First Light and Reionisation Epoch Simulations (FLARES) X：高红移下的环境星系偏置与巡天方差
First Light and Reionisation Epoch Simulations (FLARES) X: Environmental Galaxy Bias and Survey Variance at High Redshift
Peter A. Thomas, Christopher C. Lovell, Maxwell G. A. Maltz, Aswin P. Vijayan, Stephen M. Wilkins, Dimitrios Irodotou, William J. Roper, Louise Seeyave
备注：
Accepted version. Thanks to the referee contains more extensive description of testing, comparison to online Cosmic Variance Calculator, and greater range of survey areas than the original submission
Upcoming deep galaxy surveys with JWST will probe galaxy evolution during the epoch of reionisation (EoR, $5\leq z\leq10$) over relatively compact areas (e.g. $\sim$ 300\,arcmin$^2$ for the JADES GTO survey). It is therefore imperative that we understand the degree of survey variance, to evaluate how representative the galaxy populations in these studies will be. We use the First Light And Reionisation Epoch Simulations (FLARES) to measure the galaxy bias of various tracers over an unprecedentedly large range in overdensity for a hydrodynamic simulation, and use these relations to assess the impact of bias and clustering on survey variance in the EoR. Star formation is highly biased relative to the underlying dark matter distribution, with the mean ratio of the stellar to dark matter density varying by a factor of 100 between regions of low and high matter overdensity (smoothed on a scale of 14$\,h^{-1}$cMpc). This is reflected in the galaxy distribution --the most massive galaxies are found solely in regions of high overdensity. As a consequence of the above, galaxies in the EoR are highly clustered, which can lead to large variance in survey number counts. For mean number counts $N\lesssim 100$ (1000), in a unit redshift slice of angular area 300\,arcmin$^2$ (1.4\,deg$^2$), the 2-sigma range in $N$ is roughly a factor of four (two). We present relations between the expected variance and survey area for different survey geometries; these relations will be of use to observers wishing to understand the impact of survey variance on their results.
The impact of cosmic ray feedback during the epoch of reionisation
EPFL（洛桑联邦理工学院）；Centre de Recherche Astrophysique de Lyon, CNRS UMR 5574, Univ. Lyon, Ens de Lyon（里昂天体物理研究中心）；Institut d’Astrophysique de Paris, CNRS, UMR 7095, Sorbonne Université（巴黎天体物理研究所）；Department of Astronomy, Yonsei University（延世大学天文学系）；Department of Astrophysical Sciences, Princeton University（普林斯顿大学天体物理科学系）；Program in Applied and Computational Mathematics, Princeton University（普林斯顿大学应用与计算数学项目）
First Light and Reionization Epoch Simulations (FLARES) XXII: UV-dust spatial offsets at the Epoch of Reionisation
University of Hertfordshire（赫特福德大学）；University of Sussex（萨塞克斯大学）；Technical University of Denmark（丹麦技术大学）；Academia Sinica（中央研究院）；University of Cambridge（剑桥大学）
Interpreting ALMA Observations of the ISM During the Epoch of Reionisation
我们目前的宇宙学，辐射流体动力学模拟星系形成的时期，再电离的努力对建模的星际介质（ISM）和解释ALMA观测。模拟和没有恒星辐射进行了比较，在大（百万秒差距），中间（几十千秒差距），和小（子千秒差距）尺度。在大尺度上，星系周围的致密区域在紫外光子穿透空隙之前首先恢复;然而，大量的中性气体仍然存在于晕中。中性气体的空间分布是高度动态的，并且与年龄超过几百万年的恒星存在反相关。对于我们具体的反馈实现，大多数金属保持在晕的维里半径内，并且它们按质量成比例地分布在电离和中性介质上。对于我们质量最大的星系${\rm M_h}\sim10^{11}$ M $_{\odot}$，大部分的CII和OI质量与冷中性团块有关。NII更分散，并在较温暖的气体中产生，而OIII则在具有较高电离参数的较热气体中产生，由光加热和超新星产生。如果ISM中存在较小的高金属丰度气体，那么这些离子的发射可能会被ALMA观测到，而星系的低金属丰度可能会导致这些系统低于本地[CII]-SFR关系。尘埃的存在会导致UV/Ly $α$和[CII]发射之间的空间偏移，正如Maiolino等人最近的观测所表明的那样。[OIII]可能在空间上与这两个分量偏移，因为它来自密度-温度相空间的不同部分。
First Light And Reionisation Epoch Simulations (FLARES) XX: Comparing semi-analytic models at high-redshift
University of Sussex（萨塞克斯大学）；The University of Western Australia（西澳大学）；University of Hertfordshire（赫特福德大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Flatiron Institute（平顿研究所）；University of Malta（马耳他大学）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）
The accretion of quasars at the epoch of reionisation: $JWST$ catches the primeval monsters slowly feasting
Scuola Normale Superiore（高等师范学校）；INAF – Osservatorio Astrofisico di Arcetri（国家天体物理研究所阿切特里天文台）；Università degli Studi di Firenze（佛罗伦萨大学）；INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica Milano（国家天体物理研究所米兰空间天体物理学和宇宙学研究所）；Pontificia Universidad Católica de Chile（智利天主教Pontifícia大学）；European Space Agency (ESA)（欧洲航天局）
On the unique evolutionary mechanisms of massive quiescent galaxies in the epoch of reionisation
Swinburne University of Technology（斯威本科技大学）；JWST Australia Data Centre [JADC], Swinburne Advanced Manufacturing and Design Centre [AMDC]（JWST澳大利亚数据中心，斯威本先进制造与设计中心）
Ionising properties of galaxies in JADES for a stellar mass complete sample: resolving the cosmic ionising photon budget crisis at the Epoch of Reionisation
The clustering of C IV and Si IV at the end of reionisation: A perspective from the E-XQR-30 survey
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）；IFPU - Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）；Centre for Extragalactic Astronomy, Durham University（杜伦大学河外天文中心）；Scuola Normale Superiore（比萨高等师范学院）；Centre for Astrophysics and Supercomputing, Swinburne University of Technology（斯威本科技大学天体物理学与超级计算中心）；Institute for Theoretical Physics, Heidelberg University（海德堡大学理论物理研究所）；Institute for Astronomy, University of Edinburgh（爱丁堡大学天文研究所）；ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO3D)（三维全天体物理学卓越研究中心）；Dipartimento di Fisica, Universitá di Trieste, Sezione di Astronomia（的里雅斯特大学物理系天文学部）；Institute of Astronomy, University of Cambridge（剑桥大学天文研究所）；Kavli Institute for Cosmology, University of Cambridge（剑桥大学卡弗里宇宙学研究所）；Augustana Campus, University of Alberta（阿尔伯塔大学奥古斯塔纳校区）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Tianjin Normal University（天津师范大学）；Research School of Astronomy and Astrophysics, Australian National University（澳大利亚国立大学天文与天体物理研究学院）
First Light and Reionization Epoch Simulations (FLARES) -- XV: The physical properties of super-massive black holes and their impact on galaxies in the early universe
Quasar Impostors: Two Extremely UV-Bright ($M_{\rm UV}\approx-23.5$) Reionisation-Epoch Galaxies Powered by Very Massive Stars
Leiden University（莱顿大学）；University of California, Santa Barbara（加州大学圣塔芭芭拉分校）；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 California, Los Angeles（加州大学洛杉矶分校）
The Extraordinary Maser Flaring Event in the Massive Protostellar System NGC6334I: Multi-Epoch Milliarcsecond Resolution Investigation of the 6.7-GHz Methanol Masers
CSIRO Space and Astronomy（澳大利亚联邦科学与工业研究组织空间与天文部）；University of Tasmania（塔斯马尼亚大学）；International Centre for Radio Astronomy Research, The University of Western Australia（西澳大学国际射电天文学研究中心）；Joint Institute for VLBI ERIC（甚长基线干涉测量欧洲研究基础设施合作联合研究所）；Hartebeesthoek Radio Astronomy Observatory（哈特比斯霍克射电天文台）
Resolving the Assembly of Disk Galaxies from the Epoch of Reionisation to Cosmic Noon
Research School of Astronomy and Astrophysics, Australian National University（澳大利亚国立大学天体物理与天文学研究学院）；Istituto Nazionale di Astrofisica (INAF)（意大利国家天体物理研究所）；Scuola Normale Superiore（比萨高等师范学院）；Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天体物理研究所）；DARK, Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯玻尔研究所DARK中心）
The Nature of High-Redshift Massive Quiescent Galaxies -- Searching for RUBIES-UDS-QG-z7 in FLARES
University of Sussex（苏塞克斯大学）；University of Portsmouth（朴茨茅斯大学）；University of Malta（马耳他大学）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）
Unveiling the Cosmic Dawn with SHARP: Probing extended Lyman-$α$ nebulae in a Universe less than 600 Myr old
INAF-IASF Milano（意大利国家天体物理研究所米兰天文物理研究所）；INAF – Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；Department of Mathematics and Physics, Roma Tre University（罗马三大大学数学与物理系）；INAF–OAT, Osservatorio Astronomico di Trieste（意大利国家天体物理研究所的里雅斯特天文台）
