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Broad-band spectral analysis of Mrk 926 using multi-epoch X-ray observations

Broad-band spectral analysis of Mrk 926 using multi-epoch X-ray observations
Broad-band spectral analysis of Mrk 926 using multi-epoch X-ray observations
The X-ray spectra of some active galactic nuclei (AGN) show a soft X-ray excess, emission in excess to the extrapolated primary X-ray continuum below 2 keV. Recent studies have shown that this soft excess can be described well as originating from either a relativistic ionized reflection, the extreme blurring of the reprocessed emission from the innermost region of the accretion disk, or Comptonization from an optically thick and warm region called the 'warm corona', in which electron scattering is the dominant source of opacity. To constrain the origin of the soft excess in the Seyfert 1 galaxy Mrk 926, we carry out an multi-epoch X-ray spectral study using observations from Suzaku (2009), XMM-Newton and NuSTAR (2016), and NuSTAR and Swift-XRT (2021). The broadband X-ray spectra of Mrk 926 contains: a thermally Comptonized primary continuum, a variable soft excess, and distant reflection. We find that in Mrk 926 as in so many sources, it is difficult to make a definite statement as to what is causing the observed soft excess. A warm coronal-like component is slightly preferred by the data but a reflection origin is also possible. Using archival radio data, we detect an optically-thin radio component in our broadband study of Mrk 926. While this component is consistent with an optically-thin radio jet, future multi-wavelength observations including high spatial resolution radio observations at multiple frequencies are required to probe the origin of the radio emission in more detail.
Astrophysics - High Energy Astrophysical Phenomena
0035-8711
4788 - 4794
Chalise, S.
02dc0d04-15c1-442b-8fd6-cb8a35f1d81d
Lohfink, A. M.
4efee873-2053-4837-92d2-2f1c7a6c4ccd
Chauhan, J.
ae7a3b04-9c5a-49d4-bce1-57420590d39b
Russell, T. D.
39142bae-8cbc-4cfb-a455-41c05c504ac1
Buisson, D. J. K.
f96b1210-d056-4948-9e4a-deeb669e6d1a
Mallick, L.
783ab2cd-e49d-41f4-95a7-745ec949ab72
Chalise, S.
02dc0d04-15c1-442b-8fd6-cb8a35f1d81d
Lohfink, A. M.
4efee873-2053-4837-92d2-2f1c7a6c4ccd
Chauhan, J.
ae7a3b04-9c5a-49d4-bce1-57420590d39b
Russell, T. D.
39142bae-8cbc-4cfb-a455-41c05c504ac1
Buisson, D. J. K.
f96b1210-d056-4948-9e4a-deeb669e6d1a
Mallick, L.
783ab2cd-e49d-41f4-95a7-745ec949ab72

Chalise, S., Lohfink, A. M., Chauhan, J., Russell, T. D., Buisson, D. J. K. and Mallick, L. (2022) Broad-band spectral analysis of Mrk 926 using multi-epoch X-ray observations. Monthly Notices of the Royal Astronomical Society, Advance Access, 517 (4), 4788 - 4794. (doi:10.1093/mnras/stac2953).

Record type: Article

Abstract

The X-ray spectra of some active galactic nuclei (AGN) show a soft X-ray excess, emission in excess to the extrapolated primary X-ray continuum below 2 keV. Recent studies have shown that this soft excess can be described well as originating from either a relativistic ionized reflection, the extreme blurring of the reprocessed emission from the innermost region of the accretion disk, or Comptonization from an optically thick and warm region called the 'warm corona', in which electron scattering is the dominant source of opacity. To constrain the origin of the soft excess in the Seyfert 1 galaxy Mrk 926, we carry out an multi-epoch X-ray spectral study using observations from Suzaku (2009), XMM-Newton and NuSTAR (2016), and NuSTAR and Swift-XRT (2021). The broadband X-ray spectra of Mrk 926 contains: a thermally Comptonized primary continuum, a variable soft excess, and distant reflection. We find that in Mrk 926 as in so many sources, it is difficult to make a definite statement as to what is causing the observed soft excess. A warm coronal-like component is slightly preferred by the data but a reflection origin is also possible. Using archival radio data, we detect an optically-thin radio component in our broadband study of Mrk 926. While this component is consistent with an optically-thin radio jet, future multi-wavelength observations including high spatial resolution radio observations at multiple frequencies are required to probe the origin of the radio emission in more detail.

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Accepted/In Press date: 10 October 2022
e-pub ahead of print date: 18 October 2022
Keywords: Astrophysics - High Energy Astrophysical Phenomena

Identifiers

Local EPrints ID: 471892
URI: http://eprints.soton.ac.uk/id/eprint/471892
ISSN: 0035-8711
PURE UUID: 9aadd118-9b82-479b-963c-df056cb00c6b

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Date deposited: 22 Nov 2022 17:37
Last modified: 10 Jan 2023 17:50

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Contributors

Author: S. Chalise
Author: A. M. Lohfink
Author: J. Chauhan
Author: T. D. Russell
Author: D. J. K. Buisson
Author: L. Mallick

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