Stretch to stretch, dust to dust: Lower-value local H0 measurements from the two-population modelling of type Ia supernovae

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Table 2.

Best-fit Hubble constant and extinction-related parameters of the young supernova population.

model	H₀	$\hat{R_{B}}$ $\widehat{R_{\mathrm{B}}}$		σ_{R_B}		σ_{M_B}		τ		⟨E(B − V)⟩
										\|c\|< 0.15
		HF-pop y	cal	HF-pop y	cal	HF-pop y	cal	HF-pop y	cal	cal
model A	$71 . 45_{- 1.03}^{+ 1.03}$ $71.45^{+1.03}_{-1.03}$	$4 . 28_{- 0.61}^{+ 0.68}$ $4.28^{+0.68}_{-0.61}$		$0 . 93_{- 0.30}^{+ 0.33}$ $0.93^{+ 0.33 }_{- 0.30 }$		$0 . 051_{- 0.018}^{+ 0.018}$ $0.051^{+ 0.018 }_{- 0.018 }$		$0 . 050_{- 0.012}^{+ 0.011}$ $0.050 ^{+ 0.011 }_{- 0.012 }$		$0 . 0466_{- 0.010}^{+ 0.009}$ $0.0466^{+0.009}_{-0.010}$
model B	$70 . 59_{- 1.16}^{+ 1.15}$ $70.59^{+1.15}_{-1.16}$	$4 . 22_{- 0.51}^{+ 0.53}$ $4.22^{+0.53}_{-0.51}$	≡4.3	$0 . 91_{- 0.28}^{+ 0.31}$ $0.91^{+0.31}_{-0.28}$	≡0.4	$0 . 060_{- 0.015}^{+ 0.015}$ $0.060^{+0.015}_{-0.015}$	< 0.038	$0 . 051_{- 0.010}^{+ 0.010}$ $0.051^{+0.010}_{-0.010}$	$0 . 101_{- 0.037}^{+ 0.040}$ $0.101^{+0.040}_{-0.037}$	$0 . 071_{- 0.015}^{+ 0.015}$ $0.071^{+0.015}_{-0.015}$
omitting 4 SNe with x₁ < −0.8 in the calibration sample
model A	$71 . 20_{- 1.05}^{+ 1.05}$ $71.20^{+1.05}_{-1.05}$	$4 . 37_{- 0.62}^{+ 0.69}$ $4.37^{+0.69}_{-0.62}$		$0 . 94_{- 0.31}^{+ 0.34}$ $0.94^{+ 0.34 }_{- 0.31 }$		$0 . 050_{- 0.019}^{+ 0.018}$ $0.050^{+ 0.018 }_{- 0.019 }$	$0 . 049_{- 0.011}^{+ 0.011}$ $0.049 ^{+ 0.011 }_{- 0.011 }$		$0 . 0456_{- 0.009}^{+ 0.009}$ $0.0456^{+0.009}_{-0.009}$
model B	$70 . 19_{- 1.15}^{+ 1.15}$ $70.19^{+1.15}_{-1.15}$	$4 . 22_{- 0.52}^{+ 0.55}$ $4.22^{+0.55}_{-0.52}$	≡4.3	$0 . 91_{- 0.29}^{+ 0.32}$ $0.91^{+0.32}_{-0.29}$	≡0.4	$0 . 060_{- 0.015}^{+ 0.015}$ $0.060^{+0.015}_{-0.015}$	< 0.036	$0 . 051_{- 0.010}^{+ 0.010}$ $0.051^{+0.010}_{-0.010}$	$0 . 120_{- 0.041}^{+ 0.045}$ $0.120^{+0.045}_{-0.041}$	$0 . 077_{- 0.013}^{+ 0.013}$ $0.077^{+0.013}_{-0.013}$

Notes. The extinction properties are either assumed to be the same along the cosmic distance ladder (model A) or allowed to differ (model B) between the Hubble flow and the calibration sample. The results are summarised as the posterior mean values and errors given by credible intervals (or upper limit in the case of σ_{M_B} in the calibration sample) containing 68 per cent of the marginalised probabilities. Two parameters in model B are fixed, and their values are provided with the sign ‘≡’. The last column shows the mean reddening in the calibration sample conditioned on the selected range of colours |c|< 0.15.

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