Evidence for late-time dust formation in the ejecta of supernova SN 1995N from emission-line asymmetries

• Published in: Monthly notices of the Royal Astronomical Society Vol. 525; no. 4; pp. 4928 - 4941
• Main Authors: Wesson, R, Bevan, A M, Barlow, M J, De Looze, I, Matsuura, M, Clayton, G, Andrews, J
• Format: Journal Article
• Language: English
• Published: Oxford University Press 11.09.2023
• Subjects: supernovae: individual: SN 1995N; (ISM) dust, extinction; supernovae: general; radiative transfer
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/stad2505

ABSTRACT We present a study of the dust associated with the core-collapse supernova SN 1995N. Infrared emission detected 14–15 yr after the explosion was previously attributed to thermally echoing circumstellar material (CSM) associated with the supernova (SN) progenitor. We argue that this late-time emission is unlikely to be an echo, and is more plausibly explained by newly formed dust in the SN ejecta, indirectly heated by the interaction between the ejecta and the CSM. Further evidence in support of this scenario comes from emission-line profiles in spectra obtained 22 yr after the explosion; these are asymmetric, showing greater attenuation on the red wing, consistent with absorption by dust within the expanding ejecta. The spectral energy distribution and emission-line profiles at epochs later than ∼5000 d are both consistent with the presence of about 0.4 M⊙ of amorphous carbon dust. The onset of dust formation is apparent in archival optical spectra, taken between 700 and 1700 d after the assumed explosion date. As this is considerably later than most other instances where the onset of dust formation has been detected, we argue that the explosion date must be later than previously assumed.