X-ray evidence for a mildly relativistic and variable outflow   in the luminous Seyfert 1 galaxy Mrk 509

Cappi, M.; Tombesi, Francesco; Bianchi, S.; Dadina, M.; Giustini, M.; Malaguti, G.; Maraschi, L.; Palumbo, G. G. C.; Petrucci, Pierre-Olivier; Ponti, G.; Vignali, C.; Yaqoob, T.

doi:10.1051/0004-6361/200912137

Cited by 90 publications

(127 citation statements)

References 37 publications

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“…In summary, we do not find significant evidence of an ultrafast outflow in this Chandra HETGS observation of Mrk 509, in spite of previous detections by Cappi et al (2009) and Ponti et al (2009). This result is in line with the observation of no signatures of such outflows in the combined 600 ks XMM-Newton pn spectrum, with the exception of a marginal detection of two absorption features at 9 keV and 10.2 keV (Ponti et al 2013) during observation 4 which could be attributed to Fe xxvi outflowing at ∼−0.3c.…”

Section: Ultra-fast Outflowscontrasting

confidence: 99%

“…The lack of detection of these features, previously reported in other Mrk 509 observations (Dadina et al 2005;Cappi et al 2009;Ponti et al 2009), might be due to intrinsic time variability, as they are formed very close to the accretion disc.…”

Section: Discussionmentioning

confidence: 63%

“…7.1 we showed that the presence of such lines is not statistically significant at the expected blueshifts for an ultra-fast outflow. However, given the statistical uncertainties we also cannot rule out such lines at the strength of about 20 eV equivalent width as reported by Cappi et al (2009). For this equivalent width, we derive a hydrogen column density of 1.2 × 10 26 and 3.1 × 10 26 m −2 for Fe xxv and Fe xxvi, respectively.…”

Section: Ultra-fast Outflowsmentioning

confidence: 79%

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Multiwavelength campaign on Mrk 509

Kaastra

Ebrero

Arav

et al. 2014

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Context. We present in this paper the results of a 270 ks Chandra HETGS observation in the context of a large multiwavelength campaign on the Seyfert galaxy Mrk 509. Aims. The HETGS spectrum allows us to study the high ionisation warm absorber and the Fe-K complex in Mrk 509. We search for variability in the spectral properties of the source with respect to previous observations in this campaign, as well as for evidence of ultra-fast outflow signatures. Methods. The Chandra HETGS X-ray spectrum of Mrk 509 was analysed using the SPEX fitting package. Results. We confirm the basic structure of the warm absorber found in the 600 ks XMM-Newton RGS observation observed three years earlier, consisting of five distinct ionisation components in a multikinematic regime. We find little or no variability in the physical properties of the different warm absorber phases with respect to previous observations in this campaign, except for component D2 which has a higher column density at the expense of component C2 at the same outflow velocity (−240 km s −1 ). Contrary to prior reports we find no −700 km s −1 outflow component. The O viii absorption line profiles show an average covering factor of 0.81 ± 0.08 for outflow velocities faster than −100 km s −1 , similar to those measured in the UV. This supports the idea of a patchy wind. The relative metal abundances in the outflow are close to proto-solar. The narrow component of the Fe Kα emission line shows no changes with respect to previous observations which confirms its origin in distant matter. The narrow line has a red wing that can be interpreted to be a weak relativistic emission line. We find no significant evidence of ultra-fast outflows in our new spectrum down to the sensitivity limit of our data.

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Section: Ultra-fast Outflowscontrasting

confidence: 99%

Section: Discussionmentioning

confidence: 63%

Section: Ultra-fast Outflowsmentioning

confidence: 79%

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Multiwavelength campaign on Mrk 509

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Ebrero

Arav

et al. 2014

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“…EPIC data from XMM-Newton observations (in 2000, 2001, 2005, and 2006) show evidence of a complex Fe K emission line, with a narrow and a neutral component possibly produced far from the source, plus a broad and variable component possibly originating in the accretion disk (Pounds et al 2001;Page et al 2003;Ponti et al 2009Ponti et al , 2013. Using XMM-Newton observations of Mrk 509, Cappi et al (2009) detected the presence of lines, at ∼8-8.5 keV and ∼9.7 keV, consistent with being produced by Fe Kα and Kβ shell absorptions associated with mildly relativistic and variable outflow. These variable features were not observed during the 2009 campaign .…”

Section: Mrk 509 -Xmm-newton/integral Campaignmentioning

confidence: 99%

Multiwavelength campaign on Mrk 509

Boissay

Paltani

Ponti

et al. 2014

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Active galactic nuclei (AGN) are the most luminous persistent objects in the universe. The X-ray domain is particularly important because the X-ray flux represents a significant fraction of the bolometric emission from such objects and probes the innermost regions of accretion disks, where most of this power is generated. An excess of X-ray emission below ∼2 keV, called soft-excess, is very common in Type 1 AGN spectra. The origin of this feature remains debated. Originally modeled with a blackbody, there are now several possibilities to model the soft-excess, including warm Comptonization and blurred ionized reflection. In this paper, we test ionized-reflection models on Mrk 509, a bright Seyfert 1 galaxy for which we have a unique data set, in order to determine whether it can be responsible for the strong soft-excess. We use ten simultaneous XMM-Newton and INTEGRAL observations performed every four days. We present here the results of the spectral analysis, the evolution of the parameters, and the variability properties of the X-ray emission. The application of blurred ionized-reflection models leads to a very strong reflection and an extreme geometry, but fails to reproduce the broad-band spectrum of Mrk 509. Two different scenarios for blurred ionized reflection are discussed: stable geometry and lamp-post configuration. In both cases we find that the model parameters do not follow the expected relations, indicating that the model is fine-tuned to fit the data without physical justification. A large, slow variation in the soft-excess without a counterpart in the hard X-rays could be explained by a change in ionization of the reflector. However, such a change does not naturally follow from the assumed geometrical configuration. Warm Comptonization remains the most probable origin of the soft-excess in this object. Nevertheless, it is possible that both ionized reflection and warm Comptonization mechanisms can explain the soft-excess in all objects, one dominating the other one, depending on the physical conditions of the disk and the corona.

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“…We use this study as a starting point for our analysis of the three new observations taken in 2005 and 2006. Using these data, Cappi et al (2009) found evidence of a highly ionized and mildly relativistic outflow. Clearly, Mrk 509 is an excellent source to investigate in further detail.…”

Section: Introductionmentioning

confidence: 99%

The outflow in Mrk 509

Detmers¹,

Kaastra

Costantini³

et al. 2010

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We analyzed three XMM-Newton observations of the Seyfert 1 galaxy Mrk 509, with the goal of detecting small variations in the ionized outflow properties. Measurements such as these are limited by the quality of the cross-calibration between RGS, the best instrument for characterizing the spectrum, and EPIC-pn, the best instrument for characterizing the variability. For all three observations we are able to improve the relative calibration of RGS and pn consistently to 4%. In all observations we detect three different outflow components and, thanks to our accurate cross-calibration, we are able to detect small differences in the ionization parameter and column density in the highest ionized component of the outflow. This constrains the location of this component of the outflow to within 0.5 pc of the central source. Our method for modeling the relative effective area is not restricted to just this source and can in principle be extended to other types of sources as well.

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X-ray evidence for a mildly relativistic and variable outflow in the luminous Seyfert 1 galaxy Mrk 509

Cited by 90 publications

References 37 publications

Multiwavelength campaign on Mrk 509

Multiwavelength campaign on Mrk 509

Multiwavelength campaign on Mrk 509

The outflow in Mrk 509

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