On the Neutrino and Gamma-Ray Emission from NGC 1068

Journal Article · Thu Jul 06 04:00:00 EDT 2023 · TBD

OSTI ID:2202844

Blanco, Carlos ^[1]; Hooper, Dan ^[2]; Linden, Tim ^[3]; Pinetti, Elena ^[4]

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1. Princeton U.; Stockholm U., OKC
2. Fermilab; Chicago U., Astron. Astrophys. Ctr.; Chicago U., KICP
3. Stockholm U., OKC
4. Fermilab; Chicago U., KICP

IceCube has recently reported the detection of $$\sim 1-10 \,{\rm TeV}$$ neutrinos from the nearby active galaxy, NGC 1068. The lack of TeV-scale emission from this source suggests that these neutrinos are generated in the dense corona that surrounds NGC 1068's supermassive black hole. In this paper, we present a physical model for this source, including the processes of pair production, pion production, synchrotron, and inverse Compton scattering. We have also performed a new analysis of Fermi-LAT data from the direction of NGC 1068, finding that the gamma-ray emission from this source is very soft but bright at energies below $$\sim 1 \, {\rm GeV}$$. Our model can predict a gamma-ray spectrum that is consistent with Fermi-LAT observations, but only if the magnetic field within the corona of this active galactic nucleus (AGN) is quite high, namely $$B\gtrsim 6 \, {\rm kG}$$. To explain the observed neutrino emission, this source must accelerate protons with a total power that is comparable to its intrinsic X-ray luminosity. In this context, we consider two additional nearby active galaxies, NGC 4151 and NGC 3079, which have been identified as promising targets for IceCube.

• Research Organization: Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States)
• Sponsoring Organization: USDOE Office of Science (SC), High Energy Physics (HEP) (SC-25)
• DOE Contract Number: AC02-07CH11359
• OSTI ID: 2202844
• Report Number(s): FERMILAB-PUB-23-469-T; arXiv:2307.03259; oai:inspirehep.net:2675234
• Journal Information: TBD, Journal Name: TBD
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS