Ejecta, Rings, and Dust in SN 1987A with JWST MIRI/MRS
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| Format: | Preprint |
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2023
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| author | Jones, O. C. Kavanagh, P. J. Barlow, M. J. Temim, T. Fransson, C. Larsson, J. Blommaert, J. A. D. L. Meixner, M. Lau, R. M. Sargent, B. Bouchet, P. Hjorth, J. Wright, G. S. Coulais, A. Fox, O. D. Gastaud, R. Glasse, A. Habel, N. Hirschauer, A. S. Jaspers, J. Krause, O. Lenkić Nayak, O. Rest, A. Tikkanen, T. Wesson, R. Colina, L. van Dishoeck, E. F. Güdel, M. Henning, Th. Lagage, P. -O. Östlin Ray, T. P. Vandenbussche, B. |
| author_facet | Jones, O. C. Kavanagh, P. J. Barlow, M. J. Temim, T. Fransson, C. Larsson, J. Blommaert, J. A. D. L. Meixner, M. Lau, R. M. Sargent, B. Bouchet, P. Hjorth, J. Wright, G. S. Coulais, A. Fox, O. D. Gastaud, R. Glasse, A. Habel, N. Hirschauer, A. S. Jaspers, J. Krause, O. Lenkić Nayak, O. Rest, A. Tikkanen, T. Wesson, R. Colina, L. van Dishoeck, E. F. Güdel, M. Henning, Th. Lagage, P. -O. Östlin Ray, T. P. Vandenbussche, B. |
| contents | Supernova (SN) 1987A is the nearest supernova in $\sim$400 years. Using the {\em JWST} MIRI Medium Resolution Spectrograph, we spatially resolved the ejecta, equatorial ring (ER) and outer rings in the mid-infrared 12,927 days after the explosion. The spectra are rich in line and dust continuum emission, both in the ejecta and the ring. Broad emission lines (280-380~km~s$^{-1}$ FWHM) seen from all singly-ionized species originate from the expanding ER, with properties consistent with dense post-shock cooling gas. Narrower emission lines (100-170~km~s$^{-1}$ FWHM) are seen from species originating from a more extended lower-density component whose high ionization may have been produced by shocks progressing through the ER, or by the UV radiation pulse associated with the original supernova event. The asymmetric east-west dust emission in the ER has continued to fade, with constant temperature, signifying a reduction in dust mass. Small grains in the ER are preferentially destroyed, with larger grains from the progenitor surviving the transition from SN into SNR. The ER is fit with a single set of optical constants, eliminating the need for a secondary featureless hot dust component. We find several broad ejecta emission lines from [Ne~{\sc ii}], [Ar~{\sc ii}], [Fe~{\sc ii}], and [Ni~{\sc ii}]. With the exception of [Fe~{\sc ii}]~25.99$μ$m, these all originate from the ejecta close to the ring and are likely being excited by X-rays from the interaction. The [Fe~{\sc ii}]~5.34$μ$m to 25.99$μ$m line ratio indicates a temperature of only a few hundred K in the inner core, consistent with being powered by ${}^{44}$Ti decay. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2307_06692 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | Ejecta, Rings, and Dust in SN 1987A with JWST MIRI/MRS Jones, O. C. Kavanagh, P. J. Barlow, M. J. Temim, T. Fransson, C. Larsson, J. Blommaert, J. A. D. L. Meixner, M. Lau, R. M. Sargent, B. Bouchet, P. Hjorth, J. Wright, G. S. Coulais, A. Fox, O. D. Gastaud, R. Glasse, A. Habel, N. Hirschauer, A. S. Jaspers, J. Krause, O. Lenkić Nayak, O. Rest, A. Tikkanen, T. Wesson, R. Colina, L. van Dishoeck, E. F. Güdel, M. Henning, Th. Lagage, P. -O. Östlin Ray, T. P. Vandenbussche, B. High Energy Astrophysical Phenomena Astrophysics of Galaxies Solar and Stellar Astrophysics Supernova (SN) 1987A is the nearest supernova in $\sim$400 years. Using the {\em JWST} MIRI Medium Resolution Spectrograph, we spatially resolved the ejecta, equatorial ring (ER) and outer rings in the mid-infrared 12,927 days after the explosion. The spectra are rich in line and dust continuum emission, both in the ejecta and the ring. Broad emission lines (280-380~km~s$^{-1}$ FWHM) seen from all singly-ionized species originate from the expanding ER, with properties consistent with dense post-shock cooling gas. Narrower emission lines (100-170~km~s$^{-1}$ FWHM) are seen from species originating from a more extended lower-density component whose high ionization may have been produced by shocks progressing through the ER, or by the UV radiation pulse associated with the original supernova event. The asymmetric east-west dust emission in the ER has continued to fade, with constant temperature, signifying a reduction in dust mass. Small grains in the ER are preferentially destroyed, with larger grains from the progenitor surviving the transition from SN into SNR. The ER is fit with a single set of optical constants, eliminating the need for a secondary featureless hot dust component. We find several broad ejecta emission lines from [Ne~{\sc ii}], [Ar~{\sc ii}], [Fe~{\sc ii}], and [Ni~{\sc ii}]. With the exception of [Fe~{\sc ii}]~25.99$μ$m, these all originate from the ejecta close to the ring and are likely being excited by X-rays from the interaction. The [Fe~{\sc ii}]~5.34$μ$m to 25.99$μ$m line ratio indicates a temperature of only a few hundred K in the inner core, consistent with being powered by ${}^{44}$Ti decay. |
| title | Ejecta, Rings, and Dust in SN 1987A with JWST MIRI/MRS |
| topic | High Energy Astrophysical Phenomena Astrophysics of Galaxies Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2307.06692 |