000094451 001__ 94451
000094451 005__ 20201122125253.0
000094451 0248_ $$2sideral$$a118461
000094451 0247_ $$2doi$$a10.1051/0004-6361/201935265
000094451 037__ $$aART-2019-118461
000094451 041__ $$aeng
000094451 100__ $$aMarziani, P.
000094451 245__ $$aBlack hole mass estimates in quasars. A comparative analysis of high- and low-ionization lines
000094451 260__ $$c2019
000094451 5060_ $$aAccess copy available to the general public$$fUnrestricted
000094451 5203_ $$aContext: The interline comparison between high- and low-ionization emission lines has yielded a wealth of information on the structure and dynamics of the quasar broad line region (BLR), including perhaps the earliest unambiguous evidence in favor of a disk + wind structure in radio-quiet quasars.
Aims: We carried out an analysis of the C IVλ1549 and Hβ line profiles of 28 Hamburg-ESO high-luminosity quasars and of 48 low-z, low-luminosity sources in order to test whether the width of the high-ionization line C IVλ1549 could be correlated with Hβ and be used as a virial broadening estimator.
Methods: We analyze intermediate- to high-S/N, moderate-resolution optical and near-infrared (NIR) spectra covering the redshifted C IVλ1549 and Hβ over a broad range of luminosity log L ∼ 44 − 48.5 [erg s−1] and redshift (0 − 3), following an approach based on the quasar main sequence.
Results: The present analysis indicates that the line width of C IVλ1549 is not immediately offering a virial broadening estimator equivalent to Hβ. At the same time a virialized part of the BLR appears to be preserved even at the highest luminosities. We suggest a correction to FWHM(C IVλ1549) for Eddington ratio (using the C IVλ1549 blueshift as a proxy) and luminosity effects that can be applied over more than four dex in luminosity.
Conclusions: Great care should be used in estimating high-L black hole masses MBH from C IVλ1549 line width. However, once a corrected FWHM C IVλ1549 is used, a C IVλ1549-based scaling law can yield unbiased MBH values with respect to the ones based on Hβ with sample standard deviation ≈0.3 dex.
000094451 536__ $$9info:eu-repo/grantAgreement/ES/DGA-FEDER/E24-17R$$9info:eu-repo/grantAgreement/ES/MINECO/AYA2016-76682-C3-1-P$$9info:eu-repo/grantAgreement/ES/MINECO-FEDER/MTM2015-64095-P$$9info:eu-repo/grantAgreement/ES/MINECO/SEV-2017-0709
000094451 540__ $$9info:eu-repo/semantics/openAccess$$aAll rights reserved$$uhttp://www.europeana.eu/rights/rr-f/
000094451 590__ $$a5.636$$b2019
000094451 591__ $$aASTRONOMY & ASTROPHYSICS$$b11 / 68 = 0.162$$c2019$$dQ1$$eT1
000094451 592__ $$a2.174$$b2019
000094451 593__ $$aSpace and Planetary Science$$c2019$$dQ1
000094451 593__ $$aAstronomy and Astrophysics$$c2019$$dQ1
000094451 655_4 $$ainfo:eu-repo/semantics/article$$vinfo:eu-repo/semantics/publishedVersion
000094451 700__ $$aOlmo, A. del
000094451 700__ $$0(orcid)0000-0002-7374-3222$$aMartínez-Carballo, M.A.$$uUniversidad de Zaragoza
000094451 700__ $$aMartínez-Aldama, M.L.
000094451 700__ $$aStirpe, G.M.
000094451 700__ $$aNegrete, C.A.
000094451 700__ $$aDultzin, D.
000094451 700__ $$aD’Onofrio, M.
000094451 700__ $$aBon, E.
000094451 700__ $$aBon, N.
000094451 7102_ $$12005$$2595$$aUniversidad de Zaragoza$$bDpto. Matemática Aplicada$$cÁrea Matemática Aplicada
000094451 773__ $$g627 (2019), A88 [20 pp]$$pAstron. astrophys.$$tAstronomy & astrophysics$$x0004-6361
000094451 8564_ $$s1970380$$uhttps://zaguan.unizar.es/record/94451/files/texto_completo.pdf$$yVersión publicada
000094451 8564_ $$s571438$$uhttps://zaguan.unizar.es/record/94451/files/texto_completo.jpg?subformat=icon$$xicon$$yVersión publicada
000094451 909CO $$ooai:zaguan.unizar.es:94451$$particulos$$pdriver
000094451 951__ $$a2020-11-22-12:44:38
000094451 980__ $$aARTICLE