SN2010ay is a luminous and broad-lined type Ic supernova within a low-metallicity host galaxy

N. E. Sanders, A. M. Soderberg, S. Valenti, R. J. Foley, R. Chornock, L. Chomiuk, E. Berger, S. Smartt, K. Hurley, S. D. Barthelmy, E. M. Levesque, G. Narayan, M. T. Botticella, M. S. Briggs, V. Connaughton, Y. Terada, N. Gehrels, S. Golenetskii, E. Mazets, T. ClineA. Von Kienlin, W. Boynton, K. C. Chambers, T. Grav, J. N. Heasley, K. W. Hodapp, R. Jedicke, N. Kaiser, R. P. Kirshner, R. P. Kudritzki, G. A. Luppino, R. H. Lupton, E. A. Magnier, D. G. Monet, J. S. Morgan, P. M. Onaka, P. A. Price, C. W. Stubbs, J. L. Tonry, R. J. Wainscoat, M. F. Waterson

Research output: Contribution to journalArticlepeer-review

Abstract

We report on our serendipitous pre-discovery detection and follow-up observations of the broad-lined TypeIc supernova (SNIc) 2010ay at z = 0.067 imaged by the Pan-STARRS1 3π survey just ∼4 days after explosion. The supernova (SN) had a peak luminosity, MR ≈ -20.2 mag, significantly more luminous than known GRB-SNe and one of the most luminous SNeIb/c ever discovered. The absorption velocity of SN2010ay is vSi 19 × 103kms-1 at ∼40 days after explosion, 2-5 times higher than other broad-lined SNe and similar to the GRB-SN2010bh at comparable epochs. Moreover, the velocity declines 2 times slower than other SNeIc-BL and GRB-SNe. Assuming that the optical emission is powered by radioactive decay, the peak magnitude implies the synthesis of an unusually large mass of 56Ni, MNi = 0.9 M. Applying scaling relations to the light curve, we estimate a total ejecta mass, M ej ≈ 4.7 M, and total kinetic energy, E K ≈ 11 × 1051 erg. The ratio of MNi to Mej is ∼ 2 times as large for SN2010ay as typical GRB-SNe and may suggest an additional energy reservoir. The metallicity (log (O/H) PP04 + 12 = 8.19) of the explosion site within the host galaxy places SN2010ay in the low-metallicity regime populated by GRB-SNe, and ∼0.5(0.2)dex lower than that typically measured for the host environments of normal (broad-lined) SNe Ic. We constrain any gamma-ray emission with E γ ≲ 6 × 1048erg (25-150keV), and our deep radio follow-up observations with the Expanded Very Large Array rule out relativistic ejecta with energy E ≳ 1048erg. We therefore rule out the association of a relativistic outflow like those that accompanied SN1998bw and traditional long-duration gamma-ray bursts (GRBs), but we place less-stringent constraints on a weak afterglow like that seen from XRF060218. If this SN did not harbor a GRB, these observations challenge the importance of progenitor metallicity for the production of relativistic ejecta and suggest that other parameters also play a key role.

Original languageEnglish (US)
Article number184
JournalAstrophysical Journal
Volume756
Issue number2
DOIs
StatePublished - Sep 10 2012

Keywords

  • gamma-ray burst: general
  • supernovae: general
  • supernovae: individual (2010ay)

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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