The Type II supernovae 2006V and 2006au: two SN 1987A-like events^⋆,⋆⋆

¹ Department of Astronomy, The Oskar Klein CenterStockholm University, AlbaNova, 10691 Stockholm, Sweden
e-mail: ftadd@astro.su.se
² Affiliated member Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen Ø, Denmark
³ Carnegie Observatories, Las Campanas Observatory, Casilla 601, La Serena, Chile
⁴ Universidad de Chile, Departamento de Astronomía, Casilla 36-D, Santiago, Chile
⁵ Institute for the Physics and Mathematics of the Universe (IPMU), University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, 277-8583 Chiba, Japan
⁶ Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA
⁷ Astrophysics Research Centre, School of Mathematics and Physics, Queen University Belfast, Belfast BT7 1NN, UK
⁸ INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy

Received: 14 September 2011
Accepted: 25 October 2011

Abstract

Context. Supernova 1987A revealed that a blue supergiant (BSG) star can end its life as a core-collapse supernova (SN). SN 1987A and other similar objects exhibit properties that distinguish them from ordinary Type II Plateau (IIP) SNe, whose progenitors are believed to be red supergiants (RSGs). Similarities among 1987A-like events include a long rise to maximum, early luminosity fainter than that of normal Type IIP SNe, and radioactivity acting as the primary source powering the light curves.

Aims. We present and analyze two SNe monitored by the Carnegie Supernova Project that are reminiscent of SN 1987A.

Methods. Optical and near-infrared (NIR) light curves, and optical spectroscopy of SNe 2006V and 2006au are presented. These observations are compared to those of SN 1987A, and are used to estimate properties of their progenitors.

Results. Both objects exhibit a slow rise to maximum and light curve evolution similar to that of SN 1987A. At the earliest epochs, SN 2006au also displays an initial dip which we interpret as the signature of the adiabatic cooling phase that ensues shock break-out. SNe 2006V and 2006au are both found to be bluer, hotter and brighter than SN 1987A. Spectra of SNe 2006V and 2006au are similar to those of SN 1987A and other normal Type II objects, although both consistently exhibit expansion velocities higher than SN 1987A. Semi-analytic models are fit to the UVOIR light curve of each object from which physical properties of the progenitors are estimated. This yields ejecta mass estimates of M_ej ≈ 20 M_⊙, explosion energies of E ≈ 2−3 × 10⁵¹ erg s^-1, and progenitor radii of R ≈ 75−100 R_⊙ for both SNe.

Conclusions. The progenitors of SNe 2006V and 2006au were most likely BSGs with a larger explosion energy as compared to that of SN 1987A.