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dc.contributor.authorLandt, Hermine
dc.contributor.authorMitchell, Jake A. J.
dc.contributor.authorWard, Martin J.
dc.contributor.authorMercatoris, Paul
dc.contributor.authorPott, Jörg-Uwe
dc.contributor.authorHorne, Keith
dc.contributor.authorHernández Santisteban, Juan V.
dc.contributor.authorMalhotra, Daksh
dc.contributor.authorCackett, Edward M.
dc.contributor.authorGoad, Michael R.
dc.contributor.authorRomero Colmenero, Encarni
dc.contributor.authorWinkler, Hartmut
dc.date.accessioned2023-03-08T11:30:08Z
dc.date.available2023-03-08T11:30:08Z
dc.date.issued2023-03-07
dc.identifier283657897
dc.identifierf1c3149f-2457-4a62-806e-460bb4d1d289
dc.identifier85149892823
dc.identifier.citationLandt , H , Mitchell , J A J , Ward , M J , Mercatoris , P , Pott , J-U , Horne , K , Hernández Santisteban , J V , Malhotra , D , Cackett , E M , Goad , M R , Romero Colmenero , E & Winkler , H 2023 , ' A complex dust morphology in the high-luminosity AGN Mrk 876 ' , Astrophysical Journal , vol. 945 , 62 . https://doi.org/10.3847/1538-4357/acb92den
dc.identifier.issn0004-637X
dc.identifier.otherJisc: 943713
dc.identifier.otherpublisher-id: apjacb92d
dc.identifier.othermanuscript: acb92d
dc.identifier.otherother: aas43933
dc.identifier.otherORCID: /0000-0002-6733-5556/work/130660135
dc.identifier.urihttps://hdl.handle.net/10023/27126
dc.descriptionFunding: H.L. acknowledges a Daphne Jackson Fellowship, sponsored by the Science and Technology Facilities Council (STFC), UK. J.A.J.M. acknowledges the support of STFC studentship ST/S50536/1. H.L., J.A.J.M., and M.J.W. acknowledge support from STFC grants ST/P000541/1 and ST/T000244/1. K.H. and J.V.H.S. acknowledge support from STFC grant ST/R000824/1. E.R.C. acknowledges the support of the South African National Research Foundation.en
dc.description.abstractRecent models for the inner structures of active galactic nuclei (AGNs) advocate the presence of a radiatively accelerated dusty outflow launched from the outer regions of the accretion disk. Here, we present the first near-IR variable (rms) spectrum for the high-luminosity nearby AGN Mrk 876. We find that it tracks the accretion disk spectrum out to longer wavelengths than the mean spectrum, due to a reduced dust emission. The implied outer accretion disk radius is consistent with the IR results predicted by a contemporaneous optical accretion disk reverberation mapping campaign, and much larger than the self-gravity radius. The reduced flux variability of the hot dust could either be due to the presence of a secondary constant dust component in the mean spectrum or be introduced by the destructive superposition of the dust and accretion disk variability signals, or be some combination of the two. Assuming thermal equilibrium for optically thin dust, we derive the luminosity-based dust radii for different grain properties, using our measurement of the temperature. We find that in all the cases considered, the values are significantly larger than the dust response time measured by IR photometric monitoring campaigns, with the least discrepancy present relative to the result for a wavelength-independent dust emissivity law, i.e., a blackbody, which is appropriate for large grain sizes. This result can be well explained by assuming a flared disk-like structure for the hot dust.
dc.format.extent13
dc.format.extent1253252
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.subjectQB Astronomyen
dc.subjectNDASen
dc.subjectMCCen
dc.subject.lccQBen
dc.titleA complex dust morphology in the high-luminosity AGN Mrk 876en
dc.typeJournal articleen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews. St Andrews Centre for Exoplanet Scienceen
dc.identifier.doihttps://doi.org/10.3847/1538-4357/acb92d
dc.description.statusPeer revieweden


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