Constraining Dust Formation in the Superluminous Supernova 2017gci with JWST Observations
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| Autores principales: | , , , , , , , , , , , , , |
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| Formato: | Preprint |
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2024
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| author | Gomez, Sebastian Temim, Tea Fox, Ori Villar, V. Ashley Shahbandeh, Melissa Ashall, Chris Jencson, Jacob E. Langeroodi, Danial De Looze, Ilse Milisavljevic, Dan Pierel, Justin Rest, Armin Szalai, Tamás Tinyanont, Samaporn |
| author_facet | Gomez, Sebastian Temim, Tea Fox, Ori Villar, V. Ashley Shahbandeh, Melissa Ashall, Chris Jencson, Jacob E. Langeroodi, Danial De Looze, Ilse Milisavljevic, Dan Pierel, Justin Rest, Armin Szalai, Tamás Tinyanont, Samaporn |
| contents | We present JWST/MIRI observations of the Type I superluminous supernova (SLSN) 2017gci taken over 2000 rest-frame days after the supernova (SN) exploded, which represent the latest phase images taken of any known SLSN. We find that archival \WISE detections of SN\,2017gci taken 70 to 200 days after explosion are most likely explained by an IR dust echo from a $\sim 3 \times 10^{-4}$ M$_\odot$ shell of pre-existing dust, as opposed to freshly-formed dust. New JWST observations reveal IR emission in the field of SN\,2017gci, which we determine is most likely dominated by the host galaxy of the SN, based on the expected flux of the galaxy and the measurable separation between said emission and the location of the SN. Based on models for IR emission of carbonate dust, we place a $3σ$ upper limit of $0.83$ M$_\odot$ of dust formed in SN\,2017gci, with a lowest $1σ$ limit of $0.44$ M$_\odot$. Infrared (IR) detections of other SLSNe have suggested that SLSNe could be among the most efficient dust producers in the universe. Our results suggest that SLSNe do not necessarily form more dust than other types of SNe, but instead might have a more accelerated dust formation process. More IR observations of a larger sample of SLSNe will be required to determine how efficient dust production is in SLSNe. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2408_15397 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Constraining Dust Formation in the Superluminous Supernova 2017gci with JWST Observations Gomez, Sebastian Temim, Tea Fox, Ori Villar, V. Ashley Shahbandeh, Melissa Ashall, Chris Jencson, Jacob E. Langeroodi, Danial De Looze, Ilse Milisavljevic, Dan Pierel, Justin Rest, Armin Szalai, Tamás Tinyanont, Samaporn High Energy Astrophysical Phenomena We present JWST/MIRI observations of the Type I superluminous supernova (SLSN) 2017gci taken over 2000 rest-frame days after the supernova (SN) exploded, which represent the latest phase images taken of any known SLSN. We find that archival \WISE detections of SN\,2017gci taken 70 to 200 days after explosion are most likely explained by an IR dust echo from a $\sim 3 \times 10^{-4}$ M$_\odot$ shell of pre-existing dust, as opposed to freshly-formed dust. New JWST observations reveal IR emission in the field of SN\,2017gci, which we determine is most likely dominated by the host galaxy of the SN, based on the expected flux of the galaxy and the measurable separation between said emission and the location of the SN. Based on models for IR emission of carbonate dust, we place a $3σ$ upper limit of $0.83$ M$_\odot$ of dust formed in SN\,2017gci, with a lowest $1σ$ limit of $0.44$ M$_\odot$. Infrared (IR) detections of other SLSNe have suggested that SLSNe could be among the most efficient dust producers in the universe. Our results suggest that SLSNe do not necessarily form more dust than other types of SNe, but instead might have a more accelerated dust formation process. More IR observations of a larger sample of SLSNe will be required to determine how efficient dust production is in SLSNe. |
| title | Constraining Dust Formation in the Superluminous Supernova 2017gci with JWST Observations |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2408.15397 |