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dc.contributor.authorGonzalez-Martin, O.-
dc.contributor.authorPapadakis, I.-
dc.contributor.authorBraito, V.-
dc.contributor.authorMasegosa, J.-
dc.contributor.authorMarquez, I.-
dc.contributor.authorMateos, S.-
dc.contributor.authorAcosta-Pulido, J. A.-
dc.contributor.authorMartinez, M. A.-
dc.contributor.authorEbrero, J.-
dc.contributor.authorEsquej, P.-
dc.contributor.authorO'Brien, P.-
dc.contributor.authorTueller, J.-
dc.contributor.authorWarwick, R. S.-
dc.contributor.authorWatson, M. G.-
dc.identifier.citationAstronomy & Astrophysics, 2011, 527-
dc.description.abstractContext. Low-ionisation, nuclear emission-line region (LINER) nuclei are said to be different from other active galactic nuclei (AGN) due to the presence of complex absorbing structures along the line-of-sight and/or an inefficient mode of accretion onto the supermassive black hole. However, this is still open. Aims. We investigate the broad band X-ray spectrum of NGC 4102, one of the most luminous LINERs in the Swift/BAT survey. Methods. We studied a 80 ks Suzaku spectrum of NGC 4102, together with archival Chandra and Swift/BAT observations. We also studied the optical (3.5 m/TWIN at Calar Alto observatory) and near-infrared (WHT/LIRIS at Observatorio Roque los Muchachos) spectra that were taken at the same time as the Suzaku data. Results. There is strong evidence that NGC 4102 is a Compton-thick AGN, as suggested by the Swift/BAT detected intrinsic continuum and the presence of a strong narrow, neutral FeKα emission line. We have also detected ionised FeXXV emission lines in the Suzaku spectrum of the source. NGC 4102 shows a variable soft excess found at a significantly higher flux state at the time of Suzaku observations when compared to Chandra observations. Finally, a complex structure of absorbers is seen with at least two absorbers besides the Compton-thick one, derived from the X-ray spectral analysis and the optical extinction. Conclusions. All the signatures described in this paper strongly suggest that NGC 4102 is a Compton-thick Type-2 AGN from the X-ray point of view. The “soft excess”, the electron scattered continuum component, and the ionised iron emission line might arise from Compton-thin material photoionised by the AGN. From variability and geometrical arguments, this material should be located somewhere between 0.4 and 2 pc away from the nuclear source, inside the torus and perpendicular to the disc. The bolometric luminosity (Lbol = 1.4 × 1043 erg s-1) and accretion rate (ṁEdd = 5.4 × 10-3) are consistent with other low-luminosity AGN. However, the optical and near infrared spectra correspond to that of a LINER source. We suggest that the LINER classification might be due a different spectral energy distribution according to its steeper spectral index.-
dc.publisherEDP Sciences for European Southern Observatory (ESO)-
dc.rightsCopyright © 2011 ESO. Reproduced with permission from Astronomy & Astrophysics, © ESO.-
dc.sourceWeb of Science-
dc.subjectScience & Technology-
dc.subjectPhysical Sciences-
dc.subjectAstronomy & Astrophysics-
dc.subjectgalaxies: active-
dc.subjectgalaxies: nuclei-
dc.subjectgalaxies: Seyfert-
dc.subjectgalaxies: individual: NGC 4102-
dc.subjectX-ray: galaxies-
dc.subjectBLACK-HOLE MASS-
dc.subjectHOST GALAXIES-
dc.titleSuzaku observation of the LINER NGC4102-
dc.typeJournal Article-
dc.description.versionPublisher Version-
Appears in Collections:Published Articles, Dept. of Physics and Astronomy

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