2021/06/17 by Vinit Dhiman, Alok C. Gupta, Haritma Gaur +1 · 22 citations
Chemistry · Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Blazar #Chemistry #Dark Matter and Cosmic Phenomena #Duty cycle #Flux (metallurgy) #Gamma ray #Light curve #Materials science #Physics #Population #Power (physics) #Radio Astronomy Observations and Technology #Range (aeronautics) #Spectral density #Spectral line #Spectral slope #Statistics #astro-ph.HE
paper · pdf · doi:10.1093/mnras/stab1743
published in Monthly Notices of the Royal Astronomical Society 506(1), 1198-1208 (Oxford University Press) · 11 pages, 4 tables, 7 figures, The redshift of the blazar has been updated, leading to minor changes in certain quantities but no changes to conclusions. Complete Fig. 1-3 will be published as supplementary material and can be provided on request
openalex publication_date 2021/06/17 · openalex created_date 2021/06/22 · arxiv created 2021/06/25 · arxiv updated 2021/06/30 · openalex updated_date 2026/08/05
ABSTRACT We present variability analyses of twenty pointed XMM–Newton observations of the high energy peaked TeV blazar PG 1553+113 taken during 2010–2018. We found intraday variability in the total X-ray energy range (0.3–10 keV) in 16 out of 19 light curves or a duty cycle of ∼84 per cent. A discrete correlation function analysis of the intraday light curves in the soft and hard X-ray bands peaks on zero lag, showing that the emission in hard and soft bands are co-spatial and emitted from the same population of leptons. Red-noise dominates the power spectral density (PSD) of all the LCs, although the PSDs have a range of spectral slopes from −2.36 to −0.14. On longer time-scales, the optical and UV variability patterns look almost identical and well correlated, as are the soft and hard X-ray bands, but the optical/UV variations are not correlated to those in the X-ray band, indicating that the optical/UV and X-ray emissions are emitted by two different populations of leptons. We briefly discuss physical mechanisms that may be capable of explaining the observed flux and spectral variability of PG 1553+113 on these diverse time-scales.