Figure 8 - Long-term Optical and γ-Ray Variability of the Blazar PKS 1222+216

Figure 8. SEDs of the source fitted with the Jetset code for the γ-ray flaring and quiescent epochs. The optical/UV photometric data were obtained from Swift UVOT filters (V, B, U, UVW1, UVM2, and UVW2), and the X-ray (0.3-10 keV) spectra were taken from XRT observations. LAT spectra were used for the high-energy γ-ray emission. The upper limits in the LAT spectra are plotted as downward arrows.

SEDs of the source fitted with the Jetset code for the γ-ray flaring and quiescent epochs. The optical/UV photometric data were obtained from Swift UVOT filters (V, B, U, UVW1, UVM2, and UVW2), and the X-ray (0.3-10 keV) spectra were taken from XRT observations. LAT spectra were used for the high-energy γ-ray emission. The upper limits in the LAT spectra are plotted as downward arrows.

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Reference

Long-term Optical and γ-Ray Variability of the Blazar PKS 1222+216 - Scientific Figure on ResearchGate. Available from: https://www.researchgate.net/figure/SEDs-of-the-source-fitted-with-the-Jetset-code-for-the-g-ray-flaring-and-quiescent_fig3_365256344 [accessed 27 Apr 2025]

Caption

Figure 8. SEDs of the source fitted with the Jetset code for the γ-ray flaring and quiescent epochs. The optical/UV photometric data were obtained from Swift UVOT filters (V, B, U, UVW1, UVM2, and UVW2), and the X-ray (0.3-10 keV) spectra were taken from XRT observations. LAT spectra were used for the high-energy γ-ray emission. The upper limits in the LAT spectra are plotted as downward arrows.

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<a href="https://www.researchgate.net/figure/SEDs-of-the-source-fitted-with-the-Jetset-code-for-the-g-ray-flaring-and-quiescent_fig3_365256344"><img src="https://www.researchgate.net/publication/365256344/figure/fig3/AS:11431281096477447@1668158578904/SEDs-of-the-source-fitted-with-the-Jetset-code-for-the-g-ray-flaring-and-quiescent.png" alt="SEDs of the source fitted with the Jetset code for the γ-ray flaring and quiescent epochs. The optical/UV photometric data were obtained from Swift UVOT filters (V, B, U, UVW1, UVM2, and UVW2), and the X-ray (0.3-10 keV) spectra were taken from XRT observations. LAT spectra were used for the high-energy γ-ray emission. The upper limits in the LAT spectra are plotted as downward arrows."/></a>