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Gamma-ray signature of superluminous supernovae: Fermi-LAT GeV detection of SN 2017egm and evidence of a central engine

Fuente: arXiv

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Hauptverfasser:	Acero, F., Acharyya, A., Adelfio, A., Ajello, M., Aviano, E., Baldini, L., Ballet, J., Bartolini, C., Bastieri, D., Gonzalez, J. Becerra, Bellazzini, R., Bissaldi, E., Bonino, R., Bruel, P., Buson, S., Cameron, R. A., Caraveo, P. A., Casaburo, F., Casini, F., Cavazzuti, E., Cheung, C. C., Cibrario, N., Cozzolongo, G., Orestano, P. Cristarella, Cuna, F., Cutini, S., D'Ammando, F., Depalo, D., Digel, S. W., Di Lalla, N., Dinesh, A., Di Venere, L., Fauverge, P., Fiori, A., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasbarra, C., Gasparrini, D., Germani, S., Giacchino, F., Giglietto, N., Giliberti, M., Giordano, F., Giroletti, M., Grenier, I. A., Grondin, M. -H., Guiriec, S., Gupta, R., Hays, E., Hewitt, J. W., Airasca, A. Holzmann, Horan, D., Hou, X., Kayanoki, T., Kerr, M., Kuss, M., Laviron, A., Lemoine-Goumard, M., Liguori, A., Li, J., Liodakis, I., Loizzo, P., Longo, F., Loparco, F., Pérez, S. López, Lorusso, L., Lovellette, M. N., Lubrano, P., Maldera, S., Manfreda, A., Martí-Devesa, G., Martinelli, R., Mazziotta, M. N., Michailidis, M., Michelson, P. F., Mirabal, N., Mizuno, T., Monti-Guarnieri, P., Monzani, M. E., Morselli, A., Moskalenko, I. V., Negro, M., Omodei, N., Orienti, M., Orlando, E., Panzarini, G., Persic, M., Pesce-Rollins, M., Pillera, R., Porter, T. A., Principe, G., Rainò, S., Rando, R., Rani, B., Razzano, M., Reimer, A., Reimer, O., Sánchez-Conde, M., Parkinson, P. M. Saz, Serini, D., Sgrò, C., Siskind, E. J., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Thompson, D. J., Torres, D. F., Wadiasingh, Z., Wood, K., Zaharijas, G., Zhang, W., Chatzopoulos, E., Metzger, B. D., Pessi, P. J., Vurm, I.
Format:	Preprint
Veröffentlicht:	2026
Schlagworte:	High Energy Astrophysical Phenomena
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author	Acero, F. Acharyya, A. Adelfio, A. Ajello, M. Aviano, E. Baldini, L. Ballet, J. Bartolini, C. Bastieri, D. Gonzalez, J. Becerra Bellazzini, R. Bissaldi, E. Bonino, R. Bruel, P. Buson, S. Cameron, R. A. Caraveo, P. A. Casaburo, F. Casini, F. Cavazzuti, E. Cheung, C. C. Cibrario, N. Cozzolongo, G. Orestano, P. Cristarella Cuna, F. Cutini, S. D'Ammando, F. Depalo, D. Digel, S. W. Di Lalla, N. Dinesh, A. Di Venere, L. Fauverge, P. Fiori, A. Franckowiak, A. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasbarra, C. Gasparrini, D. Germani, S. Giacchino, F. Giglietto, N. Giliberti, M. Giordano, F. Giroletti, M. Grenier, I. A. Grondin, M. -H. Guiriec, S. Gupta, R. Hays, E. Hewitt, J. W. Airasca, A. Holzmann Horan, D. Hou, X. Kayanoki, T. Kerr, M. Kuss, M. Laviron, A. Lemoine-Goumard, M. Liguori, A. Li, J. Liodakis, I. Loizzo, P. Longo, F. Loparco, F. Pérez, S. López Lorusso, L. Lovellette, M. N. Lubrano, P. Maldera, S. Manfreda, A. Martí-Devesa, G. Martinelli, R. Mazziotta, M. N. Michailidis, M. Michelson, P. F. Mirabal, N. Mizuno, T. Monti-Guarnieri, P. Monzani, M. E. Morselli, A. Moskalenko, I. V. Negro, M. Omodei, N. Orienti, M. Orlando, E. Panzarini, G. Persic, M. Pesce-Rollins, M. Pillera, R. Porter, T. A. Principe, G. Rainò, S. Rando, R. Rani, B. Razzano, M. Reimer, A. Reimer, O. Sánchez-Conde, M. Parkinson, P. M. Saz Serini, D. Sgrò, C. Siskind, E. J. Spandre, G. Spinelli, P. Suson, D. J. Tajima, H. Thompson, D. J. Torres, D. F. Wadiasingh, Z. Wood, K. Zaharijas, G. Zhang, W. Chatzopoulos, E. Metzger, B. D. Pessi, P. J. Vurm, I.
author_facet	Acero, F. Acharyya, A. Adelfio, A. Ajello, M. Aviano, E. Baldini, L. Ballet, J. Bartolini, C. Bastieri, D. Gonzalez, J. Becerra Bellazzini, R. Bissaldi, E. Bonino, R. Bruel, P. Buson, S. Cameron, R. A. Caraveo, P. A. Casaburo, F. Casini, F. Cavazzuti, E. Cheung, C. C. Cibrario, N. Cozzolongo, G. Orestano, P. Cristarella Cuna, F. Cutini, S. D'Ammando, F. Depalo, D. Digel, S. W. Di Lalla, N. Dinesh, A. Di Venere, L. Fauverge, P. Fiori, A. Franckowiak, A. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasbarra, C. Gasparrini, D. Germani, S. Giacchino, F. Giglietto, N. Giliberti, M. Giordano, F. Giroletti, M. Grenier, I. A. Grondin, M. -H. Guiriec, S. Gupta, R. Hays, E. Hewitt, J. W. Airasca, A. Holzmann Horan, D. Hou, X. Kayanoki, T. Kerr, M. Kuss, M. Laviron, A. Lemoine-Goumard, M. Liguori, A. Li, J. Liodakis, I. Loizzo, P. Longo, F. Loparco, F. Pérez, S. López Lorusso, L. Lovellette, M. N. Lubrano, P. Maldera, S. Manfreda, A. Martí-Devesa, G. Martinelli, R. Mazziotta, M. N. Michailidis, M. Michelson, P. F. Mirabal, N. Mizuno, T. Monti-Guarnieri, P. Monzani, M. E. Morselli, A. Moskalenko, I. V. Negro, M. Omodei, N. Orienti, M. Orlando, E. Panzarini, G. Persic, M. Pesce-Rollins, M. Pillera, R. Porter, T. A. Principe, G. Rainò, S. Rando, R. Rani, B. Razzano, M. Reimer, A. Reimer, O. Sánchez-Conde, M. Parkinson, P. M. Saz Serini, D. Sgrò, C. Siskind, E. J. Spandre, G. Spinelli, P. Suson, D. J. Tajima, H. Thompson, D. J. Torres, D. F. Wadiasingh, Z. Wood, K. Zaharijas, G. Zhang, W. Chatzopoulos, E. Metzger, B. D. Pessi, P. J. Vurm, I.
contents	Superluminous supernovae (SLSNe) are a rare class of transients with peak luminosities 10-100 times greater than those of standard core-collapse supernovae (SNe). The mechanisms powering their extreme brightness remain debated, with circumstellar medium (CSM) interaction, or energy injection from a central engine like a magnetar wind nebula being the most plausible scenarios. To further constrain the underlying mechanism, we carried out a systematic search for GeV gamma-ray emission using the Fermi-LAT telescope from a sample of nearby hydrogen-poor (Type I) and hydrogen-rich (Type II) SLSNe over the past 16 years. Among the sample, only SN 2017egm shows significant gamma-ray emission, with likelihood test statistic (TS) values of 26-33 (i.e., >5$σ$) depending on the adopted time window. The signal arises between 50 and 160 days after explosion and is well described by a power-law spectrum with index $Γ=2.17 \pm 0.23$. The emission is consistent both in terms of its light curve and its spectrum, with predictions from magnetar models requiring either low nebular magnetization or faster spin-down than dipole losses. The CSM shell interaction scenario can reproduce the observed flux level but not the observed timing of the gamma-ray signal. In addition, the observed ratio, $L_γ/L_{opt} \sim 1$, is inconsistent with theoretical expectations and not in line with ratio measurements in other interacting CSM-dominated objects (e.g., novae or SNe) where this ratio is less than $10^{-2}$. Our study strongly suggests that a central engine like a magnetar plays a key role in this SLSN and could explain the bulk of the optical and gamma-ray light curves properties. Finally, simulations of 50 hours of CTAO observations indicate that a SN 2017egm-like event would be detectable up to 140 Mpc in the magnetar model but not in the CSM model due to strong gamma-gamma absorption.
format	Preprint
id	arxiv_https___arxiv_org_abs_2605_29909
institution	arXiv
publishDate	2026
record_format	arxiv
spellingShingle	Gamma-ray signature of superluminous supernovae: Fermi-LAT GeV detection of SN 2017egm and evidence of a central engine Acero, F. Acharyya, A. Adelfio, A. Ajello, M. Aviano, E. Baldini, L. Ballet, J. Bartolini, C. Bastieri, D. Gonzalez, J. Becerra Bellazzini, R. Bissaldi, E. Bonino, R. Bruel, P. Buson, S. Cameron, R. A. Caraveo, P. A. Casaburo, F. Casini, F. Cavazzuti, E. Cheung, C. C. Cibrario, N. Cozzolongo, G. Orestano, P. Cristarella Cuna, F. Cutini, S. D'Ammando, F. Depalo, D. Digel, S. W. Di Lalla, N. Dinesh, A. Di Venere, L. Fauverge, P. Fiori, A. Franckowiak, A. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasbarra, C. Gasparrini, D. Germani, S. Giacchino, F. Giglietto, N. Giliberti, M. Giordano, F. Giroletti, M. Grenier, I. A. Grondin, M. -H. Guiriec, S. Gupta, R. Hays, E. Hewitt, J. W. Airasca, A. Holzmann Horan, D. Hou, X. Kayanoki, T. Kerr, M. Kuss, M. Laviron, A. Lemoine-Goumard, M. Liguori, A. Li, J. Liodakis, I. Loizzo, P. Longo, F. Loparco, F. Pérez, S. López Lorusso, L. Lovellette, M. N. Lubrano, P. Maldera, S. Manfreda, A. Martí-Devesa, G. Martinelli, R. Mazziotta, M. N. Michailidis, M. Michelson, P. F. Mirabal, N. Mizuno, T. Monti-Guarnieri, P. Monzani, M. E. Morselli, A. Moskalenko, I. V. Negro, M. Omodei, N. Orienti, M. Orlando, E. Panzarini, G. Persic, M. Pesce-Rollins, M. Pillera, R. Porter, T. A. Principe, G. Rainò, S. Rando, R. Rani, B. Razzano, M. Reimer, A. Reimer, O. Sánchez-Conde, M. Parkinson, P. M. Saz Serini, D. Sgrò, C. Siskind, E. J. Spandre, G. Spinelli, P. Suson, D. J. Tajima, H. Thompson, D. J. Torres, D. F. Wadiasingh, Z. Wood, K. Zaharijas, G. Zhang, W. Chatzopoulos, E. Metzger, B. D. Pessi, P. J. Vurm, I. High Energy Astrophysical Phenomena Superluminous supernovae (SLSNe) are a rare class of transients with peak luminosities 10-100 times greater than those of standard core-collapse supernovae (SNe). The mechanisms powering their extreme brightness remain debated, with circumstellar medium (CSM) interaction, or energy injection from a central engine like a magnetar wind nebula being the most plausible scenarios. To further constrain the underlying mechanism, we carried out a systematic search for GeV gamma-ray emission using the Fermi-LAT telescope from a sample of nearby hydrogen-poor (Type I) and hydrogen-rich (Type II) SLSNe over the past 16 years. Among the sample, only SN 2017egm shows significant gamma-ray emission, with likelihood test statistic (TS) values of 26-33 (i.e., >5$σ$) depending on the adopted time window. The signal arises between 50 and 160 days after explosion and is well described by a power-law spectrum with index $Γ=2.17 \pm 0.23$. The emission is consistent both in terms of its light curve and its spectrum, with predictions from magnetar models requiring either low nebular magnetization or faster spin-down than dipole losses. The CSM shell interaction scenario can reproduce the observed flux level but not the observed timing of the gamma-ray signal. In addition, the observed ratio, $L_γ/L_{opt} \sim 1$, is inconsistent with theoretical expectations and not in line with ratio measurements in other interacting CSM-dominated objects (e.g., novae or SNe) where this ratio is less than $10^{-2}$. Our study strongly suggests that a central engine like a magnetar plays a key role in this SLSN and could explain the bulk of the optical and gamma-ray light curves properties. Finally, simulations of 50 hours of CTAO observations indicate that a SN 2017egm-like event would be detectable up to 140 Mpc in the magnetar model but not in the CSM model due to strong gamma-gamma absorption.
title	Gamma-ray signature of superluminous supernovae: Fermi-LAT GeV detection of SN 2017egm and evidence of a central engine
topic	High Energy Astrophysical Phenomena
url	https://arxiv.org/abs/2605.29909