AI 中文总结
研究红移1.88 < z < 3.52时射电AGN活动与莱曼α发射的联系，通过测量fAGN,radio和fLya，利用HETDEX与LOFAR数据，经完整性校正得出相关占比及变化，发现多数莱曼α发射由恒星形成驱动，两者缺乏相关性。
AI 中文摘要
莱曼α发射体（LAEs）是具有强莱曼α发射的星系，可追踪早期恒星形成和电离辐射。它们与活动星系核（AGNs）的联系是理解（扩展）莱曼α发射背后机制的关键。在这项工作中，我们测量了被识别为射电发射AGN的LAEs占比（fAGN,radio）和表现出莱曼α发射的射电源占比（fLya），以研究红移1.88 < z < 3.52时射电AGN活动与莱曼α发射之间的联系。我们识别出928个在霍比-埃伯利望远镜暗能量实验（HETDEX）和低频阵列（LOFAR）调查中均被探测到的源。这些匹配来自55,109个经光谱确认的LAEs和27,625个射电源。应用完整性校正后，我们得到fAGN,radio = 1.77 ± 0.04%和fLya = 18.15 ± 0.14%。fAGN,radio随莱曼α光度增加从0.4 ± 0.1%增至9.7 ± 1.3%，而fLya随射电光度从0.7 ± 0.1%升至55.8 ± 14.5%。“有射电AGN的LAEs”和“有莱曼α发射的光学AGN”在AGN阈值以上显示出相似的射电光度，尽管光学AGN有更高的莱曼α光度。我们发现莱曼α光度与射电光度或光谱指数之间无显著相关性。莱曼α线宽随莱曼α光度增加但与射电大小无相关性。我们的结果表明，红移1.88 < z < 3.52时的大多数莱曼α发射由恒星形成驱动，射电AGN活动局限于一个小的高光度子集（1.77 ± 0.04%）。莱曼α与射电性质之间缺乏相关性表明，莱曼α发射主要由宿主星系气体性质而非直接的AGN喷流耦合控制。
英文摘要
Lya emitters (LAEs) are galaxies with strong Lya emission, tracing early star formation and ionizing radiation. Their connection to active galactic nuclei (AGNs) is key to understanding the mechanisms behind (extended) Lya emission. In this work, we measure the fraction of LAEs identified as radio-emitting AGN (fAGN,radio) and the fraction of radio sources that exhibit Lya emission (fLya) to investigate the connection between radio AGN activity and Lya emission at 1.88 < z < 3.52. We identify 928 sources detected in both the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX) and the LOw Frequency ARray (LOFAR) surveys. These matches are drawn from 55,109 spectroscopically confirmed LAEs and 27,625 radio sources. After applying completeness corrections, we obtain fAGN,radio = 1.77 $\pm$ 0.04% and fLya = 18.15 $\pm$ 0.14%. The fraction fAGN,radio increases from 0.4 $\pm$ 0.1% to 9.7 $\pm$ 1.3% with increasing Lya luminosity, while fLya rises from 0.7 $\pm$ 0.1% to 55.8 $\pm$ 14.5% with radio luminosity. `LAEs with radio AGN' and `optical AGN with Lya emission' show similar radio luminosities above the AGN threshold, although optical AGN have higher Lya luminosities. We find no significant correlation between Lya luminosity and either radio luminosity or spectral index. Lya line width increases with Lya luminosity but shows no correlation with radio size. Our results show that most Lya emission at 1.88 < z < 3.52 is powered by star formation, with radio AGN activity confined to a small luminous subset (1.77 $\pm$ 0.04%). The absence of correlations between Lya and radio properties suggests that Lya emission is governed primarily by host-galaxy gas properties rather than direct AGN jet coupling.
Comments14 pages, 10 figures, 2 tables. Accepted for publication in Astronomy & Astrophysics (A&A)
