Unveiling the broad band X-ray continuum and iron line complex in Mrk 841

Petrucci, P.-O.; Ponti, G.; Matt, Giorgio; Longinotti, A. L.; Malzac, J.; Mouchet, M.; Boisson, C.; Maraschi, L.; Nandra, K.; Ferrando, P.

doi:10.1051/0004-6361:20077787

Cited by 40 publications

(46 citation statements)

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“…Of course we know that the rms-spectra of AGN are not flat (e.g. Ponti et al 2004Ponti et al , 2006Ponti et al , 2007Ponti et al , 2010Gallo et al 2004Gallo et al , 2007Gierliński & Done 2006;Goosman et al 2006;Petrucci et al 2007;Larsson et al 2008;Zoghbi et al 2010). In other words, the components mentioned above, do affect the observed variability at different energy bands to some extent.…”

Section: σ 2 Rms In Various Energy Bandsmentioning

confidence: 99%

CAIXA: a catalogue of AGN in theXMM-Newtonarchive

Ponti

Papadakis

Bianchi

et al. 2012

A&A

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Context. We report on the results of the first XMM-Newton systematic "excess variance" study of all the radio quiet, X-ray un-obscured AGN. The entire sample consist of 161 sources observed by XMM-Newton for more than 10 ks in pointed observations, which is the largest sample used so far to study AGN X-ray variability on time scales less than a day. Aims. Recently it has been suggested that the same engine might be at work in the core of every black hole (BH) accreting object. In this hypothesis, the same variability should be observed in all AGN, once rescaled by the M BH (M BH ) and accretion rate (ṁ). Methods. We systematically compute the excess variance for all AGN, on different time-scales (10, 20, 40 and 80 ks) and in different energy bands (0.3-0.7, 0.7-2 and 2-10 keV). Results. We observe a highly significant and tight (∼0.7 dex) correlation between σ 2 rms and M BH . The subsample of reverberation mapped AGN shows an even smaller scatter (only a factor of 2-3) comparable to the one induced by the M BH uncertainties. This implies that X-ray variability can be used as an accurate tool to measure M BH and this method is more accurate than the ones based on single epoch optical spectra. This allows us to measure M BH for 65 AGN and estimate lower limits for the remaining 96 AGN. On the other hand, the σ 2 rms vs. accretion rate dependence is weaker than expected based on the PSD break frequency scaling. This strongly suggests that both the PSD high frequency break and the normalisation depend on accretion rate in such a way that they almost completely counterbalance each other (PSD amp ∝ṁ −0.8 ). A highly significant correlation between σ 2 rms and 2-10 keV spectral index is observed. The highly significant correlations between σ 2 rms and both the L Bol and the FWHM Hβ are consistent with being just by-products of the σ 2 rms vs. M BH relation. The soft and medium σ 2 rms is very well correlated with the hard σ 2 rms , with no deviations from a linear one to one correlation. This suggests that the additional soft components (i.e. soft excess, warm absorber) add a minor contribution to the total variability. Once the variability is rescaled for M BH andṁ, no significant difference between narrow-line and broad-line Seyfert 1 is observed. Conclusions. The results are in agreement with a picture where, to first approximation, all local AGN have the same variability properties once rescaled for M BH andṁ.

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Section: σ 2 Rms In Various Energy Bandsmentioning

confidence: 99%

CAIXA: a catalogue of AGN in theXMM-Newtonarchive

Ponti

Papadakis

Bianchi

et al. 2012

A&A

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“…A valid alternative model was proposed by Gierlinski & Done (2004) who explained the soft excess as arising from ionised absorption in a relativistically smeared wind. According to Petrucci et al (2007), both models were statistically indistinguishable in the EPIC data of Mrk 841. This paper presents the very first analysis of the highresolution soft X-ray spectra of Mrk 841, and it makes use of all the available XMM-Newton data sets, i.e., the five observations previously studied by Petrucci et al (2007).…”

Section: Introductionmentioning

confidence: 99%

“…The source varied significantly in flux and spectral shape over the time covered by XMM-Newton observations (see Table 1 and see Petrucci et al 2007 for an extensive discussion on the variability properties of the source). The soft X-ray flux decreased by a factor of ∼3.5 from 2001 to 2005, thus it is necessary to consider these two "epochs" separately.…”

Section: The Xmm-newton Observationsmentioning

confidence: 99%

“…Evidence for a moderately deep OVII absorption edge was also reported in ASCA data by Reynolds (1997). XMM-Newton data at CCD resolution highlighted the presence of a variable and complex narrow Fe Kα line (Petrucci et al 2002;Longinotti et al 2004;Petrucci et al 2007). Besides the study of Fe K band, the later paper focused on the analysis of the soft excess in Mrk 841 by testing two competing models.…”

Section: Introductionmentioning

confidence: 99%

“…In this paper, we present only the highresolution spectra gathered by the RGS instrument (den Herder et al 2001). For more details on the EPIC data and on the broadband spectrum, the reader is referred to Petrucci et al (2007). All the raw data were processed with SAS version 7.0.0.…”

Section: Introductionmentioning

confidence: 99%

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High-resolution X-ray spectroscopy of the Seyfert 1 Mrk 841: insights into the warm absorber and warm emitter

Longinotti

Costantini

Petrucci

et al. 2010

A&A

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Context. The Seyfert 1 galaxy Mrk 841 was observed five times between 2001 and 2005 by the XMM-Newton X-ray observatory. The source is well known for showing spectral complexity in the variable iron line and in the soft X-ray excess. Aims. The availability of multiple exposures obtained by the reflection grating spectrometer (RGS) cameras allows thorough study of the complex absorption and emission spectral features in the soft X-ray band. This paper reports on the first study of Mrk 841 soft X-ray spectrum at high spectral resolution. Methods. The three combined exposures obtained in January 2001 and the two obtained in January and July 2005 were analysed with the SPEX software. Results. We detect a two-phase warm absorber. A medium ionisation component (log ξ ∼ 1.5−2.2 erg s cm −1 ) is responsible for a deep absorption feature in the unresolved transition array of the Fe M-shell and for several absorption lines in the OVI-VIII band, and a higher ionisation phase with log ξ ∼ 3 erg s cm −1 is required to fit absorption in the NeIX-X band. The ionisation state and the column density of the gas present moderate variation from 2001 to 2005 for both phases. The high ionisation component of the warm absorber has no effect on the Fe K band. No significant velocity shift of the absorption lines is measured in the RGS data. Remarkably, the 2005 spectra show emission features consistent with photoionisation in a high-density (n e ≥ 10 11 cm −3 ) gas. A prominent OVII line triplet was clearly observed in January 2005 and narrow radiative recombination continua (RRC) of OVII and CVI were observed in both 2005 data sets. A broad Gaussian line around 21.7 Å was also required to fit all the data sets. The derived radial distance for the emission lines seems to suggest that the photoionisation takes place within the optical broad line region of the source.

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Active galaxies

Matt¹

2008

Astron Nachr

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In this paper I will review, in an unavoidably incomplete and biased way, the main results obtained by XMM-Newton on Active Galactic Nuclei. I will then highlight the major issues still open in which XMM-Newton can still give important contributions, expecially if the observing programs will shift in the future towards more long exposures of single objects and observations of large samples. I will also argue in favour of a legacy program consisting of good S/N observations of a flux-limited, sizeable sample of AGN. (C) 2008 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim

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Unveiling the broad band X-ray continuum and iron line complex in Mrk 841

Cited by 40 publications

References 42 publications

CAIXA: a catalogue of AGN in theXMM-Newtonarchive

CAIXA: a catalogue of AGN in theXMM-Newtonarchive

High-resolution X-ray spectroscopy of the Seyfert 1 Mrk 841: insights into the warm absorber and warm emitter

Active galaxies

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