<i>XMM</i>–<i>Newton</i>observations of the Seyfert 1 galaxy ESO 141–G55

Gondoin, P.; Orr, A.; Lumb, D.

doi:10.1051/0004-6361:20021694

Cited by 14 publications

(8 citation statements)

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“…This also explains the low to moderate ionization state of the disk. These relatively lower values are consistent with the 2001 XMM-Newton observation (Gondoin et al 2003) and other Seyfert 1s as well, e.g., Zw 229.015, where these values are log ξ = 2.56 +0.15 −0.15 erg cm s −1 and R ∼ 0.4. The iron abundance of the material in the accretion disk and the inclination of the disk to the line of sight plays an important role in describing the reflected spectra of Seyfert 1 galaxies (Crummy et al 2006;García et al 2014).…”

Section: The Soft Excesssupporting

confidence: 90%

“…In this work, we take a broadband spectroscopic approach to address the origin of the soft excess, the Fe K line complex and the Compton hump at E > 10 keV in the Seyfert 1 galaxy ESO 141-G055 (Elvis et al 1978) where the presence of soft excess and Fe line have been affirmatively detected by previous studies (Turner et al 1993;Gondoin et al 2003). A recent NuSTAR observation in 2016 gives us a rare opportunity to take a hard Xray (> 10 keV) look of this source.…”

Section: Introductionmentioning

confidence: 99%

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A broadband X-ray spectral study of the Seyfert 1 galaxy ESO 141--G055 with XMM-Newton and NuSTAR

Ghosh,

Laha

2020

Preprint

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We have extensively studied the broadband X-ray spectra of the source ESO 141-G055 using all available XMM-Newton and NuSTAR observations. We detect a prominent soft excess below 2 keV, a narrow Fe line and a Compton hump (> 10 keV). The origin of the soft excess is still debated. We used two models to describe the soft excess: the blurred reflection from the ionized accretion disk and the intrinsic thermal Comptonisation model. We find that both of these models explain the soft excess equally well. We confirm that we do not detect any broad Fe line in the X-ray spectra of this source, although both the physical models prefer a maximally spinning black hole scenario (a>0.96). This may mean that either the broad Fe line is absent or blurred beyond detection. The Eddington rate of the source is estimated to be λ Edd ∼ 0.31. In the reflection model, the Compton hump has a contribution from both ionized and neutral reflection components. The neutral reflector which simultaneously describes the narrow Fe Kα and the Compton hump has a column density of N H 7 × 10 24 cm −2 . In addition, we detect a partially covering ionized absorption with ionization parameter log ξ/ erg cm s −1 = 0.1 +0.1 −0.1 and column density N H = 20.6 +1.0 −1.0 × 10 22 cm −2 with a covering factor of 0.21 +0.01 −0.01 .

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Section: The Soft Excesssupporting

confidence: 90%

Section: Introductionmentioning

confidence: 99%

A broadband X-ray spectral study of the Seyfert 1 galaxy ESO 141--G055 with XMM-Newton and NuSTAR

Ghosh,

Laha

2020

Preprint

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“…We note that, since submission of this paper the 2000 November XMM–Newton observation of NGC 3227 has also been published by Gondoin et al (2003). They fit a slightly different model to us, we refer readers to Gondoin et al for a full discussion of their model.…”

Section: A Transient Absorption Eventmentioning

confidence: 91%

An absorption event in the X-ray light curve of NGC 3227

Lamer

Uttley

McHardy

2003

Monthly Notices of the Royal Astronomical Society

119

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We have monitored the Seyfert galaxy NGC 3227 with the Rossi X‐ray Timing Explorer (RXTE) since 1999 January. During late 2000 and early 2001 we observed an unusual hardening of the 2–10 keV X‐ray spectrum which lasted several months. The spectral hardening was not accompanied by any correlated variation in flux above 8 keV. We therefore interpret the spectral change as transient absorption by a gas cloud of column density 2.6 × 1023 cm−2 crossing the line of sight to the X‐ray source. A spectrum obtained by XMM–Newton during an early phase of the hard‐spectrum event confirms the obscuration model and shows that the absorbing cloud is only weakly ionized. The XMM–Newton spectrum also shows that ∼10 per cent of the X‐ray flux is not obscured, but this unabsorbed component is not significantly variable and may be scattered radiation from a large‐scale scattering medium. Applying the spectral constraints on the cloud ionization parameter and assuming that the cloud follows a Keplerian orbit, we constrain the location of the cloud to be R∼ 10–100 light‐days from the central X‐ray source, and its density to be nH∼ 108 cm−3, implying that we have witnessed the eclipse of the X‐ray source by a broad line region cloud.

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“…Although Scott et al (2004) found no significant evidence of X-ray warm absorption, this source does have an intrinsic UV absorber, making it very likely that an X-ray absorber will be found in better quality data in future; Crenshaw et al (1999) found that objects in their sample with UV absorption always showed evidence of an X-ray absorber. The one remaining object without a warm absorber, ESO 141-G55 (Gondoin et al 2003) is towards the high end of the L bol −redshift distribution, but there does not seem to be anything significantly unusual about it with respect to the other sources. NGC 4258 is basically a Seyfert 2-type object, without a soft X-ray absorber; it has however been claimed to exhibit absorption lines above 6 keV (Young & Wilson 2004).…”

Section: The Prevalence Of Warm Absorbersmentioning

confidence: 92%

The nature and origin of Seyfert warm absorbers

Blustin

Page

Fuerst

et al. 2005

A&A

347

539

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Abstract.We collate the results of recent high resolution X-ray spectroscopic observations of 23 AGN, and use the resulting information to try to provide answers to some of the main open questions about warm absorbers: where do they originate, what effect do they have on their host galaxies, and what is their importance within the energetics and dynamics of the AGN system as a whole? We find that the warm absorbers of nearby Seyferts and certain QSOs are most likely to originate in outflows from the dusty torus, and that the kinetic luminosity of these outflows accounts for well under 1% of the bolometric luminosities of the AGN. Our analysis supports, however, the view that the relativistic outflows recently observed in two PG quasars have their origin in accretion disc winds, although the energetic importance of these outflows is similar to that of the Seyfert warm absorbers. We find that the observed soft X-ray absorbing ionisation phases fill less than 10% of the available volume. Finally, we show that the amount of matter processed through an AGN outflow system, over the lifetime of the AGN, is probably large enough to have a significant influence on the evolution of the host galaxy and of the AGN itself.

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XMM–Newtonobservations of the Seyfert 1 galaxy ESO 141–G55

Cited by 14 publications

References 50 publications

A broadband X-ray spectral study of the Seyfert 1 galaxy ESO 141--G055 with XMM-Newton and NuSTAR

A broadband X-ray spectral study of the Seyfert 1 galaxy ESO 141--G055 with XMM-Newton and NuSTAR

An absorption event in the X-ray light curve of NGC 3227

The nature and origin of Seyfert warm absorbers

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