@article{b2dbb9326f644a8d85220d9b8029095e,
title = "X-ray study of the double source plane gravitational lens system Eye of Horus observed with XMM-Newton",
abstract = "A double source plane (DSP) system is a precious probe for the density profile of distant galaxies and cosmological parameters. However, these measurements could be affected by the surrounding environment of the lens galaxy. Thus, it is important to evaluate the cluster-scale mass for detailed mass modelling. We observed the Eye of Horus, a DSP system discovered by the Hyper Suprime-Cam Subaru Strategic Survey (HSC-SSP), with XMM-Newton. We detected two X-ray extended emissions, originating from two clusters, one centred at the Eye of Horus, and the other located ~100 arcsec north-east to the Eye of Horus.We determined the dynamical mass assuming hydrostatic equilibrium, and evaluated their contributions to the lens mass interior of the Einstein radius. The contribution of the former cluster is 1.1+1.2-0.5 × 1012M⊙, which is 21-76 per cent of the total mass within the Einstein radius. The discrepancy is likely due to the complex gravitational structure along the line of sight. On the other hand, the contribution of the latter cluster is only ~ 2 per cent on the Eye of Horus. Therefore, the influence associated with this cluster can be ignored.",
keywords = "Clusters, Clusters, Gravitational lensing, HSC J142449- 005322 - galaxies, Individual, Intracluster medium, Strong-Galaxies",
author = "Keigo Tanaka and Ayumi Tsuji and Hiroki Akamatsu and Chan, {J. H.H.} and Jean Coupon and Eiichi Egami and Francois Finet and Ryuichi Fujimoto and Yuto Ichinohe and Jaelani, {Anton T.} and Lee, {Chien Hsiu} and Ikuyuki Mitsuishi and Anupreeta More and Surhud More and Masamune Oguri and Nobuhiro Okabe and Naomi Ota and Rusu, {Cristian E.} and Alessandro Sonnenfeld and Masayuki Tanaka and Shutaro Ueda and Wong, {Kenneth C.}",
note = "Funding Information: This work is also supported in part by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, and JSPS KAKENHI Grants Nos JP15H05892, JP17H02868, JP18K03693, and JP19H05189. Funding Information: The Pan-STARRS1 Surveys have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen{\textquoteright}s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under Grant No. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE), and the Los Alamos National Laboratory. Funding Information: The HSC collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Funding was contributed by the FIRST program from Japanese Cabinet Office, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University. This paper has used software developed for the Large Synoptic Survey Telescope.We thank the LSST Project for making their code available as free software at http://dm.lsst.org. The Pan-STARRS1 Surveys have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National CentralUniversity of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under Grant No. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE), and the Los Alamos National Laboratory. This work is supported in part by the Ministry of Science and Technology of Taiwan (Grant No. MOST 106-2628-M-001-003- MY3) and by Academia Sinica (Grant No. AS-IA-107-M01). Thiswork is also supported in part byWorld Premier International Research Center Initiative (WPI Initiative),MEXT, Japan, and JSPS KAKENHI Grants Nos JP15H05892, JP17H02868, JP18K03693, and JP19H05189. KCW is supported in part by an EACOA Fellowship awarded by the East Asia Core Observatories Association, which consists of the Academia Sinica Institute of Astronomy and Astrophysics, the National Astronomical Observatory of Japan, the National Astronomical Observatories of the Chinese Academy of Sciences, and the Korea Astronomy and Space Science Institute. Funding Information: This work is supported in part by the Ministry of Science and Technology of Taiwan (Grant No. MOST 106-2628-M-001-003-MY3) and by Academia Sinica (Grant No. AS-IA-107-M01). Funding Information: The HSC collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Funding was contributed by the FIRST program from Japanese Cabinet Office, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University. Funding Information: KCW is supported in part by an EACOA Fellowship awarded by the East Asia Core Observatories Association, which consists of the Academia Sinica Institute of Astronomy and Astrophysics, the National Astronomical Observatory of Japan, the National Astronomical Observatories of the Chinese Academy of Sciences, and the Korea Astronomy and Space Science Institute. Publisher Copyright: {\textcopyright} 2019 The Author(s).",
year = "2020",
month = jan,
doi = "10.1093/mnras/stz3188",
language = "English (US)",
volume = "491",
pages = "3411--3418",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "3",
}