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Evidence for a Pulsar Wind Nebula in the Type Ib Peculiar Supernova SN 2012au

D. MilisavljevicDepartment of Physics and Astronomy, Purdue University, 525 Northwestern Avenue, West Lafayette, IN 47907, USA; [email protected]D. PatnaudeSmithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138, USARoger A. ChevalierDepartment of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904, USAJ. C. RaymondSmithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138, USARobert A. Fesen6127 Wilder Laboratory, Department of Physics and Astronomy, Dartmouth College, Hanover, NH 03755, USAR. MarguttiCenter for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University, Evanston, IL 60208, USABrody ConnerDepartment of Physics and Astronomy, Purdue University, 525 Northwestern Avenue, West Lafayette, IN 47907, USA; [email protected]John BanovetzDepartment of Physics and Astronomy, Purdue University, 525 Northwestern Avenue, West Lafayette, IN 47907, USA; [email protected]

2018en

ABI

Annotatsiya

Abstract We present an optical spectrum of the energetic Type Ib supernova (SN) 2012au obtained at an unprecedented epoch of 6.2 yr after explosion. Forbidden transition emission lines of oxygen and sulfur are detected with expansion velocities of ≈2300 km s −1 . The lack of narrow H Balmer lines suggests that interaction with circumstellar material is not a dominant source of the observed late-time emission. We also present a deep Chandra observation that reveals no X-ray emission down to a luminosity of L X < 2 × 10 38 erg s −1 (0.5–10 keV). Our findings are consistent with the notion that SN 2012au is associated with a diverse subset of SNe, including long-duration gamma-ray burst SNe and superluminous SNe, harboring pulsar/magnetar wind nebulae that influence core-collapse explosion dynamics on a wide range of energy scales. We hypothesize that these systems may all evolve into a similar late-time phase dominated by forbidden oxygen transitions, and predict that emission line widths should remain constant or broaden a few percent per year due to the acceleration of ejecta by the pulsar/magnetar bubble.

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DOI: 10.3847/2041-8213/aadd4e

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