Galaxy and Mass Assembly (GAMA): active galactic nuclei in pairs of galaxies

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dc.contributor.authorGordon, Yjan A.
dc.contributor.authorOwers, Matt S.
dc.contributor.authorPimbblet, Kevin A.
dc.contributor.authorCroom, Scott M.
dc.contributor.authorAlpaslan, Mehmet
dc.contributor.authorBaldry, Ivan K.
dc.contributor.authorBrough, Sarah
dc.contributor.authorBrown, Michael J. I.
dc.contributor.authorCluver, Michelle E.
dc.contributor.authorConselice, Christopher J.
dc.contributor.authorDavies, Luke J. M.
dc.contributor.authorHolwerda, Benne W.
dc.contributor.authorHopkins, Andrew M.
dc.contributor.authorGunawardhana, Madusha L. P.
dc.contributor.authorLoveday, Jonathan
dc.contributor.authorTaylor, Edward N.
dc.contributor.authorWang, Lingyu
dc.date.accessioned2024-01-10T12:39:10Z
dc.date.available2024-01-10T12:39:10Z
dc.date.issued2017
dc.description.abstractThere exist conflicting observations on whether or not the environment of broad-and narrowline active galatic nuclei (AGN) differ and this consequently questions the validity of the AGN unification model. The high spectroscopic completeness of the Galaxy and Mass Assembly (GAMA) survey makes it ideal for a comprehensive analysis of the close environment of galaxies. To exploit this, and conduct a comparative analysis of the environment of broad-and narrow-line AGN within GAMA, we use a double-Gaussian emission line fitting method to model the more complex line profiles associated with broad-line AGN. We select 209 type 1 (i.e. unobscured), 464 type 1.5-1.9 (partially obscured), and 281 type 2 (obscured) AGN within the GAMA II data base. Comparing the fractions of these with neighbouring galaxies out to a pair separation of 350 kpc h(-1) and triangle z < 0.012 shows no difference between AGN of different type, except at separations less than 20 kpc h(-1) where our observations suggest an excess of type 2 AGN in close pairs. We analyse the properties of the galaxies neighbouring our AGN and find no significant differences in colour or the star formation activity of these galaxies. Further to this, we find that Sigma(5) is also consistent between broad-and narrow-line AGN. We conclude that the observations presented here are consistent with AGN unification.
dc.description.funderUniversity of Hull through an internally funded PhDstudentship
dc.description.funderAustralian Research Council
dc.description.funderSDSS-III
dc.description.funderScience and Technology Facilities Council
dc.fechaingreso.objetodigital2024-04-29
dc.format.extent16 páginas
dc.fuente.origenWOS
dc.identifier.doi10.1093/mnras/stw2925
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/stw2925
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/77155
dc.identifier.wosidWOS:000395165900013
dc.information.autorucFísica;Gunawardhana, MLP;S/I;1038201
dc.issue.numero3
dc.language.isoen
dc.nota.accesocontenido parcial
dc.pagina.final2686
dc.pagina.inicio2671
dc.publisherOXFORD UNIV PRESS
dc.revistaMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
dc.rightsacceso restringido
dc.subjectmethods: observational
dc.subjectgalaxies: active
dc.subjectgalaxies: evolution
dc.subjectgalaxies: interactions.
dc.subjectDIGITAL SKY SURVEY
dc.subjectSTAR-FORMATION
dc.subjectSEYFERT-GALAXIES
dc.subjectREDSHIFT SURVEY
dc.subject2DF-SDSS LRG
dc.subjectDATA RELEASE
dc.subjectAGN ACTIVITY
dc.subjectENVIRONMENT
dc.subjectSTELLAR
dc.subjectEMISSION
dc.titleGalaxy and Mass Assembly (GAMA): active galactic nuclei in pairs of galaxies
dc.typeartículo
dc.volumen465
sipa.codpersvinculados1038201
sipa.indexWOS
sipa.indexScopus
sipa.trazabilidadCarga SIPA;09-01-2024
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