학술논문
VERITAS and Fermi-LAT Constraints on the Gamma-Ray Emission from Superluminous Supernovae SN2015bn and SN2017egm
Document Type
article
Author
A. Acharyya; C. B. Adams; P. Bangale; W. Benbow; J. H. Buckley; M. Capasso; V. V. Dwarkadas; M. Errando; A. Falcone; Q. Feng; J. P. Finley; G. M. Foote; L. Fortson; A. Furniss; G. Gallagher; A. Gent; W. F Hanlon; O. Hervet; J. Holder; T. B. Humensky; W. Jin; P. Kaaret; M. Kertzman; M. Kherlakian; D. Kieda; T. K Kleiner; S. Kumar; M. J. Lang; M. Lundy; G. Maier; C. E McGrath; J. Millis; P. Moriarty; R. Mukherjee; M. Nievas-Rosillo; S. O’Brien; R. A. Ong; S. R. Patel; K. Pfrang; M. Pohl; E. Pueschel; J. Quinn; K. Ragan; P. T. Reynolds; D. Ribeiro; E. Roache; J. L. Ryan; I. Sadeh; M. Santander; G. H. Sembroski; R. Shang; M. Splettstoesser; D. Tak; J. V. Tucci; A. Weinstein; D. A. Williams; VERITAS collaboration; B. D. Metzger; M. Nicholl; I. Vurm
Source
The Astrophysical Journal, Vol 945, Iss 1, p 30 (2023)
Subject
Language
English
ISSN
1538-4357
Abstract
Superluminous supernovae (SLSNe) are a rare class of stellar explosions with luminosities ∼ 10–100 times greater than ordinary core-collapse supernovae. One popular model to explain the enhanced optical output of hydrogen-poor (Type I) SLSNe invokes energy injection from a rapidly spinning magnetar. A prediction in this case is that high-energy gamma-rays, generated in the wind nebula of the magnetar, could escape through the expanding supernova ejecta at late times (months or more after optical peak). This paper presents a search for gamma-ray emission in the broad energy band from 100 MeV to 30 TeV from two Type I SLSNe, SN2015bn, and SN2017egm, using observations from Fermi-LAT and VERITAS. Although no gamma-ray emission was detected from either source, the derived upper limits approach the putative magnetar’s spin-down luminosity. Prospects are explored for detecting very-high-energy (VHE; 100 GeV–100 TeV) emission from SLSNe-I with existing and planned facilities such as VERITAS and CTA.