Line intensity mapping (LIM) experiments probing the nearby universe can expect a considerable amount of cosmic infrared background (CIB) contiuum emission coming from near and far-infrared galaxies. For the purpose of using the LIM data to constrain the star formation rate (SFR), we argue that the CIB continuum - traditionally treated as contamination - can be combined with the LIM signal to enhance the SFR constraints achievable. We first present a power spectrum model that is capable of joining continuum and line emissions that assume the same prior SFR model. We subsequently analyze the effectiveness of the joint model in the context of the EXperiment for Cryogenic Large-Aperture Intensity Mapping (EXCLAIM), which utilizes the [CII] molecular line to study the SFR. We numerically compute the theoretical power spectra according to our model and the EXCLAIM survey specifics, and perform Fisher analysis to obtain SFR parameter constraints. We find that although the joint model has no considerable advantage over LIM alone assuming the current survey level of EXCLAIM, its effects become significant when we consider more optimistic values of survey resolution and angular span that are expected of future LIM experiments. By manipulating the Fisher formalism, we show that the CIB is not only an additional SFR sensitive signal, but also serves to break the SFR parameter degeneracy that naturally emerges from the [CII] Fisher matrix. For this reason, addition of the CIB will allow improvements in the survey parameters to be better reflected in the SFR constraints, and can be effectively utilized by future LIM experiments.
Challenges of standard halo models in constraining galaxy properties from CIB anisotropies
Institutes of Computer Science and Astrophysics, Foundation for Research and Technology Hellas (FORTH)（计算机科学与天体物理研究所，希腊研究与技术基金会）；Aix Marseille Univ, CNRS, CNES, LAM（艾克斯马赛大学）；Université de Strasbourg, CNRS, Observatoire astronomique de Strasbourg, UMR 7550（斯特拉斯堡大学）；Kavli Institute for Particle Astrophysics and Cosmology, Stanford University（斯坦福大学卡弗里粒子天体物理学与宇宙学研究所）；SLAC National Accelerator Laboratory（SLAC国家加速器实验室）
Constraining the Expansion History and Early Dark Energy with Line Intensity Mapping
考虑线强度映射（IM）实验测量3 < z < 6范围内的重子声学振荡（BAO）的可能性。这将把膨胀历史限制在目前尚未探索的红移范围内。我们计算的地图深度，未来的IM实验针对CO（1-0）旋转过渡线和[CII]离子化碳精细结构线将需要实现，以测量BAO。我们发现，不久的将来IM实验可以限制BAO规模为5%或更好的CO/[CII]模型振幅。这种测量的精确度可能会对早期暗能量的模型产生竞争性限制。
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）
First Identification of a CMB Lensing Signal Produced by $1.5$ Million Galaxies at $z\sim$4: Constraints on Matter Density Fluctuations at High Redshift
Euclid: A UV-faint quasar in a highly luminous star-forming host galaxy at $z \approx 7.7$
Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚空间科学与天体物理观测台）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Hamburger Sternwarte, University of Hamburg（汉堡大学汉堡天文台）；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）；INAF-IASF Milano（意大利国家天体物理研究所米兰天文科学与技术研究所）；Institut für Theoretische Physik, University of Heidelberg（海德堡大学理论物理研究所）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）
Comparison of Cross-Correlation Methods for Line Intensity Mapping
University of Wisconsin-Madison（威斯康星大学麦迪逊分校）；Southern Methodist University（南方卫理公会大学）；New York University（纽约大学）；Flatiron Institute（平顿研究所）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Cornell University（康奈尔大学）
Euclid: Inferring star-formation history via cross-correlations of photometric clustering and shear with the cosmic infrared background
Università degli Studi di Torino（都灵大学）；INFN-Sezione di Torino（意大利国家核物理学会都灵分部）；INAF-Osservatorio Astrofisico di Torino（意大利国家天体物理研究所都灵天文台）；Università di Roma Tor Vergata（罗马托尔维加塔大学）；INFN, Sezione di Roma 2（意大利国家核物理学会罗马第二分部）；Université Paris-Saclay（巴黎萨克雷大学）；CNRS, Institut d’astrophysique spatiale（法国国家科学研究中心空间天体物理研究所）；Université de Strasbourg（斯特拉斯堡大学）；CNRS, Observatoire astronomique de Strasbourg（法国国家科学研究中心斯特拉斯堡天文台）；ESAC/ESA（欧洲空间应用中心/欧洲空间局）
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）
