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

Open Access

Fig. 6.

Rest-frame DM as a function of the stellar mass of the host (left), SFR of the host (middle), and projected offset from the center of the host (right). The black points correspond to DM $_{host}^{direct}$ $_{\mathrm{host}}^{\mathrm{direct}}$ , while the light blue and the dark blue points correspond to DM $_{host}^{ISM}$ $_{\mathrm{host}}^{\mathrm{ISM}}$ and DM $_{host}^{halo}$ $_{\mathrm{host}}^{\mathrm{halo}}$ , respectively. The black line shows a linear fit for DM $_{host}^{direct}$ $_{\mathrm{host}}^{\mathrm{direct}}$ (=DM $_{host}^{halo}$ $_{\mathrm{host}}^{\mathrm{halo}}$ + DM $_{host}^{ISM}$ $_{\mathrm{host}}^{\mathrm{ISM}}$ ), while the light blue and dark blue lines are the linear fits of DM $_{host}^{ISM}$ $_{\mathrm{host}}^{\mathrm{ISM}}$ and DM $_{host}^{halo}$ $_{\mathrm{host}}^{\mathrm{halo}}$ , respectively. The parameters of these fits are presented in Table B.1, and the Pearson coefficients and p-values are given in the figure legends.

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