Fermi detection of $γ$-rays from the radio-quiet Seyfert galaxy NGC 3281
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| Format: | Preprint |
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2025
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| _version_ | 1866914058012196864 |
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| author | Liu, Jun-Rong Feng, Hua Wang, Jian-Min |
| author_facet | Liu, Jun-Rong Feng, Hua Wang, Jian-Min |
| contents | We report the detection of significant $γ$-ray emission with $\it Fermi$-LAT from the radio-quiet Seyfert 2 galaxy NGC 3281, with a luminosity of $5.9\,(\pm 1.7)\times10^{41}\rm\,erg\,s^{-1}$ at a significance of $6.22\,σ$ (TS = $42.81$). The power-law photon index is $2.61~(\pm 0.24)$, indicative of a soft spectrum. The star formation activity in NGC 3281 is insufficient to explain its $γ$-ray luminosity based on the empirical relation between the infrared and $γ$-ray luminosities observed in other sources. The multiwavelength spectrum can be explained as due to inverse Compton scattering by relativistic electrons in the corona or jet of seed photons from the corona, disk and torus. The source is Compton-thick and attenuation of GeV photons due to pair production in the corona is nonnegligible (with an optical depth of about 10). The intrinsic $γ$-ray luminosity is inferred to be $3.4\,\times10^{42}$ and $2.2\,\times10^{41}\rm\,erg\,s^{-1}$ for the corona and jet model, respectively. The observed $γ$-ray and radio luminosities is roughly consistent with the known correlation between the two quantities, among the lowest luminosity regime. The jet origin is valid only if the radio emission is dominated by the jet. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2509_21958 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Fermi detection of $γ$-rays from the radio-quiet Seyfert galaxy NGC 3281 Liu, Jun-Rong Feng, Hua Wang, Jian-Min High Energy Astrophysical Phenomena Astrophysics of Galaxies We report the detection of significant $γ$-ray emission with $\it Fermi$-LAT from the radio-quiet Seyfert 2 galaxy NGC 3281, with a luminosity of $5.9\,(\pm 1.7)\times10^{41}\rm\,erg\,s^{-1}$ at a significance of $6.22\,σ$ (TS = $42.81$). The power-law photon index is $2.61~(\pm 0.24)$, indicative of a soft spectrum. The star formation activity in NGC 3281 is insufficient to explain its $γ$-ray luminosity based on the empirical relation between the infrared and $γ$-ray luminosities observed in other sources. The multiwavelength spectrum can be explained as due to inverse Compton scattering by relativistic electrons in the corona or jet of seed photons from the corona, disk and torus. The source is Compton-thick and attenuation of GeV photons due to pair production in the corona is nonnegligible (with an optical depth of about 10). The intrinsic $γ$-ray luminosity is inferred to be $3.4\,\times10^{42}$ and $2.2\,\times10^{41}\rm\,erg\,s^{-1}$ for the corona and jet model, respectively. The observed $γ$-ray and radio luminosities is roughly consistent with the known correlation between the two quantities, among the lowest luminosity regime. The jet origin is valid only if the radio emission is dominated by the jet. |
| title | Fermi detection of $γ$-rays from the radio-quiet Seyfert galaxy NGC 3281 |
| topic | High Energy Astrophysical Phenomena Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2509.21958 |