Searching for Strong Gravitational Lenses

被引：0
作者：
Cameron Lemon
Frédéric Courbin
Anupreeta More
Paul Schechter
Raoul Cañameras
Ludovic Delchambre
Calvin Leung
Yiping Shu
Chiara Spiniello
Yashar Hezaveh
Jonas Klüter
Richard McMahon
机构：
[1] Observatoire de Sauverny,Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Fédérale de Lausanne (EPFL)
[2] The Inter-University Centre for Astronomy and Astrophysics (IUCAA),TUM School of Natural Sciences, Department of Physics
[3] Kavli Institute for the Physics and Mathematics of the Universe (IPMU),Institut d’Astrophysique et de Géophysique
[4] MIT Kavli Institute,Purple Mountain Observatory
[5] Max-Planck-Institut fur Astrophysik,Sub
[6] Technical University of Munich,Department of Astrophysics, Department of Physics
[7] Université de Liège,Département de Physique
[8] Chinese Academy of Sciences,Center for Computational Astrophysics
[9] INAF – Osservatorio Astronomico di Capodimonte,Department of Physics and Astronomy
[10] University of Oxford,Institute of Astronomy
[11] Université de Montréal,Kavli Institute for Cosmology
[12] Flatiron Institute,undefined
[13] Louisiana State University,undefined
[14] University of Cambridge,undefined
[15] University of Cambridge,undefined
来源：
Space Science Reviews | 2024年 / 220卷
关键词：
Gravitational lensing: strong;
D O I：
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学科分类号：
摘要：
Strong gravitational lenses provide unique laboratories for cosmological and astrophysical investigations, but they must first be discovered – a task that can be met with significant contamination by other astrophysical objects and asterisms. Here we review strong lens searches, covering various sources (quasars, galaxies, supernovae, FRBs, GRBs, and GWs), lenses (early- and late-type galaxies, groups, and clusters), datasets (imaging, spectra, and lightcurves), and wavelengths. We first present the physical characteristics of the lens and source populations, highlighting relevant details for constructing targeted searches. Search techniques are described based on the main lensing feature that is required for the technique to work, namely one of: (i) an associated magnification, (ii) multiple spatially-resolved images, (iii) multiple redshifts, or (iv) a non-zero time delay between images. To use the current lens samples for science, and for the design of future searches, we list several selection biases that exist due to these discovery techniques. We conclude by discussing the future of lens searches in upcoming surveys and the new population of lenses that will be discovered.
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