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dc.contributor.authorBenn, Chris R.
dc.contributor.authorCarballo Fidalgo, Ruth 
dc.contributor.authorHolt, Joanna
dc.contributor.authorVigotti, Mario
dc.contributor.authorGonzález Serrano, José Ignacio 
dc.contributor.authorMack, Karl Heinz
dc.contributor.authorPerley, Rick A.
dc.contributor.otherUniversidad de Cantabriaes_ES
dc.date.accessioned2013-04-09T13:16:36Z
dc.date.available2013-04-09T13:16:36Z
dc.date.issued2005-07
dc.identifier.issn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttp://hdl.handle.net/10902/1894
dc.description.abstractWe present observations of the most radio-luminous broad absorption-line (BAL) quasar known, 1624+3758, at redshift z= 3.377. The quasar has several unusual properties. (1) The Fe II UV191 1787-Å emission line is very prominent. (2) The BAL trough (BALnicity index 2990 km s−1) is detached by 21 000 km s−1 and extends to velocity v=−29 000 km s−1. There are additional intrinsic absorbers at −1900 and −2800 km s−1. (3) The radio rotation measure of the quasar, 18 350 rad m−2, is the second highest known. The radio luminosity is P1.4 GHz= 4.3 × 1027 W Hz−1 (H0= 50 km s−1 Mpc−1, q0= 0.5) and the radio loudness is R*= 260. The radio source is compact and the radio spectrum is GHz-peaked, consistent with it being relatively young. The width of the C IV emission line, in conjunction with the total optical luminosity, implies a black hole mass MBH∼ 109 M⊙, L/LEddington≈ 2. The high Eddington ratio and the radio-loudness place this quasar in one corner of Boroson's two-component scheme for the classification of active galactic nuclei, implying a very high accretion rate, and this may account for some of the unusual observed properties. The v=−1900 km s−1 absorber is a possible Lyman-limit system, with N(H I) = 4 × 1018 cm−2, and a covering factor of 0.7. A complex mini-BAL absorber at v=−2200 to −3400 km s−1 is detected in each of C IV, N V and O VI. The blue and red components of the C IV doublet happen to be unblended, allowing both the covering factor and optical depth to be determined as a function of velocity. Variation of the covering factor with velocity dominates the form of the mini-BAL, with the absorption being saturated (e−τ≈ 0) over most of the velocity range. The velocity dependence of the covering factor and the large velocity width imply that the mini-BAL is intrinsic to the quasar. There is some evidence of line-locking between velocity components in the C IV mini-BAL, suggesting that radiation pressure plays a role in accelerating the outflow.es_ES
dc.format.extent16 p.es_ES
dc.language.isoenges_ES
dc.publisherRoyal Astronomical Societyes_ES
dc.rights© 2005 RASes_ES
dc.sourceMonthly Notices of the Royal Astronomical Society, 2005, 360(4), 1455-1470es_ES
dc.subject.otherGalaxies: high-redshiftes_ES
dc.subject.otherIntergalactic mediumes_ES
dc.subject.otherQuasars: absorption lineses_ES
dc.subject.otherQuasars: emission lineses_ES
dc.subject.otherQuasars: generales_ES
dc.subject.otherEarly Universees_ES
dc.titleUnusual high-redshift radio broad absorption-line quasar 1624+3758es_ES
dc.typeinfo:eu-repo/semantics/articlees_ES
dc.relation.publisherVersionhttp://dx.doi.org/10.1111/j.1365-2966.2005.09143.x
dc.rights.accessRightsopenAccesses_ES
dc.identifier.DOI10.1111/j.1365-2966.2005.09143.x
dc.type.versionpublishedVersiones_ES


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