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Table 2.

Data for the 141 SNe Ia used in this analysis.

SN name zCMB c x1 Local Mass Local SFR Local sSFR Global Mass 𝒫Y 𝒫HM Refs.
mag log(M*/M) log(M* yr−1 kpc−2) log(yr−1 kpc−2) log(M*/M) % %
SNF20060511-014 −0.07 ± 0.14 0.0467 −0.03 ± 0.03 −0.65 ± 0.17 59 97
SNF20060512-001 −0.06 ± 0.13 0.0389 +0.02 ± 0.03 +0.71 ± 0.13 100 0
SNF20060512-002 −0.45 ± 0.12 0.0509 +0.05 ± 0.03 −0.92 ± 0.19 0 100
SNF20060521-001 −0.03 ± 0.13 0.0679 −0.05 ± 0.03 −1.15 ± 0.23 0 10
SNF20060521-008 −0.27 ± 0.14 0.0562 +0.09 ± 0.03 −1.36 ± 0.20 37 100
SNF20060526-003 +0.01 ± 0.12 0.0788 −0.03 ± 0.03 +0.30 ± 0.14 90 100

Notes. The complete table is available at the CDS. includes a 0.094 mag residual dispersion. Heliocentric redshifts are taken from Childress et al. (2013b), except for LSQ12ekl, LSQ13vy, PTF10wnm PTF10xyt, PTF10zdk, and PTF11mty, for which heliocentric redshifts were derived from our local Hα measurements. 𝒫Y is the statistical classification for a SN Ia to be young, as given Eq. (3). 𝒫HM is the probability for the global stellar mass of the SN host galaxy to be higher than log(M*/M) = 10. The Refs column provides references for external discoveries, as follows: (1) Drake et al. (2009) (2) Maguire et al. (2012) (3) Barone-Nugent et al. (2012) (4) Maguire et al. (2013) (5) Weyant et al. (2014) (6) Maguire et al. (2014) (7) Boles; Armstrong (8) del Olmo, Martinez,Pedraz, Alises; Trondal, Schwartz (9) Sako et al. (2008) (10) Quimby et al (11) Kelly et al. (2010) (12) LOSS (13) Blondin et al. (2012) (14) Ciabattari, Donati, Mazzoni (15) Arbour (16) Ciabattari et al. (17) Zhang et al. (2015)

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