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SN 2018bsz: Significant Dust Formation in a Nearby Superluminous Supernova

  • Authors: T.-W. Chen, 婷琬 陳, S. J. Brennan, R. Wesson, M. Fraser, T. Schweyer, C. Inserra, S. Schulze, M. Nicholl, J. P. Anderson, E. Y. Hsiao, 亦麒 蕭, A. Jerkstrand, E. Kankare, E. C. Kool, T. Kravtsov, H. Kuncarayakti, G. Leloudas, C.-J. Li, 傳睿 李, M. Matsuura, M. Pursiainen, R. Roy, A. J. Ruiter, P. Schady, I. R. Seitenzahl, J. Sollerman, L. Tartaglia, L. Wang, R. M. Yates, S. Yang, 圣 杨, D. Baade, R. Carini, A. Gal-Yam, L. Galbany, S. González-Gaitán, M. Gromadzki, C. P. Gutiérrez, R. Kotak, K. Maguire, P. A. Mazzali, T. E. Müller-Bravo, E. Paraskeva, P. J. Pessi, G. Pignata, A. Rau, D. R. Young

T.-W. Chen et al 2026 The Astrophysical Journal 1009 .

  • Provider: AAS Journals

Caption: Figure 6.

Continuation of Figure 5, showing only the best-fitting model from that grid. Predicted SED evolution for a smooth CSM shell (0.005–0.25 pc) composed of amorphous carbon grains with a = 0.1 μm. The symbols are the same as in Figure 3. This model yields the best overall agreement with the observed NIR/MIR fluxes among the CSM-shell geometries investigated, but it is disfavoured because it implies an optical depth that would violate the early-time optical 3σ limits and an inner radius that would lead to ejecta interaction after ∼1 yr (Section 4.2).

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