ner_tags: O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength O O O O O O O O O O O O B-Wavelength O O O O O O O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength B-Wavelength O O O O O O O O O O O O O O O O O O O O O B-Wavelength O O O O O O O O O O O O O O O O O O O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O
tokens: NLRs and in the NLRs, effects of the dusts on the observed values (marked by the suffix of obs) should be where D (BLRsextNLRs) , D (extNLRs) and D NLRs represent effects of dusts in all regions, effects of dusts in the regions from the BLRs to the observer and the effects of dusts in the NLRs, respectively. Effects of dust extinctions can be considered as the role factor to determine the scatters of the correlations shown in Fig. 5 . There are more similar dust extinctions on L (5100 ,obs) and on , but more different dust extinctions on the L (5100 ,obs) and on the . Therefore, there are tighter correlations between L (5100 ,obs) and than the correlation between L (5100 ,obs) and . Moreover, with considerations of dependence of Balmer decrements (which can be used to trace the dust extinctions) on [O iii ]luminosity, the steeper correlation of L (5100 ,obs) and can also be simply explained as follows. Based on the observed and the Balmer decrements from common NLRs BD obs, NLRs for our objects with both narrow H and narrow H, we can find that there is a moderately negative correlation shown in Fig. 7 , with Spearman rank correlation coefficient of about 0.32 with P null 510 8 . And the anticorrelation can be simply described by with narrow 0.045. Then, combining with the empirical equation to estimate colour excess with 3.1 as the intrinsic flux ratio of narrow H to narrow H, the intrinsic luminosity can be estimated by where k and E ( B V ) represent the reddening curve and colour excess, respectively, and narrow 0.8 k narrow . Meanwhile, similar equations to estimate L (5100 ,int)) and can be described by where ext 0.8 k ext and have probably different values of ext and 5100 from the value of narrow , because of different dust obscurations for observed continuum luminosity and for observed luminosity from the extended components of [O iii ]lines. And, the values of must be smaller than 1, otherwise an unreasonable result can be expected that intrinsic luminosity after considerations of dust extinctions could be smaller than the observed luminosity. Then, we have the following sub-equations Based on the third sub-equation in equation ( 10 ) combining with the shown results in the top panel of Fig. 6 , we can find that . Therefore, the correlation of L (5100 ,obs) versus is steeper, because of its larger slope of being about 1.2times larger than the slope of for the correlation of L (5100 ,obs) versus . Certainly, the results above are highly idealized, and seriously depend on physical properties of dusts in central regions of AGN; however, the results can be applied to find qualitative explanations to the results shown in Fig. 5 . Figure 7. Correlation between observed Balmer decrements(flux ratio of narrow H to narrow H) and the luminosities of the core components of the [O iii ]emission lines. Before the end of this section, we show our simple discussions on which component is well applied to trace central AGN intrinsic luminosity in type-2