提出了一种从大面积光学/红外光度测量中识别候选高红移类星体（HzQs;（$z\gtrsim5.5$））的新方法，这些类星体是早期宇宙中超大质量黑洞生长的独特探针.使用高斯混合模型来构建似然性，并结合基于人口统计的知情先验，我们的方法使用贝叶斯框架来分配区分HzQs和污染源的后验概率。我们还包括深层无线电数据，以获得知情的先验。使用现有的HzQ数据在文献中，我们设置了一个后阈值，接受${\sim}90\%$已知的HzQs，而拒绝$>99\%$的污染物，如矮星或较低的红移星系。运行模拟HzQs和污染物的测试样本的概率选择，我们发现，概率方法的效率高于传统的颜色切割，减少了86%的接受的污染物的分数，同时保留了类似的分数HzQs。作为一个测试，我们应用我们的方法，泛星数据发布1（PS1）源目录内的HETDEX春天领域的天空，覆盖400平方米。°的与LOFAR两米巡天数据发布1（LoTSS DR 1）的深层无线电数据相吻合。从PS1中的${\sim}5\times10^5$源的初始样本，我们的选择入围251个候选HzQ，在目视检查后进一步减少到63个。对13个高概率HzQs的浅层光谱跟踪证实了$z=5.66$上一个以前未被发现的类星体，其光度颜色为$i-z = 1.4$，位于根据颜色选择HzQs时通常探测的区域之外。这一发现证明了我们的概率HzQ选择方法在选择更完整的HzQ样本方面的有效性，这在用于大型现有和即将到来的光度数据集时具有希望。
英文摘要：
We present a novel method to identify candidate high redshift quasars (HzQs; ($z\gtrsim5.5$), which are unique probes of supermassive black hole growth in the early Universe, from large area optical/infrared photometric surveys. Using Gaussian Mixture Models to construct likelihoods and incorporate informed priors based on population statistics, our method uses a Bayesian framework to assign posterior probabilities that differentiate between HzQs and contaminating sources. We additionally include deep radio data to obtain informed priors. Using existing HzQ data in the literature, we set a posterior threshold that accepts ${\sim}90\%$ of known HzQs while rejecting $>99\%$ of contaminants such as dwarf stars or lower redshift galaxies. Running the probability selection on test samples of simulated HzQs and contaminants, we find that the efficacy of the probability method is higher than traditional colour cuts, decreasing the fraction of accepted contaminants by 86% while retaining a similar fraction of HzQs. As a test, we apply our method to the Pan-STARRS Data Release 1 (PS1) source catalogue within the HETDEX Spring field area on the sky, covering 400 sq. deg. and coinciding with deep radio data from the LOFAR Two-metre Sky Survey Data Release 1 (LoTSS DR1). From an initial sample of ${\sim}5\times10^5$ sources in PS1, our selection shortlists 251 candidate HzQs, which are further reduced to 63 after visual inspection. Shallow spectroscopic follow-up of 13 high probability HzQs resulted in the confirmation of a previously undiscovered quasar at $z=5.66$ with photometric colours $i-z = 1.4$, lying outside the typically probed regions when selecting HzQs based on colours. This discovery demonstrates the efficacy of our probabilistic HzQ selection method in selecting more complete HzQ samples, which holds promise when employed on large existing and upcoming photometric data sets.
Revealing the link between halo mass and radio jet activities in quasars
Institute for Astronomy, University of Edinburgh（爱丁堡大学天文研究所）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Astrophysics, Department of Physics, University of Oxford（牛津大学物理系天体物理学）；Centre for Extragalactic Astronomy, Department of Physics, Durham University（达勒姆大学物理系河外天文中心）；Institute for Computational Cosmology, Department of Physics, University of Durham（达勒姆大学物理系计算宇宙学研究所）；Centre for Astrophysics Research, University of Hertfordshire（赫特福德大学天体物理学研究中心）
SHELLQs-JWST: Revealing the Spectra of Extended Emission in 12 z > 6 Quasar Host Galaxies using the JWST NIRSpec Fixed Slit
Princeton University（普林斯顿大学）；Waseda University（早稻田大学）；University of Tokyo（东京大学）；Johns Hopkins University（约翰斯·霍普金斯大学）；Ehime University（爱媛大学）；National Astronomical Observatory of Japan（日本国立天文台）；Graduate University for Advanced Studies (SOKENDAI)（综合研究大学院大学）；Japan Aerospace Exploration Agency (JAXA)（日本宇宙航空研究开发机构）；University of Toyama（富山大学）；Nara Women’s University（奈良女子大学）；Academia Sinica Institute of Astronomy and Astrophysics（中央研究院天文及天文物理研究所）；University of Arizona（亚利桑那大学）
The Quasar Feedback Survey: Revealing the importance of sensitive radio imaging for AGN identification deeper into the radio-quiet regime
Newcastle University（纽卡斯尔大学）；National Centre for Radio Astrophysics (NCRA) - Tata Institute of Fundamental Research (TIFR)（国家射电天体物理中心（NCRA）- 塔塔基础研究所（TIFR））；Durham University（杜伦大学）；European Southern Observatory (ESO)（欧洲南方天文台（ESO））；Institut de Radioastronomie Millimétrique (IRAM)（毫米波射电天体物理研究所（IRAM））；University of Hertfordshire（赫特福德大学）
SDSS-V: Revealing a weak accretion state in X-ray selected red quasars
Institute for Astronomy, University of Edinburgh（爱丁堡大学天体物理研究所）；Space Telescope Science Institute（太空望远镜科学研究所）；Department of Physics, Applied Physics, and Astronomy, Binghamton University（宾夕法尼亚州立大学宾汉姆顿分校物理、应用物理与天文系）；Max-Planck-Institut für extraterrestrische Physik (MPE)（马克斯·普朗克地外物理学研究所）；Exzellenzcluster ORIGINS（ORIGINS卓越集群）；Instituto de Estudios Astrofísicos, Facultad de Ingeniería y Ciencias, Universidad Diego Portales（迭戈·波特莱斯大学工程与科学学院天体物理研究所）；Universidad Nacional Autónoma de México, Instituto de Astronomía（墨西哥国立自治大学天体物理研究所）
Revealing the Gas Recycling in the Circumgalactic Medium (CGM) Utilizing a Luminous Ly$α$ Nebula Around a Type-II Quasar at z=2.6 with the Keck Cosmic Web Imager (KCWI)
Life After the Quasar: Overmassive Black Holes and Remnant Ionised Bubbles in and Around Two z~6.6 Galaxies
University of Geneva（日内瓦大学）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；University College London（伦敦大学学院）；Heidelberg University（海德堡大学）；Max Planck Institut für Astronomie（马克斯·普朗克天文学研究所）；University of Hertfordshire（赫特福德大学）；Aix Marseille Université（艾克斯-马赛大学）；Institute of Science and Technology Austria (ISTA)（奥地利科学和技术研究所）
Dual AGNs on 100 kpc Scales from the Million Quasar Catalog
School of Physics and Astronomy, Beijing Normal University（北京师范大学物理与天文学院）；Institute for Frontier in Astronomy and Astrophysics, Beijing Normal University（北京师范大学前沿交叉科学研究院）
Blackbody Quasar and Radio Source (BBQSORS): A Candidate of Transitional Little Red Dots with a $T\sim10^4\ K$ Blackbody Spectrum
Frontier Research Institute for Interdisciplinary Sciences, Tohoku University（东北大学前沿跨学科研究院）；Department of Physics, School of Advanced Science and Engineering, Faculty of Science and Engineering, Waseda University（早稻田大学理工学学术院高等科学与工程学院物理系）；Astronomical Institute, Tohoku University（东北大学天文研究所）；Institute of Astronomy, Graduate School of Science, The University of Tokyo（东京大学理学研究科天文学研究所）；Subaru Telescope, National Astronomical Observatory of Japan（日本国立天文台昴星团望远镜）；Department of Astronomy, University of Geneva（日内瓦大学天文学系）
Constraining the density distribution of the cold Circumgalactic Medium of quasars at z>2 through Lya, HeII and Ha emission
INAF – Osservatorio Astronomico di Trieste（意大利国家天体物理研究所的里雅斯特天文台）；Dipartimento di Fisica "G. Occhialini", Università degli Studi di Milano-Bicocca（米兰比可卡大学G. Occhialini物理系）；Department of Physics and Astronomy, University of California, Riverside（加州大学河滨分校物理与天文学系）；Cahill Center for Astrophysics, California Institute of Technology（加州理工学院卡希尔天体物理学中心）；Institute for Cosmic Ray Research, The University of Tokyo（东京大学宇宙射线研究所）；Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天文研究所）；Department of Physics, Informatics and Mathematics, University of Modena and Reggio Emilia（摩德纳和雷焦艾米利亚大学物理、信息学与数学系）
Unveiling the weak radio quasar population at z $\geq$ 4
我们对以$z\geq4$光学识别的高红移类星体为中心的20厘米射电天空空场微弱图像（FIRST）巡天图进行了图像叠加，以揭示这些活动星系核（AGN）中隐藏的$μ$ Jy射电辐射。$2229$光学鉴定活动星系核全样本的中值叠加程序揭示了一个积分通量密度为52 $~μ$ Jy的未分辨点源，信噪比为$\sim10$。我们共同添加的个人图像中心像素，以估计在$1.4~$ GHz的特征单色无线电功率考虑各种值的无线电频谱指数，揭示了无线电人口与$P_\mathrm{1.4GHz}\sim10^{24}~$ W Hz $^{-1}$。假设所有的射电辐射都来自于宿主星系核区的恒星形成（SF）活动，我们得到了特征恒星形成速率的上限，即$\sim4200~$ M $_\odot~$ yr $^{-1}$。FIRST图像的角分辨率不足以区分SF和AGN在这些红移处的射电辐射起源。然而，从文献中的个别来源的属性的比较表明，一个混合的性质是可能的。未来的甚长基线射电干涉测量观测和超深平方公里阵列巡天可望具有足够的灵敏度来探测和分辨宿主星系的中心$1-10~$ kpc区域，从而区分SF和AGN相关的辐射。
