%0 Generic %1 kusakabe2017stellar %A Kusakabe, Haruka %A Shimasaku, Kazuhiro %A Ouchi, Masami %A Nakajima, Kimihiko %A Goto, Ryosuke %A Hashimoto, Takuya %A Konno, Akira %A Harikane, Yuichi %A Silverman, John D. %A Capak, Peter L. %D 2017 %K Lya emitters halo mass stellar %T Stellar and Dark Matter Halo Properties of LAEs at $z\sim2$ %U http://arxiv.org/abs/1707.09373 %X We present average stellar population properties and dark matter halo masses of $z 2$ Ly$\alpha$ emitters (LAEs) from SED fitting to stacked images and clustering analysis, respectively, using $\simeq$ $1250$ $NB387łe25.5$ objects in four separate fields of $1$ deg$^2$ in total. With an average stellar mass of $10.2\, \pm\, 3.010^8\ M_ødot$ and star formation rate of $3.4\, \pm\, 0.7\ M_ødot\ yr^-1$, the LAEs lie on a low-mass extrapolation of the star-formation main sequence (MS) with moderate star formation. Their effective dark matter halo mass is estimated to be $4.0_-2.9^+5.1 10^10\ M_ødot$ with $b_g,\, eff^\rm ave = 1.22^+0.16_-0.18$, which is lower than that of $z 2$ LAEs ($b_g,\, eff = 1.8\, \pm\, 0.3$) obtained by a previous study based on a three times smaller area with a probability of $96\%$, although this difference can be explained if the cosmic variance in these $b_g,\, eff$ is taken into account. Such a low halo mass, if it implies a low HI gas mass, is consistent with high Ly$\alpha$ escape fractions of LAEs observed. Despite the low halo mass and being in the MS mode, our LAEs have a relatively high stellar-to-halo mass ratio (SHMR) and baryon conversion efficiency, converting baryons into stars efficiently until the observed time. The extended Press-Schechter formalism predicts that at $z=0$ our LAEs are typically embedded in halos with masses similar to that of the Large Magellanic Cloud (LMC); if their SFRs are largely suppressed after $z 2$ as reported for the LMC itself, they will also have similar SHMRs to the LMC.

@misc{kusakabe2017stellar, abstract = {We present average stellar population properties and dark matter halo masses of $z \sim 2$ Ly$\alpha$ emitters (LAEs) from SED fitting to stacked images and clustering analysis, respectively, using $\simeq$ $1250$ $NB387\le25.5$ objects in four separate fields of $\simeq 1$ deg$^2$ in total. With an average stellar mass of $10.2\, \pm\, 3.0\times 10^8\ {\mathrm M_\odot}$ and star formation rate of $3.4\, \pm\, 0.7\ {\rm M_\odot}\ {\rm yr^{-1}}$, the LAEs lie on a low-mass extrapolation of the star-formation main sequence (MS) with moderate star formation. Their effective dark matter halo mass is estimated to be $4.0_{-2.9}^{+5.1} \times 10^{10}\ {\rm M_\odot}$ with $b_{\rm g,\, eff}^{\rm ave} = 1.22^{+0.16}_{-0.18}$, which is lower than that of $z \sim 2$ LAEs ($b_{\rm g,\, eff} = 1.8\, \pm\, 0.3$) obtained by a previous study based on a three times smaller area with a probability of $96\%$, although this difference can be explained if the cosmic variance in these $b_{\rm g,\, eff}$ is taken into account. Such a low halo mass, if it implies a low HI gas mass, is consistent with high Ly$\alpha$ escape fractions of LAEs observed. Despite the low halo mass and being in the MS mode, our LAEs have a relatively high stellar-to-halo mass ratio (SHMR) and baryon conversion efficiency, converting baryons into stars efficiently until the observed time. The extended Press-Schechter formalism predicts that at $z=0$ our LAEs are typically embedded in halos with masses similar to that of the Large Magellanic Cloud (LMC); if their SFRs are largely suppressed after $z \sim 2$ as reported for the LMC itself, they will also have similar SHMRs to the LMC.}, added-at = {2017-08-01T11:03:04.000+0200}, author = {Kusakabe, Haruka and Shimasaku, Kazuhiro and Ouchi, Masami and Nakajima, Kimihiko and Goto, Ryosuke and Hashimoto, Takuya and Konno, Akira and Harikane, Yuichi and Silverman, John D. and Capak, Peter L.}, biburl = {https://www.bibsonomy.org/bibtex/2d6e1763fdc05b4dbc84273e37ce1b535/miki}, description = {[1707.09373] Stellar and Dark Matter Halo Properties of LAEs at $z\sim2$}, interhash = {a25267da6efc93ad4700ff9d320eafe3}, intrahash = {d6e1763fdc05b4dbc84273e37ce1b535}, keywords = {Lya emitters halo mass stellar}, note = {cite arxiv:1707.09373Comment: 29 pages, 15 figures, 6 tables, submitted to PASJ. Comments welcome!}, timestamp = {2017-08-01T11:03:04.000+0200}, title = {Stellar and Dark Matter Halo Properties of LAEs at $z\sim2$}, url = {http://arxiv.org/abs/1707.09373}, year = 2017 }