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Detection of stellar light from quasar host galaxies at redshifts above 6.
Ding, Xuheng; Onoue, Masafusa; Silverman, John D; Matsuoka, Yoshiki; Izumi, Takuma; Strauss, Michael A; Jahnke, Knud; Phillips, Camryn L; Li, Junyao; Volonteri, Marta; Haiman, Zoltan; Andika, Irham Taufik; Aoki, Kentaro; Baba, Shunsuke; Bieri, Rebekka; Bosman, Sarah E I; Bottrell, Connor; Eilers, Anna-Christina; Fujimoto, Seiji; Habouzit, Melanie; Imanishi, Masatoshi; Inayoshi, Kohei; Iwasawa, Kazushi; Kashikawa, Nobunari; Kawaguchi, Toshihiro; Kohno, Kotaro; Lee, Chien-Hsiu; Lupi, Alessandro; Lyu, Jianwei; Nagao, Tohru; Overzier, Roderik; Schindler, Jan-Torge; Schramm, Malte; Shimasaku, Kazuhiro; Toba, Yoshiki; Trakhtenbrot, Benny; Trebitsch, Maxime; Treu, Tommaso; Umehata, Hideki; Venemans, Bram P; Vestergaard, Marianne; Walter, Fabian; Wang, Feige; Yang, Jinyi.
Afiliação
  • Ding X; Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), The University of Tokyo, Chiba, Japan. xuheng.ding@ipmu.jp.
  • Onoue M; Center for Data-Driven Discovery, Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Japan. xuheng.ding@ipmu.jp.
  • Silverman JD; Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), The University of Tokyo, Chiba, Japan. onoue@pku.edu.cn.
  • Matsuoka Y; Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing, China. onoue@pku.edu.cn.
  • Izumi T; Max Planck Institute for Astronomy, Heidelberg, Germany. onoue@pku.edu.cn.
  • Strauss MA; Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), The University of Tokyo, Chiba, Japan.
  • Jahnke K; Center for Data-Driven Discovery, Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Japan.
  • Phillips CL; Department of Astronomy, School of Science, The University of Tokyo, Bunkyo-ku, Japan.
  • Li J; Research Center for Space and Cosmic Evolution, Ehime University, Matsuyama, Japan.
  • Volonteri M; National Astronomical Observatory of Japan, Osawa, Mitaka, Japan.
  • Haiman Z; Department of Physics, Graduate School of Science, Tokyo Metropolitan University, Hachioji, Japan.
  • Andika IT; Department of Astrophysical Sciences, Princeton University, Princeton, NJ, USA.
  • Aoki K; Max Planck Institute for Astronomy, Heidelberg, Germany.
  • Baba S; Department of Astrophysical Sciences, Princeton University, Princeton, NJ, USA.
  • Bieri R; Department of Astronomy, University of Illinois at Urbana-Champaign, Urbana, IL, USA.
  • Bosman SEI; Institute of Astrophysics of Paris, CNRS, Sorbonne Université, Paris, France.
  • Bottrell C; Department of Astronomy, Columbia University, New York, NY, USA.
  • Eilers AC; Department of Physics, Columbia University, New York, NY, USA.
  • Fujimoto S; Physics Department, Technical University of München, Garching bei München, Germany.
  • Habouzit M; Max Planck Institute for Astrophysics, Garching bei München, Germany.
  • Imanishi M; Subaru Telescope, National Astronomical Observatory of Japan, Hilo, HI, USA.
  • Inayoshi K; Graduate School of Science and Engineering, Kagoshima University, Kagoshima, Japan.
  • Iwasawa K; Institute for Computational Science, University of Zurich, Zürich, Switzerland.
  • Kashikawa N; Max Planck Institute for Astronomy, Heidelberg, Germany.
  • Kawaguchi T; Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), The University of Tokyo, Chiba, Japan.
  • Kohno K; Center for Data-Driven Discovery, Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Japan.
  • Lee CH; MIT Kavli Institute for Astrophysics and Space Research, Cambridge, MA, USA.
  • Lupi A; Department of Astronomy, The University of Texas at Austin, Austin, TX, USA.
  • Lyu J; Max Planck Institute for Astronomy, Heidelberg, Germany.
  • Nagao T; Centre for Astronomy at the University of Heidelberg (ITA), Heidelberg, Germany.
  • Overzier R; National Astronomical Observatory of Japan, Osawa, Mitaka, Japan.
  • Schindler JT; Department of Astronomy, School of Science, Graduate University for Advanced Studies (SOKENDAI), Mitaka, Japan.
  • Schramm M; Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing, China.
  • Shimasaku K; Institute of Sciences of the Cosmos (ICCUB), University of Barcelona (IEEC-UB), Barcelona, Spain.
  • Toba Y; ICREA, Barcelona, Spain.
  • Trakhtenbrot B; Department of Astronomy, School of Science, The University of Tokyo, Bunkyo-ku, Japan.
  • Trebitsch M; Research Center for the Early Universe, Graduate School of Science, The University of Tokyo, Bunkyo-ku, Japan.
  • Treu T; Department of Economics, Management and Information Science, Onomichi City University, Onomichi, Japan.
  • Umehata H; Research Center for the Early Universe, Graduate School of Science, The University of Tokyo, Bunkyo-ku, Japan.
  • Venemans BP; Institute of Astronomy, Graduate School of Science, The University of Tokyo, Mitaka, Tokyo, Japan.
  • Vestergaard M; W. M. Keck Observatory, Kamuela, HI, USA.
  • Walter F; 'G. Occhialini' Physics Department, University of Studi di Milano-Bicocca, Milano, Italy.
  • Wang F; Steward Observatory, University of Arizona, Tucson, AZ, USA.
  • Yang J; Research Center for Space and Cosmic Evolution, Ehime University, Matsuyama, Japan.
Nature ; 621(7977): 51-55, 2023 Sep.
Article em En | MEDLINE | ID: mdl-37380029
ABSTRACT
The detection of starlight from the host galaxies of quasars during the reionization epoch (z > 6) has been elusive, even with deep Hubble Space Telescope observations1,2. The current highest redshift quasar host detected3, at z = 4.5, required the magnifying effect of a foreground lensing galaxy. Low-luminosity quasars4-6 from the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP)7 mitigate the challenge of detecting their underlying, previously undetected host galaxies. Here we report rest-frame optical images and spectroscopy of two HSC-SSP quasars at z > 6 with the JWST. Using near-infrared camera imaging at 3.6 and 1.5 µm and subtracting the light from the unresolved quasars, we find that the host galaxies are massive (stellar masses of 13 × and 3.4 × 1010 M☉, respectively), compact and disc-like. Near-infrared spectroscopy at medium resolution shows stellar absorption lines in the more massive quasar, confirming the detection of the host. Velocity-broadened gas in the vicinity of these quasars enables measurements of their black hole masses (1.4 × 109 and 2.0 × 108 M☉, respectively). Their location in the black hole mass-stellar mass plane is consistent with the distribution at low redshift, suggesting that the relation between black holes and their host galaxies was already in place less than a billion years after the Big Bang.
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Texto completo: 1 Base de dados: MEDLINE Idioma: En Ano de publicação: 2023 Tipo de documento: Article
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Texto completo: 1 Base de dados: MEDLINE Idioma: En Ano de publicação: 2023 Tipo de documento: Article