Astrophys. J., 883, 120-120 (2019/October-1)
Interaction of SN Ib 2004dk with a previously expelled envelope.
POOLEY D., WHEELER J.C., VINKO J., DWARKADAS V.V., SZALAI T., SILVERMAN J.M., GRIESEL M., McCULLOUGH M., MARION G.H. and MacQUEEN P.
Abstract (from CDS):
The interaction between the expanding supernova (SN) ejecta with the circumstellar material (CSM) that was expelled from the progenitor prior to explosion is a long-sought phenomenon, yet observational evidence is scarce. Here we confirm a new example: SN 2004dk, originally a hydrogen-poor, helium-rich Type Ib SN that reappeared as a strong Hα-emitting point source on narrowband Hαimages. We present follow-up optical spectroscopy that reveals the presence of a broad Hαcomponent with full width at half maximum of ∼ 290 kms–1 in addition to the narrow Hα+[N II] emission features from the host galaxy. Such a broad component is a clear sign of an ejecta-CSM interaction. We also present observations with the XMM-Newton Observatory, the Swift satellite, and the Chandra X-ray Observatory that span 10 days to 15 years after discovery. The detection of strong radio, X-ray, and Hαemission years after explosion allows various constraints to be put on pre-SN mass-loss processes. We present a wind-bubble model in which the CSM is "pre-prepared" by a fast wind interacting with a slow wind. Much of the outer density profile into which the SN explodes corresponds to no steady-state mass-loss process. We estimate that the shell of compressed slow wind material was ejected ∼1400 yr prior to explosion, perhaps during carbon burning, and that the SN shock had swept up about 0.04 M☉ of material. The region emitting the Hαhas a density of order 10–20gcm–3.
© 2019. The American Astronomical Society. All rights reserved.
circumstellar matter - supernovae: individual: 2004dk
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