Empirical estimation of host galaxy dispersion measure toward well-localized fast radio bursts

Open Access

Fig. C.1.

DM $_{host}^{direct}$ $_{\mathrm{host}}^{\mathrm{direct}}$ vs. stellar mass (in log scale; left), SFR (in log scale; middle), and projected distance (right) of the host galaxies. The black points and the black lines are the same as those in Fig. 6. The shaded area corresponds to our estimated systematic uncertainty (see Sect. 4.5).

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