Mid-infrared Dust Evolution and Late-time Circumstellar Medium Interaction in SN 2017eaw

Pearson, J; Subrayan, B; Sand, DJ; Andrews, JE; Beasor, ER; Bostroem, KA; Dong 董, Y一泽; Hoang, E; Hosseinzadeh, G; Hsu, B; Jacobson-Galán, W; Janzen, D; Jencson, J; Jha, SW; Kilpatrick, CD; Kwok, LA; Liu, C; Lundquist, MJ; Mehta, D; Miller, AA; Ravi, AP; Rehemtulla, N; Meza Retamal, N; Shrestha, M; Smith, N; Valenti, S; Whitler, L

Mid-infrared Dust Evolution and Late-time Circumstellar Medium Interaction in SN 2017eaw

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Pearson, J ORCID: 0000-0002-0744-0047, Subrayan, B ORCID: 0000-0001-8073-8731, Sand, DJ ORCID: 0000-0003-4102-380X, Andrews, JE ORCID: 0000-0003-0123-0062, Beasor, ER ORCID: 0000-0003-4666-4606, Bostroem, KA ORCID: 0000-0002-4924-444X, Dong 董, Y一泽 ORCID: 0000-0002-7937-6371, Hoang, E ORCID: 0000-0003-2744-4755, Hosseinzadeh, G ORCID: 0000-0002-0832-2974, Hsu, B ORCID: 0000-0002-9454-1742, Jacobson-Galán, W ORCID: 0000-0003-1103-3409, Janzen, D ORCID: 0000-0003-0549-3281, Jencson, J ORCID: 0000-0001-5754-4007, Jha, SW ORCID: 0000-0001-8738-6011, Kilpatrick, CD ORCID: 0000-0002-5740-7747, Kwok, LA ORCID: 0000-0003-3108-1328, Liu, C ORCID: 0000-0002-7866-4531, Lundquist, MJ ORCID: 0000-0001-9589-3793, Mehta, D ORCID: 0009-0008-9693-4348, Miller, AA ORCID: 0000-0001-9515-478X et al (2025) Mid-infrared Dust Evolution and Late-time Circumstellar Medium Interaction in SN 2017eaw. The Astrophysical Journal, 993 (2). p. 213. ISSN 0004-637X

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Publisher URL: https://doi.org/10.3847/1538-4357/ae00ba

Abstract

We present JWST/Mid-Infrared Instrument (MIRI) and complementary ground-based near-infrared observations of the Type II SN 2017eaw taken 6 yr postexplosion. SN 2017eaw is still detected out to 25 μm and there is minimal evolution in the mid-infrared spectral energy distribution (SED) between the newly acquired JWST/MIRI observations and those taken a year earlier. Modeling of the mid-infrared SED reveals a cool ∼160 K dust component of 5.5 × 10−4 M⊙ and a hot ∼1700 K component of 5.4 × 10−8 M⊙, both composed of silicate dust. Notably, there is no evidence of temperature or mass evolution in the cool dust component in the year between JWST observations. We also present new and archival HST and ground-based ultraviolet (UV) and optical observations which reveal reduced but continued circumstellar medium (CSM)–ejecta interaction at >2000 days postexplosion. The UV and mid-infrared emission show similar decline rates, suggesting both probe the interface between the ejecta and CSM. Given the continued existence of boxy Hα emission in the nebular spectra, the low inferred optical depth of the dust, and the lack of temperature and mass evolution, we suggest that the cool dust component in SN 2017eaw may be primarily due to pre-existing dust rather than newly formed dust in the ejecta or cold dense shell.

Item Type:	Article
Uncontrolled Keywords:	5109 Space Sciences; 51 Physical Sciences; 0201 Astronomical and Space Sciences; 0202 Atomic, Molecular, Nuclear, Particle and Plasma Physics; 0306 Physical Chemistry (incl. Structural); Astronomy & Astrophysics; 5101 Astronomical sciences; 5107 Particle and high energy physics; 5109 Space sciences
Subjects:	Q Science > QB Astronomy Q Science > QC Physics
Divisions:	Astrophysics Research Institute
Publisher:	American Astronomical Society
Date of acceptance:	19 August 2025
Date of first compliant Open Access:	14 November 2025
Date Deposited:	14 Nov 2025 16:29
Last Modified:	14 Nov 2025 16:45
DOI or ID number:	10.3847/1538-4357/ae00ba
URI:	https://researchonline.ljmu.ac.uk/id/eprint/27566

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