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| Natura: | Preprint |
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2025
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| Accesso online: | https://arxiv.org/abs/2512.03716 |
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| author | Stritzinger, M. D. Moriya, T. J. Bose, S. Mazzali, P. A. Lundqvist, P. Karamehmetoglu, E. Arndt, L. S. Ashall, C. Galbany, L. Hoogendam, W. B. Baron, E. DerKacy, J. M. Elias-Rosa, N. Hsiao, E. Y. Höflich, P. Pian, E. Jensen, E. A. M. Moran, S. Pastorello, A. Shahbandeh, M. Valerin, G. |
| author_facet | Stritzinger, M. D. Moriya, T. J. Bose, S. Mazzali, P. A. Lundqvist, P. Karamehmetoglu, E. Arndt, L. S. Ashall, C. Galbany, L. Hoogendam, W. B. Baron, E. DerKacy, J. M. Elias-Rosa, N. Hsiao, E. Y. Höflich, P. Pian, E. Jensen, E. A. M. Moran, S. Pastorello, A. Shahbandeh, M. Valerin, G. |
| contents | We present infant-phase observations of the SN Ic-BL 2020lao, including optical spectroscopy beginning 48 hrs after explosion. The explosion time was constrained by power-law fits to the rising TESS and ZTF light curves, with the first ZTF detection occurring 27 hrs after explosion. The optical light curves show a rapid rise lasting 8.8 days and a peak luminosity typical of SNe Ic-BL (Mr=-18.5 mag). Unlike some engine-driven SN Ic-BL events, the light curve of SN 2020lao shows no evidence of an optical afterglow or excess emission, and the absence of shock-cooling in the TESS and ZTF data constrains the progenitor to a Wolf-Rayet-like star with radius less than a few times the solar radius, ruling out any extended envelope. The spectra resemble those of the X-ray-flash-associated SN 2006aj but with higher expansion velocities. From Arnett-type fits to the bolometric light curve and measured FeII velocities, we infer a Ni mass of 0.2 solar masses, an ejecta mass of 3.2 solar masses, and a kinetic energy of about 23x10^51 erg, corresponding to a specific kinetic energy of 7x10^51 erg per solar mass. Spectral synthesis modeling broadly reproduces the photospheric spectra of SN 2020lao and suggests a specific kinetic energy of 5x10^51 erg per solar mass. SN 2020lao and SN 2006aj synthesized comparable amounts of Ni, yet SN 2020lao exhibits specific kinetic energy values 5-10 times larger. VLA and Swift/XRT non-detections reveal no afterglow emission, allowing limits on relativistic ejecta and dense circumstellar material. Given that SN 2020lao reaches a specific kinetic energy typical of engine-driven SNe Ic-BL, the lack of an optical excess with the non-detections in the radio and X-ray bands suggests that if a relativistic jet was launched, it was either viewed far off axis or choked before breakout. If there was no relativistic jet, SN 2020lao would be an extreme nonrelativistic SN Ic-BL. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2512_03716 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The broad-lined type Ic supernova 2020lao experienced an energetic explosion with no central-engine signatures Stritzinger, M. D. Moriya, T. J. Bose, S. Mazzali, P. A. Lundqvist, P. Karamehmetoglu, E. Arndt, L. S. Ashall, C. Galbany, L. Hoogendam, W. B. Baron, E. DerKacy, J. M. Elias-Rosa, N. Hsiao, E. Y. Höflich, P. Pian, E. Jensen, E. A. M. Moran, S. Pastorello, A. Shahbandeh, M. Valerin, G. High Energy Astrophysical Phenomena We present infant-phase observations of the SN Ic-BL 2020lao, including optical spectroscopy beginning 48 hrs after explosion. The explosion time was constrained by power-law fits to the rising TESS and ZTF light curves, with the first ZTF detection occurring 27 hrs after explosion. The optical light curves show a rapid rise lasting 8.8 days and a peak luminosity typical of SNe Ic-BL (Mr=-18.5 mag). Unlike some engine-driven SN Ic-BL events, the light curve of SN 2020lao shows no evidence of an optical afterglow or excess emission, and the absence of shock-cooling in the TESS and ZTF data constrains the progenitor to a Wolf-Rayet-like star with radius less than a few times the solar radius, ruling out any extended envelope. The spectra resemble those of the X-ray-flash-associated SN 2006aj but with higher expansion velocities. From Arnett-type fits to the bolometric light curve and measured FeII velocities, we infer a Ni mass of 0.2 solar masses, an ejecta mass of 3.2 solar masses, and a kinetic energy of about 23x10^51 erg, corresponding to a specific kinetic energy of 7x10^51 erg per solar mass. Spectral synthesis modeling broadly reproduces the photospheric spectra of SN 2020lao and suggests a specific kinetic energy of 5x10^51 erg per solar mass. SN 2020lao and SN 2006aj synthesized comparable amounts of Ni, yet SN 2020lao exhibits specific kinetic energy values 5-10 times larger. VLA and Swift/XRT non-detections reveal no afterglow emission, allowing limits on relativistic ejecta and dense circumstellar material. Given that SN 2020lao reaches a specific kinetic energy typical of engine-driven SNe Ic-BL, the lack of an optical excess with the non-detections in the radio and X-ray bands suggests that if a relativistic jet was launched, it was either viewed far off axis or choked before breakout. If there was no relativistic jet, SN 2020lao would be an extreme nonrelativistic SN Ic-BL. |
| title | The broad-lined type Ic supernova 2020lao experienced an energetic explosion with no central-engine signatures |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2512.03716 |