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dc.contributor.authorVasquez, Billypt_BR
dc.contributor.authorGalianni, Pasqualept_BR
dc.contributor.authorRichmond, Michaelpt_BR
dc.contributor.authorRobinson, Andrewpt_BR
dc.contributor.authorAxon, David J.pt_BR
dc.contributor.authorHorne, Keithpt_BR
dc.contributor.authorAlmeyda, Trianapt_BR
dc.contributor.authorFausnaugh, Michaelpt_BR
dc.contributor.authorPeterson, Bradley M.pt_BR
dc.contributor.authorBottorff, Markpt_BR
dc.contributor.authorGallimore, Jack F.pt_BR
dc.contributor.authorElitzur, Moshept_BR
dc.contributor.authorNetzer, Hagaipt_BR
dc.contributor.authorStorchi-Bergmann, Thaisapt_BR
dc.contributor.authorMarconi, A.pt_BR
dc.contributor.authorCapetti, A.pt_BR
dc.contributor.authorBatcheldor, Danpt_BR
dc.contributor.authorBuchanan, Catherinept_BR
dc.contributor.authorStirpe, Giovanna M.pt_BR
dc.contributor.authorKishimoto, Makotopt_BR
dc.contributor.authorPackham, Christopherpt_BR
dc.contributor.authorPérez Jiménez, Enriquept_BR
dc.contributor.authorTadhunter, Clivept_BR
dc.contributor.authorUpton, Johnpt_BR
dc.contributor.authorEstrada-Carpenter, Vicentept_BR
dc.date.accessioned2015-05-16T02:00:39Zpt_BR
dc.date.issued2015pt_BR
dc.identifier.issn0004-637Xpt_BR
dc.identifier.urihttp://hdl.handle.net/10183/116505pt_BR
dc.description.abstractWe present results from a 15 month campaign of high-cadence (∼3 days) mid-infrared Spitzer and optical (B and V) monitoring of the Seyfert 1 galaxy NGC 6418, with the objective of determining the characteristic size of the dusty torus in this active galactic nucleus (AGN). We find that the 3.6 and 4.5 μm flux variations lag behind those of the optical continuum by - 37.2+2.2 2.4 days and - 47.1+3.1 3.1 days, respectively. We report a cross-correlation time lag between the 4.5 and 3.6 μm flux of - 13.9+0.1 0.5 days. The lags indicate that the dust emitting at 3.6 and 4.5 μm is located at a distance ≈1 light-month (≈0.03 pc) from the source of the AGN UV–optical continuum. The reverberation radii are consistent with the inferred lower limit to the sublimation radius for pure graphite grains at 1800 K, but smaller by a factor of ∼2 than the corresponding lower limit for silicate grains; this is similar to what has been found for near-infrared (K-band) lags in other AGNs. The 3.6 and 4.5 μm reverberation radii fall above the K-band t ∝ L0.5 size–luminosity relationship by factors <~2.7 and <~3.4, respectively, while the 4.5 μm reverberation radius is only 27% larger than the 3.6 μm radius. This is broadly consistent with clumpy torus models, in which individual optically thick clouds emit strongly over a broad wavelength range.en
dc.format.mimetypeapplication/pdf
dc.language.isoengpt_BR
dc.relation.ispartofThe astrophysical journal. Bristol. Vol. 801, no. 2 (Mar. 2015), 127, 11 p.pt_BR
dc.rightsOpen Accessen
dc.subjectGalaxias seyfertpt_BR
dc.subjectGalaxies: activeen
dc.subjectGaláxias ativaspt_BR
dc.subjectGalaxies: individual (NGC 6418)en
dc.subjectNucleo galaticopt_BR
dc.subjectGalaxies: nucleien
dc.subjectGalaxies: Seyferten
dc.subjectAstronomia infravermelhapt_BR
dc.subjectPoeira cosmicapt_BR
dc.subjectEspectros astronômicospt_BR
dc.titleSpitzer space telescope measurements of dust reverberation lags in the Seyfert 1 galaxy NGC 6418pt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb000965715pt_BR
dc.type.originEstrangeiropt_BR


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