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Accretion disc–corona and jet emission from the radio-loud narrow-line Seyfert 1 galaxy RX J1633.3+4719

Accretion disc–corona and jet emission from the radio-loud narrow-line Seyfert 1 galaxy RX J1633.3+4719
Accretion disc–corona and jet emission from the radio-loud narrow-line Seyfert 1 galaxy RX J1633.3+4719
We perform X-ray/ultraviolet (UV) spectral and X-ray variability studies of the radio-loud narrow-line Seyfert 1 (NLS1) galaxy RX J1633.3+4719 using XMM–Newton and Suzaku observations from 2011 and 2012. The 0.3–10 keV spectra consist of an ultrasoft component described by an accretion disc blackbody (kTin=39.6+11.2?5.5 eV) and a power law due to the thermal Comptonization (?=1.96+0.24?0.31) of the disc emission. The disc temperature inferred from the soft excess is at least a factor of 2 lower than that found for the canonical soft excess emission from radio-quiet NLS1s. The UV spectrum is described by a power law with photon index 3.05+0.56?0.33. The observed UV emission is too strong to arise from the accretion disc or the host galaxy, but can be attributed to a jet. The X-ray emission from RX J1633.3+4719 is variable with fractional variability amplitude Fvar = 13.5 ± 1.0?per?cent. In contrast to radio-quiet active galactic nuclei (AGN), X-ray emission from the source becomes harder with increasing flux. The fractional rms variability increases with energy and the rms spectrum is well described by a constant disc component and a variable power-law continuum with the normalization and photon index being anticorrelated. Such spectral variability cannot be caused by variations in the absorption and must be intrinsic to the hot corona. Our finding of possible evidence for emission from the inner accretion disc, jet and hot corona from RX J1633.3+4719 in the optical to X-ray bands makes this object an ideal target to probe the disc–jet connection in AGN.
0035-8711
1705-1715
Mallick, Labani
15b17e80-7c5f-4cf4-a09e-a8bfcda3cd6e
Dewangan, G.C.
5ac9d24b-bcbb-45ab-a838-b093e67fc990
Gandhi, P.
5bc3b5af-42b0-4dd8-8f1f-f74048d4d4a9
Misra, R.
95702ea5-39c7-4579-892c-3a1f64feae78
Kembhavi, A.K.
bd81f9d0-98e8-40a2-bc43-6eded7964d46
Mallick, Labani
15b17e80-7c5f-4cf4-a09e-a8bfcda3cd6e
Dewangan, G.C.
5ac9d24b-bcbb-45ab-a838-b093e67fc990
Gandhi, P.
5bc3b5af-42b0-4dd8-8f1f-f74048d4d4a9
Misra, R.
95702ea5-39c7-4579-892c-3a1f64feae78
Kembhavi, A.K.
bd81f9d0-98e8-40a2-bc43-6eded7964d46

Mallick, Labani, Dewangan, G.C., Gandhi, P., Misra, R. and Kembhavi, A.K. (2016) Accretion disc–corona and jet emission from the radio-loud narrow-line Seyfert 1 galaxy RX J1633.3+4719. Monthly Notices of the Royal Astronomical Society, 460 (2), 1705-1715. (doi:10.1093/mnras/stw1073).

Record type: Article

Abstract

We perform X-ray/ultraviolet (UV) spectral and X-ray variability studies of the radio-loud narrow-line Seyfert 1 (NLS1) galaxy RX J1633.3+4719 using XMM–Newton and Suzaku observations from 2011 and 2012. The 0.3–10 keV spectra consist of an ultrasoft component described by an accretion disc blackbody (kTin=39.6+11.2?5.5 eV) and a power law due to the thermal Comptonization (?=1.96+0.24?0.31) of the disc emission. The disc temperature inferred from the soft excess is at least a factor of 2 lower than that found for the canonical soft excess emission from radio-quiet NLS1s. The UV spectrum is described by a power law with photon index 3.05+0.56?0.33. The observed UV emission is too strong to arise from the accretion disc or the host galaxy, but can be attributed to a jet. The X-ray emission from RX J1633.3+4719 is variable with fractional variability amplitude Fvar = 13.5 ± 1.0?per?cent. In contrast to radio-quiet active galactic nuclei (AGN), X-ray emission from the source becomes harder with increasing flux. The fractional rms variability increases with energy and the rms spectrum is well described by a constant disc component and a variable power-law continuum with the normalization and photon index being anticorrelated. Such spectral variability cannot be caused by variations in the absorption and must be intrinsic to the hot corona. Our finding of possible evidence for emission from the inner accretion disc, jet and hot corona from RX J1633.3+4719 in the optical to X-ray bands makes this object an ideal target to probe the disc–jet connection in AGN.

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Accepted/In Press date: 3 May 2016
e-pub ahead of print date: 6 May 2016
Published date: 1 August 2016
Organisations: Astronomy Group

Identifiers

Local EPrints ID: 399899
URI: http://eprints.soton.ac.uk/id/eprint/399899
ISSN: 0035-8711
PURE UUID: c234e8f9-c7da-41c0-b49c-d9ccb872557c
ORCID for P. Gandhi: ORCID iD orcid.org/0000-0003-3105-2615

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Date deposited: 02 Sep 2016 10:45
Last modified: 10 Dec 2019 01:33

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