The host dark matter haloes of [O II] emitters at 0.5 < z < 1.5
The host dark matter haloes of [O II] emitters at 0.5 < z < 1.5
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DOI：
10.1093/mnras/stx2807
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发表时间：
2017-08
影响因子：
4.8
通讯作者：
V. Gonzalez-Perez;J. Comparat;P. Norberg;C. Baugh;S. Contreras;C. Lacey;N. McCullagh;Á. Orsi;J. Helly;J. Portsmouth;Mpie;Durham;Puc;Cefca
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文献类型：
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作者：
V. Gonzalez-Perez;J. Comparat;P. Norberg;C. Baugh;S. Contreras;C. Lacey;N. McCullagh;Á. Orsi;J. Helly;J. Portsmouth;Mpie;Durham;Puc;Cefca
发射线星系(ELG)被用于几个正在进行和即将进行的调查(SDSSIV/EBOSS，DESI)，作为暗物质分布的示踪剂。利用一个新的星系形成模型，我们研究了在z1的光学ELG选择中占主导地位的[O II]发射体的特征。选择了0.5<；z<；1.5的模型[O II]发射体来模拟DEEP2、VVDS、EBoss和DESI测量。[O II]模型发射体的光度函数与观测结果符合得很好。选定的[O II]发射体由MHALO≥1010.3h−1M的光晕托管，其中∼90%是中央恒星形成星系。预测的[O II]发射体的平均晕占据分布具有恒星形成星系的典型形状，中心星系N[O II]cen的贡献远离正则阶跃函数。N[O II]cen可以描述为圆盘的非对称高斯和球体的阶跃函数之和，它们的平台值低于1。模型[O II]发射器具有接近统一的聚集偏向，这低于对EBOSS和DESI ELG的期望。在z∼1，与观测到的由[O II]发射体主导的g带选择星系的比较表明，我们的模型产生的卫星星系的[O II]发射体太少。这表明有必要修改我们对卫星星系中热气剥离的模型。
Emission line galaxies (ELGs) are used in several ongoing and upcoming surveys (SDSSIV/eBOSS, DESI) as tracers of the dark matter distribution. Using a new galaxy formation model, we explore the characteristics of [O II] emitters, which dominate optical ELG selections at z 1. Model [O II] emitters at 0.5 < z < 1.5 are selected to mimic the DEEP2, VVDS, eBOSS and DESI surveys. The luminosity functions of model [O II] emitters are in reasonable agreement with observations. The selected [O II] emitters are hosted by haloes with Mhalo ≥ 1010.3h−1M, with ∼90 per cent of them being central star-forming galaxies. The predicted mean halo occupation distributions of [O II] emitters have a shape typical of that inferred for star-forming galaxies, with the contribution from central galaxies, N[O II] cen, being far from the canonical step function. The N[O II] cen can be described as the sum of an asymmetric Gaussian for discs and a step function for spheroids, which plateau below unity. The model [O II] emitters have a clustering bias close to unity, which is below the expectations for eBOSS and DESI ELGs. At z ∼ 1, a comparison with observed g-band-selected galaxy, which is expected to be dominated by [O II] emitters, indicates that our model produces too few [O II] emitters that are satellite galaxies. This suggests the need to revise our modelling of hot gas stripping in satellite galaxies.