by models.

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