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tokens: becomes minimum at S, with the Lorentz factor reaching maximum, suggesting a highly Doppler boosting jet. Together with the fact that an active γ -ray flaring event in 1H 0323+342 coincided with the passage of a highly superluminal component through S (Doi et al. 2018 ), the recollimation shock S at the end of ACZ might be a potential site of γ -ray production as well as the jet base. The deprojected distance of this feature is ∼40–100 pc. The γ -ray production at such distances is much higher than those usually suggested in typical γ -ray blazars, while this situation is quite similar to HST-1 in the jet of M87. 6. We found that the core shift of the 1H 0323+342 jet is small between 1.4 and 43 GHz. This is consistent with the jet having a small viewing angle to our line of sight. We estimated a relative separation between the 43 GHz core and the central BH using the measured parabolic collimation profile of the inner jet, and obtained a deprojected separation of ∼(0.24–0.71)pc (or possibly shorter) for a viewing angle of 4°–12°. 7. We found various remarkable similarities in the parsec-scale jet structures between 1H 0323+342 and M87 (e.g., the collimation profile and recollimation shock). If M BH of 1H 0323+342 is ∼4 × 10 8 M ⊙ and thus follows the M BH – σ relation, we suggest that a common jet formation mechanism is at work in M87 and 1H 0323+342, where the external gas bound by the SMBH potential plays a role in collimating the jets. 8. If M BH of 1H 0323+342 is a few times (and thus close to or above the Eddington limit), which is proposed by several previous papers, the parabolic jet continues up to 10 7–8 R s from the black hole, suggesting additional large-scale structures that confine the jet. NLR outflows, which may be driven by super-Eddington accretion flows, could be responsible for the large-scale jet confinement. Appendix Calibrator 0329+3510 0329+3510 is a radio source separated by 136 on the sky from 1H 0323+342. This source is a candidate to be a high-frequency peaker, which is a subclass of young radio galaxies (Dallacasa et al. 2000 ). In Figure 9 we show self-calibrated images of 0329+3510 obtained at 15, 24, and 43 GHz. The source morphology significantly changes with frequency. At 43 GHz, where the highest angular resolution is available, the source is resolved into the core (the southernmost brightest region) and a strong knot. The core and the knot are also securely resolved at 24 GHz. However, the two features are mixed in a synthesized beam at 15 GHz and the lower frequencies. This is because the knot becomes brighter as frequency decreases (i.e., an optically thin steep spectrum), while the core spectrum is relatively flat or slightly inverted (i.e., optically thick), as well as the resolution effect. This prevents us from specifying a reliable reference position in the 0329+3510 images at ≤15 GHz. Figure 9. Self-calibrated VLBA images of 0329+3510. From left to right, the images are at 43, 24, and 15 GHz,