The Fast Uv Variability of the Active Galactic Nucleus in Fairall 9

Lohfink, A.; Reynolds, C. S.; Vasudevan, R. V.; Mushotzky, R. F.; Miller, Neal A.

doi:10.1088/0004-637x/788/1/10

Cited by 17 publications

(17 citation statements)

References 38 publications

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“…A possible solution includes contribution from both components, a thermal corona as well as a synchrotron jet (Soldi et al 2014). Such a combined model has been proposed for other radio galaxies as well, such as 3C120 (Lohfink et al 2014) and 3C273 (Grandi & Palumbo 2004;Madsen et al 2015a). However, as Rothschild et al (2006) and later Burke et al (2014) found, the X-ray continuum shape is remarkably stable over time, despite significant flux changes.…”

Section: The Geometry and Physics Of The X-ray Coronamentioning

confidence: 99%

NuSTAR AND XMM-NEWTON OBSERVATIONS OF THE HARD X-RAY SPECTRUM OF CENTAURUS A

Fürst

Müller

Madsen

et al. 2016

ApJ

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We present simultaneous XMM-Newton and Nuclear Spectroscopic Telescope Array (NuSTAR) observations spanning 3-78 keV of the nearest radio galaxy, CentaurusA (Cen A). The accretion geometry around the central engine in CenA is still debated, and we investigate possible configurations using detailed X-ray spectral modeling. NuSTAR imaged the central region of CenA with subarcminute resolution at X-ray energies above 10 keV for the first time, but found no evidence for an extended source or other off-nuclear point sources. The XMM-Newton and NuSTAR spectra agree well and can be described with an absorbed power law with a photon index Γ=1.815±0.005 and a fluorescent Fe Ka line in good agreement with literature values. The spectrum does not require a high-energy exponential rollover, with a constraint of E fold >1 MeV. A thermal Comptonization continuum describes the data well, with parameters that agree with values measured by INTEGRAL, in particular an electron temperature kT e between ≈100-300 keV and seed photon input temperatures between 5 and 50 eV. We do not find evidence for reflection or a broad iron line and put stringent upper limits of R<0.01 on the reflection fraction and accretion disk illumination. We use archival Chandra data to estimate the contribution from diffuse emission, extra-nuclear point sources, and the outer X-ray jet to the observed NuSTAR and XMM-Newton X-ray spectra and find the contribution to be negligible. We discuss different scenarios for the physical origin of the observed hard X-ray spectrum and conclude that the inner disk is replaced by an advection-dominated accretion flow or that the X-rays are dominated by synchrotron self-Compton emission from the inner regions of the radio jet or a combination thereof.

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Section: The Geometry and Physics Of The X-ray Coronamentioning

confidence: 99%

NuSTAR AND XMM-NEWTON OBSERVATIONS OF THE HARD X-RAY SPECTRUM OF CENTAURUS A

Fürst

Müller

Madsen

et al. 2016

ApJ

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“…Other than reddening, we also need to account for the host galaxy flux contribution to each of the filter band fluxes. We follow the procedure used in Lohfink et al (2014). Because the UVOT images are insufficient to perform a decomposition of the AGN and host galaxy contributions, we use the results from HST imaging as a basis.…”

Section: Swiftmentioning

confidence: 99%

The Corona of the Broad-Line Radio Galaxy 3c 390.3

Lohfink

Ogle

Tombesi

et al. 2015

ApJ

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We present the results from a joint Suzaku/NuSTAR broadband spectral analysis of 3C 390.3. The high quality data enables us to clearly separate the primary continuum from the reprocessed components allowing us to detect a high energy spectral cut-off (E 117 UV by studying the simultaneous Swift-UVOT data, we find indications that the compactness of the corona allows only a small fraction of the total UV/optical flux to be Comptonized. Our analysis of the reprocessed emission show that 3C 390.3 only has a small amount of reflection (R ∼ 0.3), and of that the vast majority is from distant neutral matter. However, we also discover a soft-X-ray excess in the source, which can be described by a weak ionized reflection component from the inner parts of the accretion disk. In addition to the backscattered emission, we also detect the highly ionized iron emission lines Fe XXV and Fe XXVI.cut

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“…Fairall 9 has also been observed in a number of multi-wavelength campaigns to probe the central engine including the broad line region (Chapman et al 1985;Wamsteker et al 1985;Morini et al 1986;Koratkar & Gaskell 1989;Recondo-Gonzalez et al 1997;Zheng et al 1995;Lohfink et al 2012bLohfink et al , 2014. Some of the campaigns cover only UV (Chapman et al 1985;Rodríguez-Pascual et al 1997;Koratkar & Gaskell 1989) or UV and optical (Wamsteker et al 1985;Lub & de Ruiter 1992;Santos-Lleó et al 1997) or UV and X-rays (Zheng et al 1995;Morini et al 1986) to search for possible correlation between continua at different wavelengths, and between the continuum and broad emission lines.…”

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confidence: 99%

“…; Lohfink et al 2014). Lohfink et al (2014) studied nearly a 2.5-months of data from a Swift monitoring campaign which revealed the UV signature of X-ray flares.…”

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Correlated X-ray/ultraviolet/optical variability and the nature of accretion disc in the bare Seyfert 1 galaxy Fairall 9

Pal

Dewangan

Connolly

et al. 2016

Mon. Not. R. Astron. Soc.

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We study multi-wavelength variability of a bare Seyfert 1 galaxy Fairall 9 using Swift monitoring observations consisting of 165 usable pointings spanning nearly two years and covering six UV/optical bands and X-rays. Fairall 9 is highly variable in all bands though the variability amplitude decreases from X-ray to optical bands.The variations in the X-ray and UV/optical bands are strongly correlated. Our reverberation mapping analysis using the JAVALIN tool shows that the variation in the UV/optical bands lag behind the variations in the X-ray band by ∼ 2 − 10 days.These lag measurements strongly suggest that the optical/UV variations are mainly caused by variations in the X-rays, and the origin of most of the optical/UV emission is X-ray reprocessing. The observed lags are found to vary as τ ∝ λ 1.36±0.13 , consistent with the prediction, τ ∝ λ 4/3 , for X-ray reprocessing in a standard accretion disc. However, the predicted lags for an standard accretion disc with X-ray reprocessing using black hole mass (M BH ∼ 2.6 × 10 8 M ⊙ ) estimated from the reverberation mapping of broad emission lines and accretion rate relative to the Eddington rate (ṁ E = 0.02) are shorter than the observed lags. These observations suggest that accretion disc in Fairall 9 is larger than that predicted by the standard disc model, and confirm similar findings in a few other Seyfert 1 galaxies such as NGC 5548.

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The Fast Uv Variability of the Active Galactic Nucleus in Fairall 9

Cited by 17 publications

References 38 publications

NuSTAR AND XMM-NEWTON OBSERVATIONS OF THE HARD X-RAY SPECTRUM OF CENTAURUS A

NuSTAR AND XMM-NEWTON OBSERVATIONS OF THE HARD X-RAY SPECTRUM OF CENTAURUS A

The Corona of the Broad-Line Radio Galaxy 3c 390.3

Correlated X-ray/ultraviolet/optical variability and the nature of accretion disc in the bare Seyfert 1 galaxy Fairall 9

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