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X-ray flux variability of active galactic nuclei observed using NuSTAR

Rani, Priyanka and Stalin, C. S. and Rakshit, Suvendu (2017) X-ray flux variability of active galactic nuclei observed using NuSTAR. Monthly Notices of the Royal Astronomical Society, 466 (3). pp. 3309-3322. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20161209-150240501

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Abstract

We present results of a systematic study of flux variability on hourly time-scales in a large sample of active galactic nuclei (AGN) in the 3−79 keV band using data from Nuclear Spectroscopic Telescope Array. Our sample consists of four BL Lac objects (BL Lacs), three flat spectrum radio quasars (FSRQs) 24 Seyfert 1, 42 Seyfert 2 and eight narrow line Seyfert 1 (NLSy1) galaxies. We find that in the 3−79 keV band, about 65 per cent of the sources in our sample show significant variations on hourly time-scales. Using the Mann–Whitney U-test and the Kolmogorov–Smirnov test, we find no difference in the variability behaviour between Seyfert 1 and 2 galaxies. The blazar sources (FSRQs and BL Lacs) in our sample are more variable than Seyfert galaxies that include Seyfert 1 and Seyfert 2 in the soft (3−10 keV), hard (10−79 keV) and total (3−79 keV) bands. NLSy1 galaxies show the highest duty cycle of variability (87 per cent), followed by BL Lacs (82 per cent), Seyfert galaxies (56 per cent) and FSRQs (23 per cent). We obtained flux doubling/halving time in the hard X-ray band less than 10 min in 11 sources. The flux variations between the hard and soft bands in all the sources in our sample are consistent with zero lag.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/stw3228DOIArticle
https://academic.oup.com/mnras/article/466/3/3309/2671018PublisherArticle
http://arxiv.org/abs/1612.02768arXivDiscussion Paper
ORCID:
AuthorORCID
Stalin, C. S.0000-0002-4998-1861
Additional Information:© 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2016 December 8. Received 2016 December 8; in original form 2016 September 26. Published: 12 December 2016. We thank the anonymous referee for his/her detailed comments that helped us to improve the manuscript. The comments by Dr. Markus Bottcher on an initial version of the manuscript is thankfully acknowledged. This research has made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology(USA). Note added in proof: We thank Dr. Madsen of the NuSTAR operations team for bringing to our attention improved background filtering for South Atlantic Anomaly (SAA) passage made available since the work in this paper as well as the ways to identify flares due to SAA from inspection of the background light curves. All data have now been checked for the existence of such events in our analysis and the updated results are given in this version of the manuscript.
Group:NuSTAR
Subject Keywords:galaxies: active – BL Lacertae objects: general – galaxies: jets – galaxies: nuclei – galaxies: Seyfert –X-rays: galaxies
Issue or Number:3
Record Number:CaltechAUTHORS:20161209-150240501
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20161209-150240501
Official Citation:Priyanka Rani, C. S. Stalin, Suvendu Rakshit; X-ray flux variability of active galactic nuclei observed using NuSTAR, Monthly Notices of the Royal Astronomical Society, Volume 466, Issue 3, 21 April 2017, Pages 3309–3322, https://doi.org/10.1093/mnras/stw3228
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:72696
Collection:CaltechAUTHORS
Deposited By: Joy Painter
Deposited On:10 Dec 2016 02:08
Last Modified:09 Mar 2020 13:19

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