Jul 12 – 23, 2021
Europe/Berlin timezone

Resolving the origin of very-high-energy gamma-ray emission from the PeVatron candidate SNR G106.3+2.7 using MAGIC telescopes

Jul 14, 2021, 12:00 PM
1h 30m


Talk GAI | Gamma Ray Indirect Discussion


Tomohiko Oka (Kyoto University)


The supernova remnant (SNR) G106.3+2.7 is associated with a 100 TeV gamma-ray source reported by HAWC and is thus a promising PeVatron candidate. However, because of the poor angular resolution of HAWC, it is difficult to pinpoint the origin of the 100 TeV source. Because the SNR contains an energetic pulsar wind nebula (PWN) dubbed Boomerang and powered by the pulsar PSR J2229+6114, it is unclear whether the gamma-ray emission originates from the SNR or PWN complex and whether it is caused by hadronic or leptonic processes. We observed gamma rays above 200 GeV in the vicinity of the SNR G106.3+2.7 using the MAGIC telescopes for ~120 hours in total between May 2017 and August 2019, with an angular resolution of 0.07 – 0.1 degrees, which is unprecedented for this object at these energies. An extended gamma-ray emission spatially correlated with the radio continuum emission at the head and tail of SNR G106.3+2.7 was detected using the MAGIC telescopes. We find a hint of gamma-ray emission above 10 TeV only from the SNR tail region, while no significant emission above 5 TeV is found at the SNR head region containing the Boomerang PWN. Therefore, the gamma rays above 35 TeV detected with the air shower experiments are, likely, mainly emitted from the SNR tail region. In this presentation we discuss the morphology of the gamma-ray emission from this complex region and attempt self-consistent multiwavelength modeling of the energy spectrum from the different sources inside it.


Supernova remnants; Particle acceleration; Galactic cosmic ray; Gamma ray source; Gamma ray observation;

Collaboration MAGIC
Subcategory Experimental Results

Primary author

Tomohiko Oka (Kyoto University)


Presentation materials