PS1-10bzj: A fast, hydrogen-poor superluminous supernova in a metal-poor host galaxy

R. Lunnan, R. Chornock, E. Berger, D. Milisavljevic, M. Drout, N. E. Sanders, P. M. Challis, I. Czekala, R. J. Foley, W. Fong, M. E. Huber, R. P. Kirshner, C. Leibler, G. H. Marion, M. McCrum, G. Narayan, A. Rest, K. C. Roth, D. Scolnic, S. J. SmarttK. Smith, A. M. Soderberg, C. W. Stubbs, J. L. Tonry, W. S. Burgett, K. C. Chambers, R. P. Kudritzki, E. A. Magnier, P. A. Price

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We present observations and analysis of PS1-10bzj, a superluminous supernova (SLSN) discovered in the Pan-STARRS Medium Deep Survey at a redshift z = 0.650. Spectroscopically, PS1-10bzj is similar to the hydrogen-poor SLSNe 2005ap and SCP 06F6, though with a steeper rise and lower peak luminosity (Mbol ≃ -21.4 mag) than previous events. We construct a bolometric light curve, and show that while PS1-10bzj's energetics were less extreme than previous events, its luminosity still cannot be explained by radioactive nickel decay alone. We explore both a magnetar spin-down and circumstellar interaction scenario and find that either can fit the data. PS1-10bzj is located in the Extended Chandra Deep Field South and the host galaxy is imaged in a number of surveys, including with the Hubble Space Telescope. The host is a compact dwarf galaxy (MB ≈ -18 mag, diameter ≲ 800 pc), with a low stellar mass (M* ≈ 2.4 × 107 Modot;), young stellar population (τ* ≈ 5 Myr), and a star formation rate of ∼2-3 Modot;yr-1. The specific star formation rate is the highest seen in an SLSN host so far (∼100 Gyr-1). We detect the [O III] λ4363 line, and find a low metallicity: 12 + (O/H) = 7.8 ± 0.2 (≃ 0.1 Zodot;). Together, this indicates that at least some of the progenitors of SLSNe come from young, low-metallicity populations.

Original languageEnglish (US)
Article number97
JournalAstrophysical Journal
Issue number2
StatePublished - Jul 10 2013

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science


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