Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12666/257
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dc.rights.licensePublished 2020 February 24 • © 2020. The American Astronomical Society. All rights reserved.-
dc.contributor.authorMartínez Paredes, M.-
dc.contributor.authorGonzález Martín, O.-
dc.contributor.authorEsparza Arredondo, D.-
dc.contributor.authorKim, M.-
dc.contributor.authorAlonso Herrero, A.-
dc.contributor.authorKrongold, Y.-
dc.contributor.authorHoang, T.-
dc.contributor.authorRamos Almeida, C.-
dc.contributor.authorAretxaga, I.-
dc.contributor.authorDultzin, D.-
dc.contributor.authorHodgson, J.-
dc.contributor.otherUnidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737-
dc.date.accessioned2021-04-12T10:48:35Z-
dc.date.available2021-04-12T10:48:35Z-
dc.date.issued2020-02-24-
dc.identifier.citationThe Astrophysical Journal 890(2): 152(2020)es
dc.identifier.issn0004-637X-
dc.identifier.otherhttps://iopscience.iop.org/article/10.3847/1538-4357/ab6732-
dc.identifier.urihttp://hdl.handle.net/20.500.12666/257-
dc.description.abstractWe measure the 10 and 18 μm silicate features in a sample of 67 local (z < 0.1) type 1 active galactic nuclei (AGN) with available Spitzer spectra dominated by nonstellar processes. We find that the 10 μm silicate feature peaks at ${10.3}_{-0.9}^{+0.7}\,\mu {\rm{m}}$ with a strength (Sip = ln fp(spectrum)/fp(continuum)) of ${0.11}_{-0.36}^{+0.15}$, while the 18 μm one peaks at ${17.3}_{-0.7}^{+0.4}\,\mu {\rm{m}}$ with a strength of ${0.14}_{-0.06}^{+0.06}$. We select from this sample sources with the strongest 10 μm silicate strength (${\sigma }_{{\mathrm{Si}}_{10\mu {\rm{m}}}}\gt 0.28$, 10 objects). We carry out a detailed modeling of the infrared spectrometer/Spitzer spectra by comparing several models that assume different geometries and dust composition: a smooth torus model, two clumpy torus models, a two-phase medium torus model, and a disk+outflow clumpy model. We find that the silicate features are well modeled by the clumpy model of Nenkova et al., and among all models, those including outflows and complex dust composition are the best. We note that even in AGN-dominated galaxies, it is usually necessary to add stellar contributions to reproduce the emission at the shortest wavelengths.es
dc.description.sponsorshipWith funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)es
dc.language.isoenges
dc.publisherThe Institute of Physics (IOP)es
dc.rightsAttribution-NonCommercial-NoDerivatives 4.0 International*
dc.rights.urihttps://creativecommons.org/licenses/by-nc-nd/4.0/*
dc.subjectActive galactic nucleies
dc.subjectInfrared astronomyes
dc.subjectDust continuum emissiones
dc.subjectActive galaxieses
dc.titleModeling the Strongest Silicate Emission Features of Local Type 1 AGNses
dc.typeinfo:eu-repo/semantics/articlees
dc.contributor.orcidMartínez Paredes, M. [0000-0002-0088-0103]-
dc.contributor.orcidGonzález Martín, O. [0000-0002-2356-8358]-
dc.contributor.orcidHoang, T. [0000-0003-2017-0982]-
dc.contributor.orcidAretzaga, I. [0000-0002-6590-3994]-
dc.identifier.doi10.3847/1538-4357/ab6732-
dc.identifier.e-issn1538-4357-
dc.description.peerreviewedPeer reviewes
dc.type.hasVersioninfo:eu-repo/semantics/publishedVersion-
dc.rights.accessRightsinfo:eu-repo/semantics/openAccess-
dc.type.coarhttp://purl.org/coar/resource_type/c_6501-
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