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

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. © 2012 The American Astronomical Society. All rights reserved.