Nebular spectroscopy of the nearby type IIb supernova 2011dh

Abstract

We present nebular spectra of the nearby Type IIb supernova (SN) 2011dh taken between 201 and 678 days after core collapse. At these late times, SN 2011dh exhibits strong emission lines including a very broad and persistent Hα feature. New models of the nebular spectra confirm that the progenitor of SN 2011dh was a low-mass giant (M ~ 13 - 15 M_sun) that ejected ~0.07 M_sun of 56Ni and ~0.27 M_sun of oxygen at the time of explosion, consistent with the recent disappearance of a candidate yellow supergiant progenitor. We show that light from the SN location is dominated by the fading SN at very late times (~2 yr) and not, for example, by a binary companion or a background source. We present evidence for interaction between the expanding SN blastwave and a circumstellar medium at late times and show that the SN is likely powered by positron deposition by ~1 yr after explosion. We also examine the geometry of the ejecta and show that SN 2011dh's nebular line profiles indicate a globally spherical explosion with aspherical components or clumps.

13 pages, 7 figures; published in MNRAS

References in corpus (8)

• Asphericity in Supernova Explosions from Late-Time Spectroscopy
• Optical and near-infrared observations of SN 2011dh - The first 100 days
• Double-peaked Oxygen Lines Are not Rare in Nebular Spectra of Core-Collapse Supernovae
• The Progenitor of Supernova 2011dh Has Vanished
• Late-Time Circumstellar Interaction in a Spitzer Selected Sample of Type IIn Supernovae
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• Type IIb Supernova SN 2011dh: Spectra and Photometry from the Ultraviolet to the Near-Infrared
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