Table D.1.
Parameters of SNe Ia with nebular spectra used in Fig. 13
| Supernova | E(B − V)MW | E(B − V)Host | RV (host) | Δm15(B) | References | Spectra References |
|---|---|---|---|---|---|---|
| SN 1990N | 0.022 | 0.00 | ... | 1.03 | (1) | (2, 3) |
| SN 1994ae | 0.026 | 0.15 | 3.1 | 0.90 | (4) | (2, 5) |
| SN 1998bu | 0.022 | 0.32 | 3.1 | 1.02 | (6) | (2, 7, 8) |
| SN 2002er | 0.138 | 0.22 | 3.1 | 1.33 | (9) | (10) |
| SN 2003du | 0.008 | 0.00 | ... | 1.02 | (11) | (12) |
| SN 2003hv | 0.013 | 0.00 | ... | 1.61 | (13) | (13) |
| SN 2004eo | 0.093 | 0.00 | ... | 1.46 | (14) | (14) |
| SN 2005cf | 0.084 | 0.10 | 3.1 | 1.05 | (15) | (15) |
| SN 2007af | 0.034 | 0.13 | 2.98 | 1.22 | (16, 17) | (2, 5) |
| SN 2007gi | 0.019 | 0.20 | 1.56 | 1.33 | (18) | (18) |
| SN 2009ig | 0.027 | 0.00 | ... | 0.89 | (19) | (20) |
| SN 2011by | 0.012 | 0.053 | 3.1 | 1.14 | (21) | (22) |
| SN 2011fe | 0.008 | 0.014 | 3.1 | 1.11 | (23, 24) | (20, 25, 26, 27) |
| SN 2012cg | 0.018 | 0.18 | 3.1 | 0.86 | (28) | (29) |
| SN 2012ht | 0.025 | 0.00 | ... | 1.30 | (30) | (29) |
| SN 2012fr | 0.018 | 0.00 | ... | 0.82 | (31) | (29, 32, 33) |
| SN 2013aa | 0.146 | 0.00 | ... | 0.95 | (34) | (29, 32, 33, 35) |
| SN 2013cs | 0.079 | 0.00 | ... | 0.81 | (36) | (29, 33) |
| SN 2013dy | 0.132 | 0.206 | 3.1 | 0.89 | (37) | (38, 39) |
| SN 2013gy | 0.049 | 0.11 | 3.1 | 1.23 | (40) | (32, 33) |
| SN 2015F | 0.175 | 0.085 | 3.1 | 1.35 | (41) | (33) |
| SN 2020nlb | 0.026 | 0.05 | 3.1 | 1.28 | (42) | (42) |
Notes. All Milky Way reddening values are from Schlafly & Finkbeiner (2011), and we assume RV = 3.1. A host RV value of 3.1 has been assumed where no RV was derived to accompany the published host reddening value. SN Specific References: (1) Lira et al. 1998; (2) Silverman et al. 2012; (3) Gómez & López 1998; (4) Stritzinger et al. 2006; (5) Blondin et al. 2012; (6) Jha et al. 1999; (7) Matheson et al. 2008; (8) Cappellaro et al. 2001; (9) Pignata et al. 2004, who estimated total reddening of E(B − V)=0.36; (10) Kotak et al. 2005; (11) Anupama et al. 2005; (12) Stanishev et al. 2007; (13) Leloudas et al. 2009; (14) Pastorello et al. 2007; (15) Wang et al. 2009b; (16) Simon et al. 2007; (17) Ganeshalingam et al. 2010; (18) Zhang et al. 2010; (19) Foley et al. 2012; (20) Stahl et al. 2020; (21) Foley et al. 2020, they derived SN 2011by to have E(B − V)Host of 0.039 mag more than SN 2011fe; (22) Silverman et al. 2013; (23) Patat et al. 2013; (24) Munari et al. 2013; (25) Zhang et al. 2016; (26) Mazzali et al. 2015; (27) Tucker et al. 2022; (28) Marion et al. 2016; (29) Maguire et al. 2018; (30) Hsiao et al. 2015; (31) Contreras et al. 2018; (32) Childress et al. 2015; (33) Graham et al. 2017; (34) Burns et al. 2020; (35) Childress et al. 2016; (36) Graham et al. 2017, note the uncertainty in Δm15(B) for SN 2013cs is large, and there is no host galaxy extinction estimate; (37) Pan et al. 2015; (38) Zhai et al. 2016; (39) Pan et al. 2015; (40) Holmbo et al. 2019; (41) Cartier et al. 2017; (42) This work.
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