Long-term and flares variability of Fermi LAT FSRQ 4C +21.35
Hashad, M., Abdou, Y., Bounduok, I., Badraan, H. (2019). Long-term and flares variability of Fermi LAT FSRQ 4C +21.35. EKB Journal Management System, 52(2), 54-61. doi: 10.21608/ajnsa.2019.3402.1078
Mohamed Hashad; Yasser Abdou; Ibrahim Bounduok; Hussein Badraan. "Long-term and flares variability of Fermi LAT FSRQ 4C +21.35". EKB Journal Management System, 52, 2, 2019, 54-61. doi: 10.21608/ajnsa.2019.3402.1078
Hashad, M., Abdou, Y., Bounduok, I., Badraan, H. (2019). 'Long-term and flares variability of Fermi LAT FSRQ 4C +21.35', EKB Journal Management System, 52(2), pp. 54-61. doi: 10.21608/ajnsa.2019.3402.1078
Hashad, M., Abdou, Y., Bounduok, I., Badraan, H. Long-term and flares variability of Fermi LAT FSRQ 4C +21.35. EKB Journal Management System, 2019; 52(2): 54-61. doi: 10.21608/ajnsa.2019.3402.1078

Long-term and flares variability of Fermi LAT FSRQ 4C +21.35

Arab Journal of Nuclear Sciences and Applications
Article 8, Volume 52, Issue 2, April 2019, Page 54-61  XML PDF (1.1 MB)
Document Type: Original Article
DOI: 10.21608/ajnsa.2019.3402.1078
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Authors
Mohamed Hashad email 1; Yasser Abdou2; Ibrahim Bounduok3; Hussein Badraan3
1Basic Science Department, Modern Academy for Engineering and Technology, Maadi, Egypt.
2Physics Department, Faculty of Science, Tanta University, Tanta 31527, Egypt.
3Physics Department, Faculty of Science, Tanta University, Tanta 31527, Egypt
Abstract
We present a long term light curve (LC) of the flat spectrum radio quasar (FSRQ) 4C +21.35 (also known as PKS 1222+216, z=0.432) observed by the Fermi Large Area Telescope (LAT) during the first seven years of the mission with weekly time binning in the energy range 0.2–50 GeV. The highest weekly integral flux was reached on MJD = 55365 (2010, Jun. 18). The variability of the source emission was studied with 12 hour time binning in two energy bands 0.2 – 0.8 GeV and 0.8 – 50 GeV. Three different statistical methods, the structure functions (SF), auto-correlation functions (ACF), and fast fourier transformer were used to study the time scales. For the 7 year-weekly binning light curve, 18 week time scale was observed. Flare I seems to have the same time scales for both energy ranges as well. Therefore the outbursts during flare I may come from the same emission mechanism/s, CCF between the two energy bands have also emphasized it. Flare II did not give significant results, CCF illustrated 6.5 day time lag that indicates the emission mechanism of the low energy band came before the high energy one with 6.5 day with a typical physical process.
Keywords
Non-thermal FSRQ; Individual 4C+21.35; Active Galaxies; Statistics
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