Gamma-ray signature of superluminous supernovae: Fermi-LAT GeV detection of SN 2017egm and evidence of a central engine
文献类型：期刊论文
| 作者 | Acero, F.1,2; Acharyya, A.3; Adelfio, A.4; Ajello, M.5; Aviano, E.6,7; Baldini, L.8,9; Ballet, J.1; Bartolini, C.10,11; Bastieri, D.12,13,14; Gonzalez, J. Becerra15 |
| 刊名 | ASTRONOMY & ASTROPHYSICS
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| 出版日期 | 2026-05-20 |
| 卷号 | 709 |
| 关键词 | astroparticle physics shock waves stars: magnetars supernovae: general supernovae: individual:: SN 2017egm |
| ISSN号 | 0004-6361 |
| DOI | 10.1051/0004-6361/202558547 |
| 产权排序 | 第45完成单位 |
| 文献子类 | Article |
| 英文摘要 | Context. 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. While the optical properties of SLSNe are extensively studied, their gamma-ray signatures remain poorly constrained. Aims. To further constrain the underlying mechanism, we carried out a systematic search for giga-electronvolt gamma-ray emission using the Fermi Large Area Telescope (LAT) from a sample of nearby hydrogen-poor (Type I) and hydrogen-rich (Type II) SLSNe over the past 16 years. Our objective is to test predictions from CSM and magnetar models, and to assess the prospects for future detections with the Cherenkov Telescope Array Observatory (CTAO). Methods. For the six targets of this sample, we studied the time variability of a putative gamma-ray signal at the optical position of the SLSN on a six-month timescale, and in the case of SN 2017egm, we further investigated variability on 15-day intervals and applied a Bayesian block algorithm to characterize the time variability of the signal. We then compared the temporal evolution and spectral properties to the predictions from a magnetar and CSM interaction model. Results. Among the sample, only SN 2017egm shows significant gamma-ray emission, with likelihood test statistic (TS) values of 26-33 (i.e., > 5 sigma) 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 Gamma = 2.17 +/- 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-gamma/L-opt similar to 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). Conclusions. 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. In order to explain the observed late-time bumps in the optical light curve of SN 2017egm, we require either: a hybrid picture combining magnetar and multiple CSM shells for the optical bumps or a pure magnetar model with infalling matter on an accretion disk. Finally, simulations of 50 hours of CTAO observations indicate that a SN 2017egm-like event would be detectable up to similar to 140 Mpc in the magnetar model but not in the CSM model due to strong gamma - gamma absorption. |
| 学科主题 | 天文学 ; 天体物理学 ; 高能天体物理学 ; 星系与宇宙学 |
| URL标识 | 查看原文 |
| 出版地 | 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE |
| WOS关键词 | LARGE-AREA TELESCOPE ; PULSATIONAL PAIR-INSTABILITY ; RADIATION-MEDIATED SHOCKS ; LIGHT-CURVE ; LIKELIHOOD ANALYSIS ; FALLBACK ACCRETION ; NGC 3191 ; EMISSION ; ACCELERATION ; CONSTRAINTS |
| 资助项目 | CNES; Beatriu de Pinos postdoctoral grant programme of the Departament de Recerca i Universitats de la Generalitat de Catalunya[2024 BP 00244]; MICIU/AEI/FEDER, UE[PID2024-155316NB-I00]; CSIC[PIE 202350E189]; Spanish program Unidad de Excelencia Maria de Maeztu[CEX2020-001058-M]; MCIN[AST-2406637]; European Union NextGeneration EU[PRTR-C17.I1]; National Science Foundation[AST-2406637]; National Science Foundation (NSF) by the NSF[AST-2506735]; NASA; Smithsonian Astrophysical Observatory (SAO)[TM4-25003X]; Simons Foundation[101042299]; ETAg grant[PRG2159]; European Union (ERC)[101042299]; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France; DOE[DE-AC02-76SF00515]; National Aeronautics and Space Administration; Centre National de la Recherche Scientifique / Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High Energy Accelerator Research Organization (KEK)[DE-AC02-76SF00515] |
| WOS研究方向 | Astronomy & Astrophysics |
| 语种 | 英语 |
| WOS记录号 | WOS:001770549400001 |
| 出版者 | EDP SCIENCES S A |
| 资助机构 | CNES ; Beatriu de Pinos postdoctoral grant programme of the Departament de Recerca i Universitats de la Generalitat de Catalunya[2024 BP 00244] ; MICIU/AEI/FEDER, UE[PID2024-155316NB-I00] ; CSIC[PIE 202350E189] ; Spanish program Unidad de Excelencia Maria de Maeztu[CEX2020-001058-M] ; MCIN[AST-2406637] ; European Union NextGeneration EU[PRTR-C17.I1] ; National Science Foundation[AST-2406637] ; National Science Foundation (NSF) by the NSF[AST-2506735] ; NASA ; Smithsonian Astrophysical Observatory (SAO)[TM4-25003X] ; Simons Foundation[101042299] ; ETAg grant[PRG2159] ; European Union (ERC)[101042299] ; Istituto Nazionale di Astrofisica in Italy ; Centre National d'Etudes Spatiales in France ; DOE[DE-AC02-76SF00515] ; National Aeronautics and Space Administration ; Centre National de la Recherche Scientifique / Institut National de Physique Nucleaire et de Physique des Particules in France ; Agenzia Spaziale Italiana ; Istituto Nazionale di Fisica Nucleare in Italy ; Ministry of Education, Culture, Sports, Science and Technology (MEXT) ; High Energy Accelerator Research Organization (KEK)[DE-AC02-76SF00515] |
| 版本 | 出版稿 |
| 源URL | [http://ir.ynao.ac.cn/handle/114a53/29240]  |
| 专题 | 星系类星体研究组 |
| 通讯作者 | Acero, F.; Martí, G. |
| 作者单位 | 1.Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, F-91191 Gif-sur-Yvette Cedex, France; 2.FSLAC IRL 2009, CNRS/IAC, La Laguna, Tenerife, Spain; 3.Center for Cosmology and Particle Physics Phenomenology, University of Southern Denmark, Campusvej 55, DK-5230 Odense M, Denmark; 4.Istituto Nazionale di Fisica Nucleare, Sezione di Perugia, I-06123 Perugia, Italy; 5.Department of Physics and Astronomy, Clemson University, Kinard Lab of Physics, Clemson, SC 29634-0978, USA; 6.Dipartimento di Fisica, Università di Trieste, I-34127 Trieste, Italy; 7.Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, I-34127 Trieste, Italy; 8.Università di Pisa, Dipartimento di Fisica E. Fermi, I-56127 Pisa, Italy; 9.Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy; 10.Istituto Nazionale di Fisica Nucleare, Sezione di Bari, I-70126 Bari, Italy; |
| 推荐引用方式 GB/T 7714 | Acero, F.,Acharyya, A.,Adelfio, A.,et al. Gamma-ray signature of superluminous supernovae: Fermi-LAT GeV detection of SN 2017egm and evidence of a central engine[J]. ASTRONOMY & ASTROPHYSICS,2026,709. |
| APA | Acero, F..,Acharyya, A..,Adelfio, A..,Ajello, M..,Aviano, E..,...&Vurm, I..(2026).Gamma-ray signature of superluminous supernovae: Fermi-LAT GeV detection of SN 2017egm and evidence of a central engine.ASTRONOMY & ASTROPHYSICS,709. |
| MLA | Acero, F.,et al."Gamma-ray signature of superluminous supernovae: Fermi-LAT GeV detection of SN 2017egm and evidence of a central engine".ASTRONOMY & ASTROPHYSICS 709(2026). |
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