Luminous supernovae

Science

Volumn 337, Issue 6097, 2012, Pages 927-932

  Gal Yam, Avishay ^a  

^a WEIZMANN INSTITUTE OF SCIENCE   (Israel)

Author keywords

[No Author keywords available]

Indexed keywords

HELIUM; HYDROGEN; IRON; MAGNESIUM; NICKEL; OXYGEN; SILICON; SULFUR;

EMISSION; EXPLOSION; GEOACCUMULATION; HYDROGEN; LUMINESCENCE; RADIOACTIVITY;

ASTRONOMY; COSMOLOGICAL PHENOMENA; ENVIRONMENTAL RADIOACTIVITY; IONIZING RADIATION; LIGHT RELATED PHENOMENA; LUMINANCE; LUMINOUS SUPERNOVAE; PHOTON; PRIORITY JOURNAL; REVIEW; SHOCK WAVE; TELESCOPE;

EID: 84865289204     PISSN: 00368075     EISSN: 10959203     Source Type: Journal    
DOI: 10.1126/science.1203601     Document Type: Review

References (81)

1. A. V. Filippenko, Annu. Rev. Astron. Astrophys. 35, 309 (1997).
2. Even the brightest SNe associated with cosmological gamma-ray bursts (e.g., the nickel-rich SN 1998bw) fall well below our SLSN threshold.
3. J. D. Neill et al., Astrophys. J. 727, 15 (2011).
4. R. M. Quimby et al., Nature 474, 487 (2011).
5. Possible early detections of SLSNe by these surveys and their modern counterparts are discussed in text S2.
6. R. Knop et al., IAU Circular 7128 (1999).
7. A. Gal-Yam et al., Nature 462, 624 (2009).
8. P. Nugent et al., IAU Circular 7133 (1999).
9. The study of the peculiar SN 1997cy (72) was perhaps the first modern study of a supernova that was substantially more luminous than the norm. The absolute peak magnitude of this event (-20.1 mag), as well as that of similar objects detected since [e.g., SN 2002ic (73)], falls below our fiducial limit defined above, and thus we do not discuss them here.
10. R. M. Quimby, thesis, University of Texas (2006).
11. R. M. Quimby et al., Astrophys. J. 668, L99 (2007).
12. N. Smith et al., Astrophys. J. 666, 1116 (2007).
13. E. O. Ofek et al., Astrophys. J. 659, L13 (2007).
14. A. Gal-Yam, P. Mazzali, http://arxiv.org/abs/1103.5165 (2011).
15. D. R. Young et al., Astron. Astrophys. 489, 359 (2008).
16. I. Arcavi et al., Astrophys. J. 721, 777 (2010).
17. W. D. Arnett, Astrophys. J. 253, 785 (1982).
18. T. Moriya, N. Tominaga, M. Tanaka, K. Maeda, K. Nomoto, Astrophys. J. 717, L83 (2010).
19. K. Hatano et al., Bull. Am. Astron. Soc. 33, 838 (2001).
20. A. V. Filippenko, W. D. Li, R. R. Treffers, M. Modjaz, in Small Telescope Astronomy on Global Scales, IAU Colloquium 183, B. Paczynski, W.-P. Chen, C. Lemme, Eds. (Astronomical Society of the Pacific, San Francisco, 2001), pp. 121-130.
21. J. Kodros et al., Central Bureau Electronic Telegrams 2461 (2010).
22. J. Vinko, J. C. Wheeler, E. Chatzopoulos, G. H. Marion, J. Caldwell, Central Bureau Electronic Telegrams 2476 (2010).
23. A. Gal-Yam, 2011, Presentation at the Stockholm "Explosive ideas about massive stars" meeting, http://explosive2011.astro.su.se/Talks- slides/Gal-Yam-20110810.pdf.
24. S. Smartt, 2011, Presentation at the Stockholm "Explosive ideas about massive stars" meeting, http://explosive2011.astro.su.se/Talks- slides/Smartt-20110813.pdf.
25. D. R. Young et al., Astron. Astrophys. 512, A70 (2010).
26. H. Umeda, K. Nomoto, Astrophys. J. 673, 1014 (2008).
27. A. Heger, S. E. Woosley, Astrophys. J. 567, 532 (2002).
28. R. Waldman, Astrophys. J. 685, 1103 (2008).
29. G. Rakavy, G. Shaviv, Astrophys. J. 148, 803 (1967).
30. Z. Barkat, G. Rakavy, N. Sack, Phys. Rev. Lett. 18, 379 (1967).
31. J. R. Bond, W. D. Arnett, B. J. Carr, Astrophys. J. 280, 825 (1984).
32. E. Scannapieco, P. Madau, S. Woosley, A. Heger, A. Ferrara, Astrophys. J. 633, 1031 (2005).
33. T. Yoshida, H. Umeda, Mon. Not. R. Astron. Soc. 412, L78 (2011).
34. ⊙) explode as pair-instability SNe at SMC- or LMC-like metallicities, although they may have to be tweaked to explain the lack of hydrogen in observed SLSN-R spectra.
35. This effective edge does not necessarily coincide with the physical edge of the star, which we define as the radius inside which material is gravitationally bound to the star.
36. S. Gezari et al., Astrophys. J. 690, 1313 (2009).
37. N. Smith, R. McCray, Astrophys. J. 671, L17 (2007).
38. A. A. Miller et al., Astrophys. J. 690, 1303 (2009).
39. E. O. Ofek et al., Astrophys. J. 724, 1396 (2010).
40. R. A. Chevalier, C. M. Irwin, Astrophys. J. 729, L6 (2011).
41. T. J. Moriya, N. Tominaga, http://arxiv.org/abs/1110.3807 (2011).
42. G. Svirski, E. Nakar, R. Sari, http://arxiv.org/abs/1202.3437 (2012).
43. There is no conflict between this process (converting kinetic energy to radiation) and the previous one (converting shock energy stored as internal heat energy into radiation) and both can contribute in any given object, although there is debate about which one is dominant for particular cases.
44. N. Smith et al., Astrophys. J. 686, 467 (2008).
45. A. Rest et al., Astrophys. J. 729, 88 (2011).
46. S. E. Woosley, S. Blinnikov, A. Heger, Nature 450, 390 (2007).
47. S. E. Woosley, Astrophys. J. 719, L204 (2010).
48. D. Kasen, L. Bildsten, Astrophys. J. 717, 245 (2010).
49. A. I. MacFadyen, S. E. Woosley, Astrophys. J. 524, 262 (1999).
50. T. R. Young, D. Smith, T. A. Johnson, Astrophys. J. 625, L87 (2005).
51. R. M. Humphreys, K. Davidson, Proc. Astron. Soc. Pac. 106, 1025 (1994).
52. A similar relation has been established in the case of a lower-luminosity SN IIn [SN 2005 gl (75, 76)].
53. A. J. Drake et al., Astrophys. J. 718, L127 (2010).
54. R. Stoll et al., Astrophys. J. 730, 34 (2011).
55. N. Smith, R. Chornock, J. M. Silverman, A. V. Filippenko, R. J. Foley, Astrophys. J. 709, 856 (2010).
56. M. Kiewe et al., Astrophys. J. 744, 10 (2012).
57. E. Chatzopoulos et al., Astrophys. J. 729, 143 (2011).
58. A. J. Drake et al., Astrophys. J. 735, 106 (2011).
59. K. Barbary et al., Astrophys. J. 690, 1358 (2009).
60. A. Pastorello et al., Astrophys. J. 724, L16 (2010).
61. D. N. Sauer et al., Mon. Not. R. Astron. Soc. 369, 1939 (2006).
62. P. A. Mazzali et al., Astrophys. J. 670, 592 (2007).
63. P. A. Mazzali, I. Maurer, S. Valenti, R. Kotak, D. Hunter, Mon. Not. R. Astron. Soc. 408, 87 (2010).
64. H. B. Perets et al., Nature 465, 322 (2010).
65. M. R. Drout et al., Astrophys. J. 741, 97 (2011).
66. N. E. Sanders et al., http://arxiv.org/abs/1110.2363 (2011).
67. A. Corsi et al., http://arxiv.org/abs/1110.5618 (2011).
68. L. Chomiuk et al., http://arxiv.org/abs/1107.3552 (2011).
69. G. Leloudas et al., http://arxiv.org/abs/1201.5393 (2012).
70. P. Podsiadlowski, P. A. Mazzali, K. Nomoto, D. Lazzati, E. Cappellaro, Astrophys. J. 607, L17 (2004).
71. D. Guetta, M. Della Valle, Astrophys. J. 657, L73 (2007).
72. L. M. Germany, D. J. Reiss, E. M. Sadler, B. P. Schmidt, C. W. Stubbs, Astrophys. J. 533, 320 (2000).
73. M. Hamuy et al., Nature 424, 651 (2003).
74. N. Langer et al., Astron. Astrophys. 475, L19 (2007).
75. A. Gal-Yam et al., Astrophys. J. 656, 372 (2007).
76. A. Gal-Yam, D. C. Leonard, Nature 458, 865 (2009).
77. I. Agnoletto et al., Astrophys. J. 691, 1348 (2009).
78. I. Arcavi et al., Astrophys. J. 742, L18 (2011).
79. D. C. Leonard et al., Proc. Astron. Soc. Pac. 114, 35 (2002).
80. See text S3 for additional details.
81. O. Yaron, A. Gal-Yam, http://arxiv.org/abs/1204.1891 (2012).