Broad Line QSO

QSO QSO (Quasar, Quasi-Stellar Object, Quasi-Stellar Radio-source)objects having very broad emission lines (FWHM = 5,000-30,000 km/s) with large redshifts, first discovered by Schmidt (1963). The optical spectra are similar to those of Sy1 nuclei, but the narrow lines are generally weaker. The direct images do not differ from those of the stars on DSS1 and even DSS2 or SDSS, however, objects typically brighter than 17m and/or with redshifts smaller than 0.3 show weak “fuzz”, indicating the host galaxy. They have very high luminosities (Mabs > -23). Quasar luminosities are often defined as MB < -21.5 + 5 logh0 (Schmidt & Green, 1983). QSO/S1 separation have been conditionally defined by the luminosity limits (MB = -21.5...-24.0), extension (QSOs as star-like and Seyferts as extended objects), and redshift limit (z=0.1; Hewitt & Burbidge, 1993), however at present the first criterion is accepted, though also conditional. There are radio-loud QSOs (quasars or RL QSOs) and radio-quiet QSOs (or RQ QSOs) with a dividing power at P5GHz ≈ 1024.7 W Hz−1. RL QSOs are 5-10% of the total of QSOs. There is a big gap in radio power between RL and RQ varieties of QSOs. All radio quasars have FR II morphology.	Q1.0 Q1.0 – objects that have quasar luminosities and similar to Seyfert 1.0s show only very strong broad permitted emission Balmer HI lines and narrow forbidden lines. Typically, the narrow lines are weak and due to large distances of many QSOs and lower S/N ratio, they are hardly observed over the noise. When the redshift is high and Balmer lines are not observed, we apply the same criteria for fine classification to MgII and other line profiles.
Q1.2 Q1.2 – objects that have quasar luminosities and similar to Seyfert 1.2s show very strong broad permitted emission Balmer HI lines and narrow forbidden lines, as well as weak narrow permitted Balmer lines. Typically, the narrow forbidden lines are also weak and due to large distances of many QSOs and lower S/N ratio, they are hardly observed over the noise. When the redshift is high and Balmer lines are not observed, we apply the same criteria for fine classification to MgII and other line profiles.	Q1.5 Q1.5 – objects that have quasar luminosities and similar to Seyfert 1.5s show strong broad permitted emission Balmer HI lines and narrow forbidden lines, as well as medium strength narrow permitted Balmer lines. The intensities of broad and narrow permitted Balmer lines is approximately equal. When the redshift is high and Balmer lines are not observed, we apply the same criteria for fine classification to MgII and other line profiles.
Q1.8 Q1.8 – objects that have quasar luminosities and similar to Seyfert 1.8s show broad permitted emission Balmer HI lines and narrow forbidden lines, as well as strong narrow permitted Balmer lines. The permitted lines show strong narrow components and weak broad components only for Hα and Hβ. When the redshift is high and Balmer lines are not observed, we apply the same criteria for fine classification to MgII and other line profiles.	Q1.9 Q1.9 – objects that have quasar luminosity and similar to Seyfert 1.9s show broad permitted emission Balmer Hα line and narrow forbidden lines, as well as strong narrow permitted Balmer lines. The permitted lines show strong narrow components and weak broad components only for Hα. When the redshift is high and Balmer lines are not observed, we apply the same criteria for fine classification to MgII and other line profiles.