Do spectra improve distance measurements of Type Ia supernovae?

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Table 3

Validation of top 5 flux ratios at maximum light from Bailey et al. (2009) (noted B09).

λ _X	λ _Y	γ	γ(B09)	WRMS^a	Δ_x₁,c

ℛ

6420	4430	−3.40 ± 0.32	−3.5 ± 0.2	0.184 ± 0.026	−0.007 ± 0.031 (0.2σ)
6420	4170	−4.43 ± 0.41	−4.9 ± 0.2	0.197 ± 0.028	0.008 ± 0.028 (0.3σ)
7720^b	4370	···	7.3 ± 0.3	···	···
6420	5120	−4.34 ± 0.42	−4.7 ± 0.3	0.237 ± 0.032	0.052 ± 0.034 (1.5σ)
7280^b	3980	···	7.9 ± 0.3	···	···

(c,ℛ^c)

6420	5190	−2.20 ± 0.57	−3.5 ± 0.3	0.176 ± 0.025	−0.012 ± 0.016 (0.8σ)
5770	6420	0.67 ± 0.22	1.4 ± 0.1	0.193 ± 0.027	0.005 ± 0.011 (0.5σ)
6420	5360	−1.71 ± 0.43	−2.3 ± 0.2	0.169 ± 0.024	−0.019 ± 0.016 (1.2σ)
6760	6420	1.79 ± 1.09	4.2 ± 0.5	0.217 ± 0.032	0.030 ± 0.025 (1.2σ)
6420	4430	−2.56 ± 0.63	−3.2 ± 0.3	0.168 ± 0.024	−0.027 ± 0.023 (1.2σ)

(x₁,c)


···	···	···	···	0.194 ± 0.027	···

Notes.

^(a)

Weighted rms of Hubble residuals from a simultaneous fit to the entire SN Ia sample (as done by Bailey et al. 2009), as opposed to prediction residuals under cross-validation. As explained in Sect. 2.3, the weighted rms of prediction Hubble residuals is a more realistic estimate of the accuracy of a given model in measuring distances to SN Ia.

^(b)

Wavelength bins redder than 7100 Å, not covered by most of our spectra.

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