An unusually fast-evolving supernova

Science

Volumn 327, Issue 5961, 2010, Pages 58-60

  Poznanski, Dovi ^a,b   Chornock, Ryan ^a   Nugent, Peter E ^b   Bloom, Joshua S ^a   Filippenko, Alexei V ^a   Ganeshalingam, Mohan ^a   Leonard, Douglas C ^c   Li, Weidong ^a   Thomas, Rollin C ^b  

^a UNIVERSITY OF CALIFORNIA   (United States)

^b LAWRENCE BERKELEY NATIONAL LABORATORY   (United States)

^c SAN DIEGO STATE UNIVERSITY   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

HELIUM;

CARBON; EXTRATERRESTRIAL MATTER; HELIUM; HYDROGEN; IRON; SPECTRUM; SURVEY;

ARTICLE; ASTRONOMY; NONHUMAN; PHOTOMETRY; PRIORITY JOURNAL; SUPERNOVA;

EID: 74849105635     PISSN: 00368075     EISSN: 10959203     Source Type: Journal    
DOI: 10.1126/science.1181709     Document Type: Article

References (26)

1. A. V. Filippenko, Annu. Rev. Astron. Astrophys. 35, 309 (1997).
2. T. Puckett, J. Newton, M. Papenkova, W. D. Li, IAU Circ. 7839, 1 (2002).
3. The blue continuum, in combination with residual host galaxy lines, explains the original erroneous classification of this object as a SN lln on the basis of a noisier spectrum (20).
4. D. A. Howell ef al., Nature 443, 308 (2006).
5. M. Hicken ef al., Astrophys. ]. Lett. 669, L17 (2007).
6. M. Yamanakaefo et al http://arxiv.org/abs/0908.2059 (2009).
7. A. Fisher, D. Branch, P. Nugent, E. Baron, Astrophys. J. Lett 481, L89 (1997).
8. W. D. Arnett, Astrophys. J. 253, 785 (1982).
9. P. G. Sutherland, J.C. Wheeler, Astrophys.J. 280, 282(1984).
10. L. Bildsten, K. J. Shen, N. N. Weinberg, G. Nelemans, Astrophys. J. Lett. 662, L95 (2007).
11. K. J. Shen, L. Bildsten, Astrophys. J. 699, 1365 (2009).
12. H. B. Perets et al, http://arxiv.org/abs/0906.2003 (2009).
13. S. Valenti et al., Nature 459, 674 (2009).
14. R. J. Foley, et al., Astron. J. 138, 376 (2009).
15. If our interpretation is correct, it would not be too surprising that the first SN .la found would be unusually luminous, because such an object would be easier to find and to recognize as such.
16. D. Kasen, Astrophys. J. 649, 939 (2006).
17. P. Nugent et al, Astrophys. J. 645, 841 (2006).
18. X. Wang et al, Astrophys. J. Lett. 699, L139 (2009).
19. Poisson statistics allow fractions in the range from 0.7 to 11% (1oσ).
20. T. Matheson, P. Berlind, IAU Cire. 7844, 5 (2002).
21. M. W. Richmond, et al., Astron. J. 111, 327 (1996).
22. K. Krisciunas, et al., http://arxiv.org/abs/0908.1918 (2009).
23. A. Fassia et al., Mon. Not R. Astron. Soc 318, 1093 (2000).
24. X. Wang et al, Astrophys. J. 697, 380 (2009).
25. M. Modjaz et al., Astrophys. J. 702, 226 (2009).
26. We thank L. Bildsten for valuable insights into the SN .la model; A. Gal-Yam, D. Kasen, D. Maoz, T. Matheson, P. Mazzali, E. Ofek, E. Quataert, K. Shen, and N. Smith for useful discussions; R. Foley for reducing the Lick 3-m spectrum of SN 2002bj; and A. A. Miller and A. Merritt for the DeepSky analysis. A. V. F.'s group has been supported by NSF grants AST-0607485 and AST0908886, by U. S. Department of Energy grants DE-FC0206ER41453 (SciDAC) and DE-FG02-08ER41563, and by the TABASGO Foundation. The Katzman Automated Imaging Telescope and its ongoing operation were made possible by donations from Sun Microsystems, the Hewlett-Packard Company, AutoScope Corporation, the Lick Observatory, NSF, the University of California, the Sylvia & Jim Katzman Foundation, and the TABASGO Foundation. Some of the data presented here were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. We thank the staffs at the Lick and Keck observatories for their assistance.