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dc.contributor.author
Dors, Oli L.
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Riffel, Rogemar A.
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Cardaci, Monica Viviana
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Hägele, Guillermo Federico
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Krabbe, Angela
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Pérez Montero, Enrique
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Rodrigues, Irapuan
dc.date.available
2018-04-19T14:53:36Z
dc.date.issued
2012-05
dc.identifier.citation
Dors, Oli L.; Riffel, Rogemar A.; Cardaci, Monica Viviana; Hägele, Guillermo Federico; Krabbe, Angela; et al.; X-rays as the dominant excitation mechanism of [Fe II] and H2 emission lines in active galaxies; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 422; 1; 5-2012; 252-260
dc.identifier.issn
0035-8711
dc.identifier.uri
http://hdl.handle.net/11336/42650
dc.description.abstract
We investigate the excitation mechanisms of near-infrared [Fe II] and H2 emission lines observed in active galactic nuclei (AGNs). We built a photoionization model grid considering a two-component continuum: one component accounts for the `big bump´ component peaking at 1Ryd and another represents the X-ray source that dominates the continuum emission at high energies. Photoionization models considering as ionizing source a spectral energy distribution obtained from photometric data of Seyfert 2 Mrk 1066 taken from the literature were considered. Results of these models were compared with a large sample of observational long-slit and Integral field Unit (IFU) spectroscopy data of the nuclear region for a sample of active objects. We found that the correlation between the observational [Fe II] lambda 1.2570μm/Pa beta and H2 lambda 2.1218μm/Brγ is well reproduced by our models, as are the relationships that involve the H2 emission-line ratios observed in the spectroscopic data. We conclude that heating by X-rays produced by active nuclei can be considered a common and very important mechanism of excitation of [Fe II] and H2.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
Wiley Blackwell Publishing, Inc
dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
Galaxies
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Seyfert Galaxies
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Infrared Galaxies
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Interstellar Medium
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Astronomía
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Ciencias Físicas
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CIENCIAS NATURALES Y EXACTAS
dc.title
X-rays as the dominant excitation mechanism of [Fe II] and H2 emission lines in active galaxies
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2018-04-16T14:55:49Z
dc.journal.volume
422
dc.journal.number
1
dc.journal.pagination
252-260
dc.journal.pais
Reino Unido
dc.description.fil
Fil: Dors, Oli L.. Universidade Do Vale Do Paraíba; Brasil
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Fil: Riffel, Rogemar A.. Universidade Federal de Santa Maria; Brasil
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Fil: Cardaci, Monica Viviana. Universidad Autónoma de Madrid. Facultad de Ciencias; España. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
dc.description.fil
Fil: Hägele, Guillermo Federico. Universidad Autónoma de Madrid. Facultad de Ciencias; España. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
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Fil: Krabbe, Angela. Universidade Do Vale Do Paraíba; Brasil
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Fil: Pérez Montero, Enrique. Inst. de Astrofísica de Andalucía; España
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Fil: Rodrigues, Irapuan. Universidade Do Vale Do Paraíba; Brasil
dc.journal.title
Monthly Notices of the Royal Astronomical Society
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1111/j.1365-2966.2012.20600.x
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/422/1/252/1020740
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