High resolution X-ray spectroscopy of the Seyfert 1 Mrk841: insights into the warm absorber and warm emitter - Astrophysics > High Energy Astrophysical PhenomenaReport as inadecuate




High resolution X-ray spectroscopy of the Seyfert 1 Mrk841: insights into the warm absorber and warm emitter - Astrophysics > High Energy Astrophysical Phenomena - Download this document for free, or read online. Document in PDF available to download.

Abstract: The Seyfert 1 galaxy Mrk841 was observed five times between 2001 and 2005 bythe XMM-Newton X-ray observatory. The source is well known for showing spectralcomplexity in the variable iron line and in the soft X-ray excess. This paperreports on the first study of Mrk841 soft X-ray spectrum at high spectralresolution. The availability of multiple exposures obtained by the ReflectionGrating Spectrometer RGS cameras allows a thorough study of the complexabsorption and emission spectral features in the soft X-ray band.The threecombined exposures obtained in January 2001 and the two obtained in January andJuly 2005 were analysed using the SPEX software. We detect a two-phase warmabsorber: a medium ionisation component logxi~1.5-2.2 ergs s cm^{-1} isresponsible for a deep absorption feature in the Unresolved Transition Array ofthe Fe M-shell and for several absorption lines in the OVI-VIII band; a higherionisation phase with logxi~3 ergs s cm^{-1} is required to fit absorption inthe NeIX-X band. The ionisation state and the column density of the gas presentmoderate variation from 2001 to 2005 for both phases. The high ionisationcomponent of the warm absorber has no effect in the Fe K band. No significantvelocity shift of the absorption lines is measured in the RGS data. Remarkably,the 2005 spectra show emission features consistent with photoionisation in ahigh density n e>10^{11} cm^{-3} gas: a prominent OVII line triplet isclearly observed in January 2005 and narrow Radiative Recombination ContinuaRRC of OVII and CVI are observed in both 2005 data sets. A broad Gaussianline around 21.7 Angstrom is also required to fit all the data sets. Thederived radial distance for the emission lines seems to suggest that thephotoionisation takes place within the optical Broad Line Region of the source.



Author: A.L. Longinotti, E. Costantini, P.O. Petrucci, C. Boisson, M. Mouchet, M. Santos-Lleo, G. Matt, G. Ponti, A. C. Goncalves

Source: https://arxiv.org/







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