tokens: SEDs from Abdo et al. ( 2010a ), a time-scale of one day due to the lack of variability data and γ min = 200 (Zhang et al. 2012 ). 4 RESULTS We used three types of EEDs to fit the SEDs of TeV BL Lacs. The SEDs for the maximum probability and the 1σ error band are shown in Fig. 1 . The one-dimensional (1D) probability distributions and the two-dimensional (2D) confidence contours of the model parameters are shown in Figs 2 – 5 . In the 1D distributions, the dotted lines show the maximum likelihood distributions and the solid lines show the marginalized distributions. In the 2D distributions, the inner contour denotes the 68 per cent CL, while the outer contour represents the 95 per cent CL. The model parameters are listed in Tables 1 – 3 . Figure 1. Left-hand panels: SEDs of the three objects fitted by three types of EEDs, where the solid black, blue dash-dot and magenta dash-dot-dot lines represent the SEDs given by the BPL, PLLP and PLC EEDs, respectively. Right-hand panels: SED contours of the three objects in γ-ray bands with the 1σ error bands, where the shaded areas in grey, blue and orange represent the SED contours given by the BPL, PLLP and PLC EEDs, respectively. Figure 2. 3C66A. Left-hand panels: Distributions of the parameters given by the three types of EEDs, where the dotted lines show the maximum likelihood distributions and the solid lines show the marginalized probability distributions. Right-hand panels: 2D confidence contours of the parameter correlations for the three types of EEDs, where the contours of the parameters with larger correlations are shown. The inner contours denote the 68 per cent CL, while the outer contours represent the 95 per cent CL. Figure 3. As Fig. 2 , but for PKS1424+240. Figure 4. As Fig. 2 , but for PKS1424+240 in the flare state. Figure 5. As Fig. 2 , but for PG1553+113. Table 1. Model parameters of the best fits and the marginalized 68 per cent confidence intervals (CI) for BPL EEDs. Table 2. The model parameters of the best fits and the marginalized 68 per cent confidence intervals (CI) for PLLP EEDs. Table 3. The model parameters of the best fits and the marginalized 68 per cent confidence intervals (CI) are listed for PLC EEDs. 4.1 3C66A The SED fitted by the PLC EED does not cover the Fermi /LAT bands, and χ 2 /dof is worse than that of the other two EEDs. It is found that the SED fitted by the PLC EED within the 68 per cent CL does not cover the Fermi band well compared with the other two EEDs. Hence, the PLC EED was ruled out in modelling the SEDs. We obtain that χ 2 /dof values are 1.22 and 1.20 for BPL and PLLP EEDs, and the parameters are well constrained except for α in both models. However, the flux in the 20–50 keV bands given by the PLLP EED is higher than that for the BPL EEDs, indicating that hard X-ray observations could distinguish between the two types of EED. In summary, the red shift of 3C66A is 0.16 and 0.24 from the BPL and PLLC models, respectively, and the red shift of the
ner_tags: O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula B-Citation I-Citation I-Citation I-Citation 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 O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O 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-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O 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-CelestialObject O O O O O O O O B-CelestialObject O O O O O O O O O O O O B-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O 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-CelestialObject O O O O O O O O O O O B-Observatory B-Telescope O O O O O O O O O O O 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-Observatory O O O O O O O O O O O O O O O O O O O O O O O O O O O O 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 B-Wavelength O O O O O O O O O O O O O O O B-CelestialObject O O O O O O O O O O O O O O O O O