A rapidly spinning supermassive black hole at the centre of NGC 1365

G. Risaliti (), F. A. Harrison (), K. K. Madsen, D. J. Walton, S. E. Boggs, F. E. Christensen, W. W. Craig, B. W. Grefenstette, C. J. Hailey, E. Nardini, Daniel Stern and W. W. Zhang
Additional contact information
G. Risaliti: INAF—Osservatoria Astrofisico di Arcetri, Largo Enrico Fermi 5, 50125 Firenze, Italy
F. A. Harrison: Cahill Center for Astrophysics, 1216 East California Boulevard, California Institute of Technology
K. K. Madsen: Cahill Center for Astrophysics, 1216 East California Boulevard, California Institute of Technology
D. J. Walton: Cahill Center for Astrophysics, 1216 East California Boulevard, California Institute of Technology
S. E. Boggs: Space Science Laboratory, University of California
F. E. Christensen: DTU Space—National Space Institute, Technical University of Denmark, Elektrovej 327, 2800 Lyngby, Denmark
W. W. Craig: DTU Space—National Space Institute, Technical University of Denmark, Elektrovej 327, 2800 Lyngby, Denmark
B. W. Grefenstette: Cahill Center for Astrophysics, 1216 East California Boulevard, California Institute of Technology
C. J. Hailey: Columbia Astrophysics Laboratory, Columbia University
E. Nardini: Astrophysics Group, School of Physical and Geographical Sciences, Keele University, Keele, Staffordshire ST5 5BG, UK
Daniel Stern: Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California 91109, USA
W. W. Zhang: NASA Goddard Space Flight Center

Nature, 2013, vol. 494, issue 7438, 449-451

Abstract: Two models (relativistic disk reflection and absorption-dominated) can explain the pattern of X-ray emission from the galaxy NGC 1365, but here reflection arising close to a rapidly spinning black hole is shown to be the correct model.

Date: 2013
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DOI: 10.1038/nature11938

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