On the Gamma-ray Efficiency of Superluminous Supernovae: Potential Detections and Population-Level Constraints
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arXiv
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| Autores principales: | , , , |
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| Formato: | Preprint |
| Publicado: |
2026
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| _version_ | 1866915943325630464 |
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| author | Crnogorčević, Milena Linden, Tim Goobar, Ariel Metzger, Brian D. |
| author_facet | Crnogorčević, Milena Linden, Tim Goobar, Ariel Metzger, Brian D. |
| contents | Superluminous supernovae (SLSNe) are among the most energetic stellar explosions, yet their central power source remains uncertain. Models invoking magnetar spin-down or circumstellar interaction predict GeV gamma-ray emission once the ejecta becomes transparent to high-energy photons. We search for such emission from 223 hydrogen-poor SLSNe using 17 years of Fermi-LAT data, defining source-specific search windows based on the Bethe--Heitler transparency time. We find no significant ($\geq5σ$) GeV emission. A joint-likelihood analysis constrains the GeV-to-optical efficiency to $η< 1.3\times10^{-3}$, two orders of magnitude below the predictions for weakly magnetized magnetar nebulae. A hierarchical population analysis shows that fewer than $0.7\%$ of SLSNe-I can have $η> 10^{-2}$. SN 2017egm, however, shows a suggestive excess ($\sim$4 $σ$). In the 0.1--500 GeV band, the observed $L_γ/L_{\rm opt} \sim 0.68$ for SN 2017egm exceeds hadronic expectations by over an order of magnitude, favoring a magnetar origin. The non-detection of the similarly nearby SN 2018bsz disfavors simple uniform-efficiency scenarios, or potentially points to diversity in the underlying powering mechanisms. We also note a possible excess from SN 2024jlc, though continued Fermi-LAT monitoring is needed because the source may still be within its transparency window. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2604_16595 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | On the Gamma-ray Efficiency of Superluminous Supernovae: Potential Detections and Population-Level Constraints Crnogorčević, Milena Linden, Tim Goobar, Ariel Metzger, Brian D. High Energy Astrophysical Phenomena Cosmology and Nongalactic Astrophysics Superluminous supernovae (SLSNe) are among the most energetic stellar explosions, yet their central power source remains uncertain. Models invoking magnetar spin-down or circumstellar interaction predict GeV gamma-ray emission once the ejecta becomes transparent to high-energy photons. We search for such emission from 223 hydrogen-poor SLSNe using 17 years of Fermi-LAT data, defining source-specific search windows based on the Bethe--Heitler transparency time. We find no significant ($\geq5σ$) GeV emission. A joint-likelihood analysis constrains the GeV-to-optical efficiency to $η< 1.3\times10^{-3}$, two orders of magnitude below the predictions for weakly magnetized magnetar nebulae. A hierarchical population analysis shows that fewer than $0.7\%$ of SLSNe-I can have $η> 10^{-2}$. SN 2017egm, however, shows a suggestive excess ($\sim$4 $σ$). In the 0.1--500 GeV band, the observed $L_γ/L_{\rm opt} \sim 0.68$ for SN 2017egm exceeds hadronic expectations by over an order of magnitude, favoring a magnetar origin. The non-detection of the similarly nearby SN 2018bsz disfavors simple uniform-efficiency scenarios, or potentially points to diversity in the underlying powering mechanisms. We also note a possible excess from SN 2024jlc, though continued Fermi-LAT monitoring is needed because the source may still be within its transparency window. |
| title | On the Gamma-ray Efficiency of Superluminous Supernovae: Potential Detections and Population-Level Constraints |
| topic | High Energy Astrophysical Phenomena Cosmology and Nongalactic Astrophysics |
| url | https://arxiv.org/abs/2604.16595 |