Broadband Modeling of Low Luminosity Active Galactic Nuclei Detected in Gamma Rays. (arXiv:2107.08256v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Tomar_G/0/1/0/all/0/1">Gunjan Tomar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gupta_N/0/1/0/all/0/1">Nayantara Gupta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prince_R/0/1/0/all/0/1">Raj Prince</a>
Low luminosity active galactic nuclei are more abundant and closer to us than
the luminous ones but harder to explore as they are faint. We have selected the
four sources NGC 315, NGC 4261, NGC 1275, and NGC 4486, which have been
detected in gamma rays byFermi-LAT. We have compiled their long-term radio,
optical, X-ray data from different telescopes, analysed XMM-Newton data for NGC
4486, XMM-Newton and Swift data for NGC 315. We have analysed the Fermi-LAT
data collected over the period of 2008 to 2020 for all of them. Electrons are
assumed to be accelerated to relativistic energies in sub-parsec scale jets,
which radiate by synchrotron and synchrotron self-Compton emission covering
radio to gamma-ray energies. This model can fit most of the multi-wavelength
data points of the four sources. However, the gamma-ray data points from NGC
315 and NGC 4261 can be well fitted only up to 1.6 GeV and 0.6 GeV,
respectively in this model. This motivates us to find out the origin of the
higher energy {gamma}-rays detected from these sources. Kilo-parsec scale jets
have been observed previously from these sources in radio and X-ray
frequencies. If we assume {gamma}-rays are also produced in kilo-parsec scale
jets of these sources from inverse Compton scattering of starlight photons by
ultra-relativistic electrons, then it is possible to fit the gamma-ray data at
higher energies. Our result also suggests that strong host galaxy emission is
required to produce GeV radiation from kilo-parsec scale jets.
Low luminosity active galactic nuclei are more abundant and closer to us than
the luminous ones but harder to explore as they are faint. We have selected the
four sources NGC 315, NGC 4261, NGC 1275, and NGC 4486, which have been
detected in gamma rays byFermi-LAT. We have compiled their long-term radio,
optical, X-ray data from different telescopes, analysed XMM-Newton data for NGC
4486, XMM-Newton and Swift data for NGC 315. We have analysed the Fermi-LAT
data collected over the period of 2008 to 2020 for all of them. Electrons are
assumed to be accelerated to relativistic energies in sub-parsec scale jets,
which radiate by synchrotron and synchrotron self-Compton emission covering
radio to gamma-ray energies. This model can fit most of the multi-wavelength
data points of the four sources. However, the gamma-ray data points from NGC
315 and NGC 4261 can be well fitted only up to 1.6 GeV and 0.6 GeV,
respectively in this model. This motivates us to find out the origin of the
higher energy {gamma}-rays detected from these sources. Kilo-parsec scale jets
have been observed previously from these sources in radio and X-ray
frequencies. If we assume {gamma}-rays are also produced in kilo-parsec scale
jets of these sources from inverse Compton scattering of starlight photons by
ultra-relativistic electrons, then it is possible to fit the gamma-ray data at
higher energies. Our result also suggests that strong host galaxy emission is
required to produce GeV radiation from kilo-parsec scale jets.
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