Line intensity mapping (LIM) is a rapidly emerging technique for constraining cosmology and galaxy formation using multi-frequency, low angular resolution maps. Many LIM applications crucially rely on cross-correlations of two line intensity maps, or of intensity maps with galaxy surveys or galaxy/CMB lensing. We present a consistent halo model to predict all these cross-correlations and enable joint analyses, in 3D redshift-space and for 2D projected maps. We extend the conditional luminosity function formalism to the multi-line case, to consistently account for correlated scatter between multiple galaxy line luminosities. This allows us to model the scale-dependent decorrelation between two line intensity maps, a key input for foreground rejection and for approaches that estimate auto-spectra from cross-spectra. This also enables LIM cross-correlations to reveal astrophysical properties of the interstellar medium inacessible with LIM auto-spectra. We expose the different sources of luminosity scatter or "line noise" in LIM, and clarify their effects on the 1-halo and galaxy shot noise terms. In particular, we show that the effective number density of halos can in some cases exceed that of galaxies, counterintuitively. Using observational and simulation input, we implement this halo model for the H$α$, [Oiii], Lyman-$α$, CO and [Cii] lines. We encourage observers and simulators to measure galaxy luminosity correlation coefficients for pairs of lines whenever possible. Our code is publicly available at https://github.com/EmmanuelSchaan/HaloGen/tree/LIM . In a companion paper, we use this halo model formalism and code to highlight the degeneracies between cosmology and astrophysics in LIM, and to compare the LIM observables to galaxy detection for a number of surveys.
Joint Line Intensity Recovery from Multi-Tracer Cross-Correlations
Stanford University（斯坦福大学）；SLAC National Accelerator Laboratory（SLAC国家加速器实验室）；Kavli Institute for Particle Astrophysics and Cosmology, Stanford University（斯坦福大学卡弗里粒子天体物理与宇宙学研究所）；Boston University（波士顿大学）
From photometric surveys to HI intensity mapping: Improving constraints on magnification biases while testing gravity
Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto（波尔图大学理学院物理与天文系）；Instituto de Astrofisica e Ciências do Espaço, Universidade do Porto CAUP（波尔图大学CAUP空间科学与天体物理研究所）；Department of Physics & Astronomy, University of the Western Cape（西开普大学物理与天文学系）
Probing primordial non-Gaussianity with the power spectrum and bispectrum of future 21cm intensity maps
在再电离之后，星系中中性氢的21厘米发射线提供了暗物质的示踪物。使用SKA和其他射电望远镜进行的下一代强度测绘调查将覆盖大范围的天空区域和广泛的红移，便于将其用作原始非高斯性的探测器。{以前的工作已经表明，双谱可以实现对原始非高斯性的严格约束，未来的调查是专门设计用于干涉仪模式下的强度映射}。在这里，我们调查的约束条件，可从单碟模式下操作的调查，\rev{using the combined power spectrum and bispectrum signal}。在功率谱的情况下，单碟调查通常优于干涉仪调查。我们发现，相反的双谱：单碟调查是没有竞争力的干涉仪模式设计的调查。
Observational Frontiers in the post-EoR 21-cm Intensity Mapping: Lessons from the SKA Pathfinders
Indian Institute of Technology Madras（印度马德拉斯理工学院）；Indian Institute of Technology Kharagpur（印度卡拉格普尔理工学院）；University of Manchester（曼彻斯特大学）；University of Western Cape（西开普敦大学）；McGill University（麦吉尔大学）；California Institute of Technology（加州理工学院）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；University of Chinese Academy of Sciences（中国科学院大学）；Northeastern University（东北大学）；ETH Zurich（苏黎世联邦理工学院）；Indian Institute of Technology Indore（印度印多尔理工学院）；Arizona State University（亚利桑那州立大学）；Massachusetts Institute of Technology（麻省理工学院）；Perimeter Institute for Theoretical Physics（理论物理珀塞尔研究所）；University of Western Australia（西澳大学）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）
Cosmology beyond standard sirens: cross-correlation of gravitational waves and neutral hydrogen intensity mapping
Gran Sasso Science Institute (GSSI)（格兰萨索科学研究所）；INFN - Laboratori Nazionali del Gran Sasso (LNGS)（意大利国家核物理研究所-格兰萨索国家实验室）；Marietta Blau Institute - Austrian Academy of Sciences（玛丽亚·布劳研究所-奥地利科学院）；Institute for Theoretical Particle Physics and Cosmology, RWTH Aachen University（亚琛工业大学理论粒子物理与宇宙学研究所）；INAF - Institute of Radioastronomy (IRA)（意大利国家天体物理研究所-射电天文研究所）；INFN, Sezione di Bologna（意大利国家核物理研究所博洛尼亚分部）；Observatoire de la Côte d’Azur, Laboratoire Lagrange（蔚蓝海岸天文台拉格朗日实验室）；Department of Physics & Astronomy, University of the Western Cape（西开普大学物理与天文学系）；Dipartimento di Fisica, Università degli Studi di Cagliari（卡利亚里大学物理系）；INFN, Sezione di Cagliari（意大利国家核物理研究所卡利亚里分部）；INAF - Osservatorio Astronomico di Cagliari（意大利国家天体物理研究所卡利亚里天文台）；INFN, Sezione di Roma（意大利国家核物理研究所罗马分部）
Field-level multi-tracers simulation-based inference of cosmological parameters from 3D maps
SISSA（国际高等研究学院）；INFN Sezione di Trieste（意大利国家核物理研究所的里雅斯特分部）；ICSC – Centro Nazionale di Ricerca in High Performance Computing, Big Data e Quantum Computing（高性能计算、大数据与量子计算国家研究中心）；Imperial College London（帝国理工学院）；IFPU - Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）
When galaxies burst: enhanced shot-noise for line-intensity mapping in the JWST era
Ben-Gurion University of the Negev（内盖夫本-古里安大学）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；Cosmic Frontier Center, The University of Texas at Austin（德克萨斯大学奥斯汀分校宇宙前沿中心）；Tel-Aviv University（特拉维夫大学）
Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；California Institute of Technology（加州理工学院）；University of Pennsylvania（宾夕法尼亚大学）
Exploring future synergies for large-scale structure between gravitational waves and radio sources
Queen Mary University of London（伦敦大学皇家玛丽学院）；Instituto de Astrofisica e Ciências do Espaço, Universidade do Porto CAUP（波尔图大学CAUP天体物理学与空间科学研究所）；University of the Western Cape（西开普敦大学）；Universidade do Porto（波尔图大学）；Institute of Cosmology and Gravitation, University of Portsmouth（朴茨茅斯大学宇宙学与引力研究所）
A New Window into the Baryon Cycle at Cosmic Noon with Line Intensity Mapping: Forecasts for auto- and cross-correlations in [CII]-158$μ$m, HI 21 cm, CO$_{J+1\rightarrow J}$, and H$α$ galaxies
University of Pennsylvania（宾夕法尼亚大学）；University of California, Los Angeles（加州大学洛杉矶分校）；California Institute of Technology（加州理工学院）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；University of Illinois Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校）；University of Virginia（弗吉尼亚大学）
