Hydrogen-poor superluminous stellar explosions

R. M. Quimby (), S. R. Kulkarni, M. M. Kasliwal, A. Gal-Yam, I. Arcavi, M. Sullivan, P. Nugent, R. Thomas, D. A. Howell, E. Nakar, L. Bildsten, C. Theissen, N. M. Law, R. Dekany, G. Rahmer, D. Hale, R. Smith, E. O. Ofek, J. Zolkower, V. Velur, R. Walters, J. Henning, K. Bui, D. McKenna, D. Poznanski, S. B. Cenko and D. Levitan
Additional contact information
R. M. Quimby: Cahill Center for Astrophysics 249-17, California Institute of Technology
S. R. Kulkarni: Cahill Center for Astrophysics 249-17, California Institute of Technology
M. M. Kasliwal: Cahill Center for Astrophysics 249-17, California Institute of Technology
A. Gal-Yam: Benoziyo Center for Astrophysics, Faculty of Physics, Weizmann Institute of Science, 76100 Rehovot, Israel
I. Arcavi: Benoziyo Center for Astrophysics, Faculty of Physics, Weizmann Institute of Science, 76100 Rehovot, Israel
M. Sullivan: University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK
P. Nugent: Lawrence Berkeley National Laboratory, 1 Cyclotron Road
R. Thomas: Lawrence Berkeley National Laboratory, 1 Cyclotron Road
D. A. Howell: Las Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Goleta, California 93117, USA
E. Nakar: Raymond and Beverly Sackler School of Physics & Astronomy, Tel Aviv University, Tel Aviv 69978, Israel
L. Bildsten: Las Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Goleta, California 93117, USA
C. Theissen: University of California, San Diego, 9500 Gilman Drive, La Jolla, California 92093, USA
N. M. Law: Cahill Center for Astrophysics 249-17, California Institute of Technology
R. Dekany: Caltech Optical Observatories, California Institute of Technology
G. Rahmer: Caltech Optical Observatories, California Institute of Technology
D. Hale: Caltech Optical Observatories, California Institute of Technology
R. Smith: Caltech Optical Observatories, California Institute of Technology
E. O. Ofek: Caltech Optical Observatories, California Institute of Technology
J. Zolkower: Caltech Optical Observatories, California Institute of Technology
V. Velur: Caltech Optical Observatories, California Institute of Technology
R. Walters: Caltech Optical Observatories, California Institute of Technology
J. Henning: Caltech Optical Observatories, California Institute of Technology
K. Bui: Caltech Optical Observatories, California Institute of Technology
D. McKenna: Caltech Optical Observatories, California Institute of Technology
D. Poznanski: Lawrence Berkeley National Laboratory, 1 Cyclotron Road
S. B. Cenko: University of California, Berkeley, 601 Campbell Hall, Berkeley, California 94720, USA
D. Levitan: California Institute of Technology

Nature, 2011, vol. 474, issue 7352, 487-489

Abstract: A new class of supernovae In all known supernovae, the radiation they emit comes from internal energy deposited in the outflowing ejecta by one or more processes: radioactive decay of freshly synthesized elements, stored heat deposited by the explosion shock in the envelope of a supergiant star, or interaction between the debris and slowly moving, hydrogen-rich circumstellar material. Quimby et al. report observations of a class of luminous supernovae whose properties cannot be explained by any of these processes. They are about ten times brighter than any type Ia supernova and emit significant ultraviolet flux for extended periods. They can be observed out to redshifts z > 4. These long-lived events, which light up their surroundings, may enable high-resolution spectroscopy to probe distant star-forming regions and primitive galaxies.

Date: 2011
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DOI: 10.1038/nature10095

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