Table 2: Results from ${\cal SN}$-fit.
SN Telescope Best fit SN % (host)$^\dagger$ $z_{\rm f}$ $z_{\rm h}$ Spectroscopic Reduced d.o.f.$^\ast$
name   template (reference)       phase$^\ddagger$ $\chi ^2$  
1999cj WHT 92A (Kirshner et al.1993) 31(Bulge) 0.355 0.362 +9 1.00 859
1999ck WHT 94D (Patat et al.1996) 48(Sa) 0.434 0.432 -9 1.17 502
1999dr1 WHT 94D (Patat et al.1996) 48(own galaxy) 0.174 0.178 +24 0.95 935
1999dt WHT 94D (Patat et al.1996) 80(Sb) 0.438 0.437 -9 1.24 623
1999du2 WHT 99ee (Hamuy et al.2002) 65(Stb4) 0.258 0.260 -9 0.87 853
1999dv WHT 03du (Anupama et al.2005) 11(Stb1) 0.177 0.186 -7 0.99 936
1999dw WHT 99ee (Hamuy et al.2002) 63(Sa) 0.464 0.460 -4 0.75 705
1999dx WHT 92A (Kirshner et al.1993) 77(S0) 0.270 0.269 +5 1.66 935
1999dy WHT 96X (Salvo et al.2001) 23(Sb) 0.202 0.215 0 1.14 934
1999dz WHT 99ee (Hamuy et al.2002) 79(Sb) 0.480 0.486 -4 1.17 671
1999ea WHT 94D (Patat et al.1996) 42(Sa) 0.398 0.397 -8 1.12 697
1999gx WHT 94D (Patat et al.1996) 64(Sa) 0.487 0.493 -4 0.93 871
1999du1 NOT 92A (Kirshner et al.1993) 28(own galaxy) 0.250 0.260 +6 0.81 572
1999dv NOT 92A (Kirshner et al.1993) 6(Sc) 0.181 0.186 +9 1.15 637
Notes:
$^\dagger$ %(host) = $\beta/(\alpha + \beta)\times 100$ (see text).
$^\ddagger$ Typical error is $\pm 3$ days.
$^\ast$ Number of degrees of freedom.
1 The observed galaxy has been used for the fit.
2 Best solution when emission lines are ignored: 99ee -9 days, 39% (Sb), $z_{\rm f}=0.261$, reduced $\chi^2=0.78$, d.o.f. = 936.

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