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

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Table B.1.

Parameters of the models.

Component	M_⋆				SFR				Offset
y	b	m	Pearson	p	b	m	Pearson	p	b	m	Pearson	p
	(pc cm⁻³)		coeff.	value	(pc cm⁻³)		coeff.	value	(pc cm⁻³)		coeff.	value
(1)	(2)				(3)				(4)
DM $_{host}^{direct}$ $_{\mathrm{host}}^{\mathrm{direct}}$	86±8	43±13	0.73	7×10⁻²	84±5	36±7	0.85	4×10⁻³	86±21	-2±4	0.22	0.71
DM $_{host}^{halo}$ $_{\mathrm{host}}^{\mathrm{halo}}$	30±1	12±2	0.89	1×10⁻³	30±1	9±1	0.91	1×10⁻³	26±5	0±1	0.13	0.69
DM $_{host}^{ISM}$ $_{\mathrm{host}}^{\mathrm{ISM}}$	55±8	31±12	0.64	3×10⁻²	55±6	27±7	0.78	3×10⁻³	60±14	-2±3	-0.18	0.57

Notes. Parameters of linear fits of the form y = mx + b for correlations shown in Fig. 6 (see also Sect. 4.2) and their corresponding Pearson coefficients and p-values. (1) Component fitted; (2) Parameters for stellar mass fits, with x = log(M_⋆/10¹⁰M_⊙); (3) Parameters for SFR fits, with x = log(SFR/M_⊙yr⁻¹); (4) Parameters for projected distance fits, with x being the impact parameter between the FRB and the galaxy center in kpc.

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