PS1-10afx at z = 1.388: Pan-STARRS1 discovery of a new type of superluminous supernova

Published

Journal Article

We present the Pan-STARRS1 discovery of PS1-10afx, a unique hydrogen-deficient superluminous supernova (SLSN) at redshift z = 1.388. The light curve peaked at z P1 = 21.7 mag, making PS1-10afx comparable to the most luminous known SNe, with Mu = -22.3 mag. Our extensive optical and near-infrared observations indicate that the bolometric light curve of PS1-10afx rose on the unusually fast timescale of 12 days to the extraordinary peak luminosity of 4.1 × 10 44 erg s -1 (M bol = -22.8 mag) and subsequently faded rapidly. Equally important, the spectral energy distribution is unusually red for an SLSN, with a color temperature of 6800 K near maximum light, in contrast to previous hydrogen-poor SLSNe, which are bright in the ultraviolet (UV). The spectra more closely resemble those of a normal SN Ic than any known SLSN, with a photospheric velocity of 11, 000 km s -1 and evidence for line blanketing in the rest-frame UV. Despite the fast rise, these parameters imply a very large emitting radius (≳ 5 × 10 15 cm). We demonstrate that no existing theoretical model can satisfactorily explain this combination of properties: (1) a nickel-powered light curve cannot match the combination of high peak luminosity with the fast timescale; (2) models powered by the spindown energy of a rapidly rotating magnetar predict significantly hotter and faster ejecta; and (3) models invoking shock breakout through a dense circumstellar medium cannot explain the observed spectra or color evolution. The host galaxy is well detected in pre-explosion imaging with a luminosity near L*, a star formation rate of 15 M yr -1 , and is fairly massive (2 × 10 10 M), with a stellar population age of 10 8 yr, also in contrast to the young dwarf hosts of known hydrogen-poor SLSNe. PS1-10afx is distinct from known examples of SLSNe in its spectra, colors, light-curve shape, and host galaxy properties, suggesting that it resulted from a different channel than other hydrogen-poor SLSNe. © 2013. The American Astronomical Society. All rights reserved.

Full Text

Duke Authors

Cited Authors

  • Chornock, R; Berger, E; Rest, A; Milisavljevic, D; Lunnan, R; Foley, RJ; Soderberg, AM; Smartt, SJ; Burgasser, AJ; Challis, P; Chomiuk, L; Czekala, I; Drout, M; Fong, W; Huber, ME; Kirshner, RP; Leibler, C; McLeod, B; Marion, GH; Narayan, G; Riess, AG; Roth, KC; Sanders, NE; Scolnic, D; Smith, K; Stubbs, CW; Tonry, JL; Valenti, S; Burgett, WS; Chambers, KC; Hodapp, KW; Kaiser, N; Kudritzki, RP; Magnier, EA; Price, PA

Published Date

  • April 20, 2013

Published In

Volume / Issue

  • 767 / 2

Electronic International Standard Serial Number (EISSN)

  • 1538-4357

International Standard Serial Number (ISSN)

  • 0004-637X

Digital Object Identifier (DOI)

  • 10.1088/0004-637X/767/2/162

Citation Source

  • Scopus