tokens: constraint is nearly same. So, we find that, different choices of the group prior p 0 ( z , Ω) cannot significantly affect the constraint of the Hubble constant. On the other hand, for LHVIK network with SBBH mergers, we find the error bars of H 0 are quite large in both cases. Figure 8. The posterior distributions of Hubble constant H 0 . The upper, middle, and lower panels show the results of for the LHVIK, LHVIKCA, CE2ETD network, respectively. The left-hand panels represent the cases of uniform window function w i = 1, and the right-hand panels represent the cases of w i proportion to the stellar mass of groups. In each panel, there are four lines. The green line is the result in the case of A and the blue one is that of B (see the main text for the details). Similarly, the red line is the result in the case of A, and the black line is that of B. Note that, green line overlaps with blue one, and red line overlaps with black one. For LHVIKCA network with SBBH mergers, we find that 44 events satisfy the criteria and are used for the parameter constraining. The posterior distributions of H 0 derived from this network are given in the middle left-hand panel of Fig. 8 , which are for both case of A and case of B. While for SBBH mergers, we find 21 events can be used for the parameter constraining, and the corresponding result is in the case of A and H 0 = 69.97 ± 0.86 km s −1 Mpc −1 in the case of B. Same to the cases of LHVIK network, we find that the effect of group prior p 0 ( z , Ω) is not significant. In comparison with the corresponding cases with LHVIK network, we find the uncertainties of H 0 are nearly five times smaller. Due to the contribution of the two 8-km detectors in the network, the localization ability for the individual event is significantly improved, which leads to two effects on the H 0 constraining: First, the uncertainties of the redshift distribution of the GW event is reduced. Secondly, the number of the GW events satisfying the criteria is increased. So, we conclude that, if the proposals of 8-km detectors can be realized in the near future, the capabilities of GW cosmological, based on the SBBHs as the standard sirens, will be greatly improved in the 2G detector era. Now, we turn to the 3G detector network CE2ETD. As anticipated, we find that the accuracies of H 0 are much better than that of the 2G detector networks. For mergers, 66 events can be used for the parameter constraining, which follow the result H 0 = 70.000 ± 0.008 km s −1 Mpc −1 for both cases with different prior choices. For SBBH mergers, the constraint of H 0 is 70.000 ± 0.018 km s −1 Mpc −1 , derived from 65 events, which satisfy the selection criteria. The posterior distributions in these cases are presented in the lower left-hand panel of Fig. 8 . We find that, even comparing with the results of 2G LHVIKCA detector network, the uncertainty of H 0 is reduced by a factor of 30. Nair, Bose Siani ( 2018 ) discussed a single ET’s accuracy of H 0
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