X-ray Flux and Spectral Variability of Blazar H 2356-309

• Main Authors: Kiran A. Wani, Haritma Gaur
• Format: Article
• Language: English
• Published: MDPI AG 2020-08-01
• Series: Galaxies
• Subjects: BL Lacertae objects; general—BL Lacertae objects; individual; H 2356-309—galaxies; active
• Online Access: https://www.mdpi.com/2075-4434/8/3/59

We present the results of timing and spectral analysis of the blazar H 2356-309 using XMM-Newton observations. This blazar is observed during 13 June 2005–24 December 2013 in total nine observations. Five of the observations show moderate flux variability with amplitude 1.7–2.2%. We search for the intra-day variability timescales in these five light curves, but did not find in any of them. The fractional variability amplitude is generally lower in the soft bands than in the hard bands, which is attributed to the energy dependent synchrotron emission. Using the hardness ratio analysis, we search for the X-ray spectral variability along with flux variability in this source. However, we did not find any significant spectral variability on intra-day timescales. We also investigate the X-ray spectral curvature of blazar H 2356-309 and found that six of our observations are well described by the log parabolic model with <inline-formula><math display="inline"><semantics><mi>α</mi></semantics></math></inline-formula> = 1.99–2.15 and <inline-formula><math display="inline"><semantics><mi>β</mi></semantics></math></inline-formula> = 0.03–0.18. Three of our observations are well described by power law model. The break energy of the X-ray spectra varies between 1.97–2.31 keV. We investigate the correlation between various parameters that are derived from log parabolic model and their implications are discussed.