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tokens: NVSS object. We restrict our samples to the SDSS–NVSS quasars with a matching radius of 15 arcsec in order to consider the selection effect by the matching radius. This sub-sample contains 6081 radio-loud objects. The relation between and with the matching radius of 15 arcsec is given aswith a scatter of 0.54. The Spearman rank correlation gives , with a p -value of . Therefore, the correlation between disk luminosity and jet power still statistically exists. The jet production efficiency is given as . 5.4. Effect of the Radio-loudness Cut At , radio-loud quasars are also referred to as radio-intermediate quasars (Falcke et al. 1996 ). Most of them are likely to be FR-I type radio quasars. Figure 9 shows the correlation between and of the SDSS–NVSS detected quasars but having . The dashed line represents . 3083 quasars are included. The regression line, shown by the solid line, is given aswith a scatter of 0.38. The Spearman rank correlation gives , with a p -value of . There is still a positive correlation between disk luminosity and jet power in radio quasars. Based on the jet production efficiency arguments above, here we have . By selecting sources at , a slightly higher jet production efficiency is expected but is still consistent with that at at the 1 σ level. Figure 9. Same as Figure 4 , but at . Figure 10 shows the estimated jet production efficiency as a function of the limiting radio-loudness. As we select high jet power objects by setting high , the jet production efficiency gradually increases with . However, even at , is still at an order of 0.1. Figure 10. Jet production efficiency as a function of the limiting radio-loudness The 1 σ statistical uncertainty of the data is also shown. 5.5. Comparison with Blazar Studies The relation between the disk and jet has been also investigated using blazar spectral fitting studies (e.g., Celotti Ghisellini 2008 ; Ghisellini et al. 2014 ; Inoue Tanaka 2016 ). Differing from our radio quasar studies, blazar studies enable us to compare accretion with jet outflow at the same epoch. Multi-wavelength observations from the radio band to gamma-rays allow us to study overall SED and physical parameters of jets via spectral fitting. A spectrum of a blazar is composed of two emission components: the low-energy component is synchrotron radiation and the other one is an inverse Compton component targeting synchrotron radiation (e.g., Jones et al. 1974 ; Maraschi et al. 1992 ) and/or an external radiation field (e.g., Dermer Schlickeiser 1993 ; Sikora et al. 1994 ). Generally, blazar spectral fitting studies predict large jet production efficiencies (e.g., Celotti Ghisellini 2008 ; Ghisellini et al. 2014 ; Inoue Tanaka 2016 ), while our results show . Such a difference has also been recently reported by Pjanka et al. ( 2016 ) using published blazar samples. Here, the jet power estimates based on blazar spectral fittings strongly rely on the assumptions on the pair fraction and the electron minimum