INTEGRALPlanckGaiaHitomiPOLARCHEOPSEuclidATHENA
HEAVENSFACTCTALOFTSPICAJEM-EUSOXIPEeXTPTheseus
ISDCCAPCDCI
Data Centre for Astrophysics
Astronomy Department of the University of Geneva

The environment of Weak Emission-Line Quasars

ABSTRACT

The nature of weak emission-line quasars (WLQs) is probed by comparing the Baldwin effect (BEff) in WLQs and normal quasars (QSOs). We selected 81 high-redshift (z>2.2) and 2 intermediate-redshift (z=1.66 and 1.89) WLQs. Their rest-frame equivalent widths (EWs) of the C IV emission-line and their Eddington ratio were obtained from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7) Quasar Catalogue or from Diamond-Stanic et al. (2009). We compare the parameters of WLQs with these of 81 normal quasars from Bright Quasar Survey (BQS) and 155 radio-quiet and radio-intermediate quasars detected by SDSS and Chandra. The influence of the Eddington ratio, LBol/LEdd, and the X-ray to optical luminosity ratio, αox, on the BEff is analysed. We find that WLQs follow a different relationship on the EW(CIV)–LBol/LEdd plane than normal quasars. This relationship disagrees with the super-Eddington hypothesis. The weakness/absence of emission-lines in WLQs does not seem to be caused by their extremely soft ionizing continuum but by low covering factor (Ω/4π) of their broad line region (BLR). Comparing emission-line intensities indicates that the ratios of high-ionization line and low-ionization line regions (i.e. ΩHILLIL) are lower in WLQs than in normal QSOs. The covering factor of the regions producing C IV and Ly α emission-lines are similar in both WLQs and QSOs.