斯巴鲁/XMM-牛顿深度调查（SXDS）。IV。在1 ° ^2场中从z=3.1到5.7的Lya发射体的演化：光度函数和AGN
The Subaru/XMM-Newton Deep Survey (SXDS). IV. Evolution of Lya Emitters from z=3.1 to 5.7 in the 1 deg^2 Field: Luminosity Functions and AGN
摘要：
我们给出了斯巴鲁/XMM-牛顿深空巡天（SXDS）场1度^2天空中z=3.1、3.7和5.7时Lya发射体（LAEs）的光度函数（LF）和各种性质。我们根据斯巴鲁/Suprime-Cam的深空成像数据获得了858个LAE候选者的光度样本，以及斯巴鲁/FOCAS和VLT/VIMOS光谱仪获得的84个已确认LAE的光谱样本，测量体积约为10^6 Mpc^3，极限Lya光度约为3x10^42 erg/s。考虑到统计误差和场与场的变化，我们推导出了Lya和UV连续谱（~1500 nm）的LF。我们发现，表观Lya LF没有显示出显着的演变之间的z=3.1和5.7的1.8和2.7倍的L* 和phi*，分别。另一方面，LAEs的UV LF从z=3.1增加到5.7，表明具有Lya发射的星系在早期更常见。我们确定六LAEs活动星系核活动从我们的光谱结合VLA，斯皮策，和XMM-牛顿数据。在光度测定法选择的z=3.1和3.7的LAEs中，只有~ 1%显示活动星系核活动，而logL（Lya）>~ 43.4-43.6 erg/s的最亮LAEs似乎总是活动星系核的宿主。我们的LAE在紫外连续光谱中比脱落星系更蓝，这表明更低的灭绝和/或更年轻的恒星星族。我们的叠加分析提供了上限的射电光度和f（HeII）/f（Lya）线分数，并限制隐藏的恒星形成（+低光度AGN）和LAEs的原始人口。
英文摘要：
We present luminosity functions (LFs) and various properties of Lya emitters (LAEs) at z=3.1, 3.7, and 5.7, in a 1 deg^2 sky of the Subaru/XMM-Newton Deep Survey (SXDS) Field. We obtain a photometric sample of 858 LAE candidates based on deep Subaru/Suprime-Cam imaging data, and a spectroscopic sample of 84 confirmed LAEs from Subaru/FOCAS and VLT/VIMOS spectroscopy in a survey volume of ~10^6 Mpc^3 with a limiting Lya luminosity of ~3x10^42 erg/s. We derive the LFs of Lya and UV-continuum (~1500 Å) for each redshift, taking into account the statistical error and the field-to-field variation. We find that the apparent Lya LF shows no significant evolution between z=3.1 and 5.7 within factors of 1.8 and 2.7 in L* and phi*, respectively. On the other hand, the UV LF of LAEs increases from z=3.1 to 5.7, indicating that galaxies with Lya emission are more common at earlier epochs. We identify six LAEs with AGN activities from our spectra combined with VLA, Spitzer, and XMM-Newton data. Among the photometrically selected LAEs at z=3.1 and 3.7, only ~1 % show AGN activities, while the brightest LAEs with logL(Lya) >~ 43.4-43.6 erg/s appear to always host AGNs. Our LAEs are bluer in UV-continuum color than dropout galaxies, suggesting lower extinction and/or younger stellar populations. Our stacking analyses provide upper limits to the radio luminosity and the f(HeII)/f(Lya) line fraction, and constrain the hidden star formation (+low-luminosity AGN) and the primordial population in LAEs.
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