The Bolometric Light-curve Modeling of 98 Type I Superluminous Supernovae Using the Magnetar- and the Circumstellar Interaction Models Reveals Surprisingly High Ejecta Masses
We present the bolometric light-curve modeling of 98 hydrogen-poor superluminous supernovae (SLSNe-I) using three types of power inputs: the magnetar model and two kinds of circumstellar interaction models, applying the constant density and the steady wind scenario. The quasi-bolometric luminosities...
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| Main Author: | |
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| Format: | Article |
| Language: | English |
| Published: |
IOP Publishing
2025-01-01
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| Series: | The Astrophysical Journal |
| Subjects: | |
| Online Access: | https://doi.org/10.3847/1538-4357/adae04 |
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| Summary: | We present the bolometric light-curve modeling of 98 hydrogen-poor superluminous supernovae (SLSNe-I) using three types of power inputs: the magnetar model and two kinds of circumstellar interaction models, applying the constant density and the steady wind scenario. The quasi-bolometric luminosities of the objects were calculated from the Zwicky Transient Facility g - and r -band data using the methodology of Chen et al., and then they were modeled with the Minim code. It was found that the light curves of 45 SLSNe-I can be fitted equally well with both the magnetar and the circumstellar material (CSM) models, 14 objects prefer the magnetar model, and 39 SLSNe-I favor the CSM model. The magnetar modeling yielded a mean spin period of P = 4.1 ± 0.20 ms and a magnetic field of B = 5.65 ± 0.43 · 10 ^14 G, consistent with the literature. However, the ejected mass was estimated to be significantly larger compared to previous studies presenting either multicolor light-curve modeling with MOSFiT or bolometric light-curve modeling: we obtained a mean value and standard error of 34.26 and 4.67 M _⊙ , respectively. The circumstellar interaction models resulted in even larger ejecta masses with a mean and standard error of 116.82 and 5.97 M _⊙ for the constant density model, and 105.99 and 4.50 M _⊙ for the steady wind model. Although the ejected mass depends strongly on the electron scattering opacity (assumed to be κ = 0.2 in this work) and the ejecta velocity, which were estimated to be globally larger compared to earlier studies, our results suggest that SLSNe-I are indeed explosions of the most-massive stars. |
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| ISSN: | 1538-4357 |