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tokens: et al. 2011 ; Ramos Almeida et al. 2011 ; Ichikawa et al. 2015 ; Audibert et al. 2017 ), i.e., N c ≃ 3–15, we find that at 86 GHz becomes ≃0.2–1.2, which is of the order of unity and agrees with observational properties of N1. To constrain the number density of the clump, getting the size of the clump ( r c ) should be required. The size of the self-gravitating clump in the context of AGNs has been estimated in the literature (e.g., Krolik Begelman 1988 ; Hönig Beckert 2007 ; Kawaguchi Mori 2011 ). According to the authors of these works, we have r c ≤ 0.05 pc at 1 pc from the central SMBH with M BH = 8 × 10 8 M ⊙ (Scharwächter et al. 2013 ). On the other hand, the size of clumps can be constrained by the observations of transient X-ray absorption events in nearby AGNs, i.e., the typical size is 0.002 pc (e.g., Markowitz et al. 2014 ; Tanimoto et al. 2019 ). By adopting N c and r c , taking into account their uncertainties of 3 ≤ N c ≤ 15 and , the lower limit of number density of each ionized cloud can be given byIn the case of ionized gas clumps, the typical Thomson scattering opacity of each cloud can be estimated as since the optical depth is given by , where σ T is the Thomson cross section. If we adopt the opacity ratio of the dusty gas and the ionized gas is ≃10 3 at the UV band for the AGN radiation (e.g., Umemura et al. 1998 ; Ohsuga Umemura 2001 ; Wada 2012 ), the optical depth of each cloud is , which is consistent with the lower value for nearby Seyfert galaxies (e.g., Table 10 in Ramos Almeida et al. 2011 ). This might indicate that the ionized gas is also clumpy within the 1 pc region of 3C 84. Wada et al. ( 2018 ) examine properties of the ionized gas irradiated by less luminous AGN such as Seyfert galaxies based on their “radiation-driven fountain” model (Wada 2012 ). They found that the ionized region show nonuniform internal structures, corresponding to the clumpy fountain flows caused by the radiation pressure on dusty gas, although the typical density () is smaller than our estimate. In addition, by the optical/NIR observations, the existence of dense clumps with cm −3 has been reported from the detection of coronal lines within NLR (e.g., Murayama Taniguchi 1998 ). These high density clouds in NLRs might contribute the absorption feature of N1. Alternatively, since the density is comparable to number density n c ≃ 10 3–5 cm −3 , based on the momentum balance between the jet thrust and the ram pressure from the clump (Nagai et al. 2017 ; Kino et al. 2018 ), these ionized clumps may contribute not only the absorption of counter jet but also the feedback on jets. Since the dust sublimation radius of 3C 84 is (e.g., Kino et al. 2018 ), the dust components in these dense clumps could be survived. If this is the case, the clumpy clouds might be related to the polar elongation in MIR continuum emission distributions revealed by high-resolution observations in nearby Seyfert galaxies (e.g., Tristram et al. 2014 ; Asmus et