%0 Generic %1 khostovan2017clustering %A Khostovan, Ali Ahmad %A Sobral, David %A Mobasher, Bahram %A Best, Philip N. %A Smail, Ian %A Matthee, Jorryt %A Darvish, Behnam %A Nayyeri, Hooshang %A Hemmati, Shoubaneh %A Stott, John P. %D 2017 %K clustering emitters evolution line redshift %T The clustering of H$\beta$+OIII and OII emitters since $z 5$: dependencies with line luminosity and stellar mass %U http://arxiv.org/abs/1705.01101 %X We investigate the clustering properties of $7000$ H$\beta$+OIII and OII narrowband-selected emitters at $z 0.8 - 4.7$ 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 $10^10.7 - 12.1M_ødot$ for our $z = 0.8 - 3.2$ H$\beta$+OIII emitters and $r_0 2.0 - 8.3h^-1$ Mpc and halo masses of $10^11.5 - 12.6M_ødot$ 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 $10^9.5M_ødot$ halos and the brightest emitters in $10^13.0M_ødot$ halos. For OII emitters, the faintest emitters are found in $10^10.5 M_ødot$ halos and the brightest emitters in $10^12.6M_ødot$ halos. A redshift-independent stellar mass dependency is also observed where the halo mass increases from $10^11M_ødot$ to $10^12.5 M_ødot$ for stellar masses of $10^8.5M_ødot$ to $10^11.5M_ødot$, 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$\beta$+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 $10^12.5 - 13M_ødot$ which may be due to quenching mechanisms in massive halos which is consistent with a transitional halo mass predicted by models.

@misc{khostovan2017clustering, 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 $10^{10.7 - 12.1}\rm{M}_\odot$ 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 $10^{11.5 - 12.6}\rm{M}_\odot$ 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 $10^{9.5}\rm{M}_\odot$ halos and 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 and the brightest emitters in $10^{12.6}\rm{M}_\odot$ halos. A redshift-independent stellar 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 investigate the interdependencies of these trends by repeating our analysis in a $L_\textrm{line} - \rm{M}_\textrm{star}$ 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 $10^{12.5 - 13}\rm{M}_\odot$ which may be due to quenching mechanisms in massive halos which is consistent with a transitional halo mass predicted by models.}, added-at = {2017-05-04T10:32:06.000+0200}, author = {Khostovan, Ali Ahmad and Sobral, David and Mobasher, Bahram and Best, Philip N. and Smail, Ian and Matthee, Jorryt and Darvish, Behnam and Nayyeri, Hooshang and Hemmati, Shoubaneh and Stott, John P.}, biburl = {https://www.bibsonomy.org/bibtex/21e140fc22be7033803a919fad00f106c/miki}, description = {[1705.01101] The clustering of H$\beta$+[OIII] and [OII] emitters since $z \sim 5$: dependencies with line luminosity and stellar mass}, interhash = {ed62f77b91c6d1529b6535a7be8ee279}, intrahash = {1e140fc22be7033803a919fad00f106c}, keywords = {clustering emitters evolution line redshift}, note = {cite arxiv:1705.01101Comment: 19 pages, 11 figures, 4 tables, submitted to MNRAS}, timestamp = {2017-05-04T10:32:06.000+0200}, title = {The clustering of H$\beta$+[OIII] and [OII] emitters since $z \sim 5$: dependencies with line luminosity and stellar mass}, url = {http://arxiv.org/abs/1705.01101}, year = 2017 }