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dc.contributor.authorBruni, Gabriele
dc.contributor.authorGonzález Serrano, José Ignacio 
dc.contributor.authorPedani, Marco
dc.contributor.authorBenn, Chris R.
dc.contributor.authorMack, Karl Heinz
dc.contributor.authorHolt, Joanna
dc.contributor.authorMontenegro-Montes, Francisco M.
dc.contributor.authorJiménez Luján, Florencia
dc.contributor.otherUniversidad de Cantabriaes_ES
dc.date.accessioned2018-06-15T11:12:51Z
dc.date.available2018-06-15T11:12:51Z
dc.date.issued2014-09
dc.identifier.issn0004-6361
dc.identifier.issn1432-0746
dc.identifier.otherAYA2008-06311-C02-02
dc.identifier.otherAYA2011-29517-C03-02
dc.identifier.urihttp://hdl.handle.net/10902/13911
dc.description.abstractContext. Broad absorption lines (BALs) are present in the spectra of ~20% of quasars (QSOs); this indicates fast outflows (up to 0.2c) that intercept the observer’s line of sight. These QSOs can be distinguished again into radio-loud (RL) BAL QSOs and radio-quiet (RQ) BAL QSOs. The first are very rare, even four times less common than RQ BAL QSOs. The reason for this is still unclear and leaves open questions about the nature of the BAL-producing outflows and their connection with the radio jet. Aims. We explored the spectroscopic characteristics of RL and RQ BAL QSOs with the aim to find a possible explanation for the rarity of RL BAL QSOs. Methods. We identified two samples of genuine BAL QSOs from SDSS optical spectra, one RL and one RQ, in a suitable redshift interval (2.5 < z < 3.5) that allowed us to observe the Mg?ii and Hß emission lines in the adjacent near-infrared (NIR) band. We collected NIR spectra of the two samples using the Telescopio Nazionale Galileo (TNG, Canary Islands). By using relations known in the literature, we estimated the black-hole mass, the broad-line region radius, and the Eddington ratio of our objects and compared the two samples. Results. We found no statistically significant differences from comparing the distributions of the cited physical quantities. This indicates that they have similar geometries, accretion rates, and central black-hole masses, regardless of whether the radio-emitting jet is present or not. Conclusions. These results show that the central engine of BAL QSOs has the same physical properties with and without a radio jet. The reasons for the rarity of RL BAL QSOs must reside in different environmental or evolutionary variables.es_ES
dc.description.sponsorshipAcknowledgements. The authors acknowledge financial support from the Spanish Ministerio de Ciencia e Innovación under projects AYA2008-06311-C02-02 and AYA2011-29517-C03-02. Part of this work was supported by the COST Action MP0905 “Black Holes in a Violent Universe”. Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) oper-ated on the island of La Palma by the Fundación Galileo Galilei of the INAF.es_ES
dc.format.extent10 p.es_ES
dc.language.isoenges_ES
dc.publisherEDP Scienceses_ES
dc.rights© ESO, 2014es_ES
dc.sourceA&A 569, A87 (2014)es_ES
dc.titleInvestigating the radio-loud phase of broad absorption line quasarses_ES
dc.typeinfo:eu-repo/semantics/articlees_ES
dc.relation.publisherVersionhttps://doi.org/10.1051/0004-6361/201424424es_ES
dc.rights.accessRightsopenAccesses_ES
dc.identifier.DOI10.1051/0004-6361/201424424
dc.type.versionpublishedVersiones_ES


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