原星系团对于研究晕质量和恒星质量在早期宇宙中如何聚集是非常重要的。寻找这种过密区域的路标是一种流行的方法来识别原星系团候选者。超亮红外星系（HLIRGs），预计将居住在过密的地区与大量的晕。我们研究了迄今为止最大的HLIRG样本的百万分之一规模的环境，并调查它们是否主要生活在过密地区。我们首先研究了Herschel 250 $μ$ m源在HLIRGs周围的面密度，并与随机位置的面密度进行了比较。然后，我们比较周围的邻居的空间分布与周围的随机选择的星系使用深IRAC选择的目录与高质量的光度红移。我们还使用红移匹配的类星体样本和亚毫米星系（SMG）样本来验证我们的方法，因为以前的聚类研究已经测量了这些种群的宿主晕质量。最后，我们采用了朋友的朋友（FOF）算法寻找（原）集群主机HLIRG。我们发现，在3.7 $σ$显著性下，在100 $\arcsec$投影半径内，HLIRGs倾向于有更多明亮的恒星形成邻居（250 $μ$ m通量密度>10 mJy）。在我们的3D分析中，我们发现相对较弱的过剩IRAC选择的源在3百万秒差距内周围HLIRGs与随机星系邻居相比，主要受光度红移的不确定性和调查深度。我们发现一个更显着的差异（在4.7 $σ$的意义）在最深的EN1字段中的低频阵列（LOFAR）检测到的邻居的数量。与2 < z < 3的HLIRG相比，3 < z < 4的HLIRG显示出更强的过剩，与宇宙缩小一致。最后，我们选择并提出了30个最有前途的原星系团候选人的名单，为未来的后续观测。
英文摘要：
Protoclusters are important for studying how halo mass and stellar mass assemble in the early universe. Finding signposts of such over-dense regions is a popular method to identify protocluster candidates. Hyperluminous infrared galaxies (HLIRGs), are expected to reside in overdense regions with massive halos. We study the Mpc-scale environment of the largest HLIRG sample to date and investigate whether they predominantly live in overdense regions. We first explore the surface density of Herschel 250 $μ$m sources around HLIRGs and compare with that around random positions. Then, we compare the spatial distribution of neighbours around HLIRGs with that around randomly selected galaxies using a deep IRAC-selected catalogue with good-quality photometric redshifts. We also use a redshift-matched quasar sample and submillimeter galaxy (SMG) sample to validate our method, as previous clustering studies have measured the host halo masses of these populations. Finally, we adopt a Friends of Friends (FOF) algorithm to seek (proto)clusters that host HLIRGs. We find that HLIRGs tend to have more bright star-forming neighbours (with 250 $μ$m flux density >10 mJy) within 100$\arcsec$ projected radius than a random galaxy at a 3.7$σ$ significance. In our 3D analysis, we find relatively weak excess of IRAC-selected sources within 3 Mpc around HLIRGs compared with random galaxy neighbours, mainly influenced by photometric redshift uncertainty and survey depth. We find a more significant difference (at a 4.7$σ$ significance) in the number of Low Frequency Array (LOFAR)-detected neighbours in the deepest EN1 field. HLIRGs at 3 < z < 4 show stronger excess compared to HLIRGs at 2 < z < 3, consistent with cosmic downsizing. Finally, we select and present a list of 30 most promising protocluster candidates for future follow-up observations.
Where Giants Dwell: Probing the Environments of Early Massive Quiescent Galaxies
INAF - Astronomical Observatory of Trieste（意大利国家天体物理研究所的里雅斯特天文台）；IFPU - Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）；Tianjin Normal University（天津师范大学）；Institute for Physics, Laboratory for Galaxy Evolution, EPFL（洛桑联邦理工学院星系演化实验室）
Star formation and morphological trends in the Antlia cluster: Probing environmental influence out to 5R200
Universidad de La Serena（拉塞雷纳大学）；Instituto de Astronomia, Geofísica e Ciências Atmosféricas da Universidade de São Paulo（圣保罗大学天文、地球物理与大气科学研究所）；Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata（拉普拉塔国立大学天文与地球物理科学学院）；Universidad de Talca（塔尔卡大学）；Millennium Nucleus for Galaxies (MINGAL)（银河系千年核心（MINGAL））；Instituto de Astrofísica de La Plata, CONICET-UNLP（拉普拉塔天体物理研究所，阿根廷国家科学研究委员会-拉普拉塔国立大学）
Deep JWST spectroscopy of galaxies in a candidate ionized bubble at $z = 8.7$: probing reionization at pMpc scales with Ly$α$ emission
University of Cambridge（剑桥大学）；University of Arizona（亚利桑那大学）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；University of California, Santa Barbara（加州大学圣塔芭芭拉分校）；University of Vienna（维也纳大学）
