出版社：SISSA, Scuola Internazionale Superiore di Studi Avanzati
摘要：SDSS J094533.99+100950.1 is an example of a weak line quasar (WLQ). Two hypotheses explaining the WLQ phenomena are present in the literature: high accretion rate (which is the case of PHL 1811) or not fully developed broad emission line region (BLR) (which could be due to the evolutionary state — reactivation phase). What PHL 1811 and WLQ have in common are very low equivalent widths of the high-ionization emission lines like CIV or HeII, typical iron emission, radio quiescence and X-ray weakness. The explanation of the atypical quasar properties could be a super-Eddington accretion rate. In addition, the ionizing radiation source can be obscured by a wind or other medium on its way to the BLR. Another possibility is that due to the evolution of the active phase in AGN the emitting matter can have unusual properties. The BLR could not be fully developed in the state before the wind is launched, thus occupying a compact region. To resolve the puzzle, spectral analysis, photoionization simulations, accretion disk continuum fitting and black hole spin estimation have been done.
