**Table 1:** Well-observed SNe Ia in the Hubble flow.
SN	Filters	Ref.	$E(B-V)_{{\rm gal}}^{a}$	$E(B-V)_{{\rm host}}$	$v_{{\rm CMB}}$ ^b	$F_{{\rm max}}^{{\rm bol}}$
					(km s^-1)	(erg s^-1 cm^-2)
SN1992bc	BVRI	1	0.022	0.000	5870	(1.565 $\pm$ 0.124) $\times$ 10^-11
SN1992bo	BVRI	1	0.027	0.000	5151	(9.106 $\pm$ 0.967) $\times$ 10^-12
SN1993H	BVRI	1	0.060	0.050	7112	(4.640 $\pm$ 0.613) $\times$ 10^-12
SN1995E	BVRI	2	0.027	0.740	3478	(5.726 $\pm$ 0.622) $\times$ 10^-11
SN1995ac	BVRI	2	0.042	0.080	14 651	(3.425 $\pm$ 0.477) $\times$ 10^-12
SN1995bd	BVRI	2	0.495	0.150	4266	(2.542 $\pm$ 0.521) $\times$ 10^-11
SN1996bo	BVRI	2	0.078	0.280	4857	(2.382 $\pm$ 0.237) $\times$ 10^-11
SN1999aa	UBVRI	3, 4, 5	0.040	0.000	4546	(2.333 $\pm$ 0.446) $\times$ 10^-11
SN1999aw	BVRI	5, 6	0.032	0.000	11 754	(3.525 $\pm$ 0.700) $\times$ 10^-12
SN1999dq	UBVRI	3	0.024	0.139	4029	(3.871 $\pm$ 0.730) $\times$ 10^-11
SN1999ee	UBVRI	7	0.020	0.280	3169	(5.781 $\pm$ 0.881) $\times$ 10^-11
SN1999gp	UBVRI	3, 8	0.056	0.070	7783	(9.270 $\pm$ 1.082) $\times$ 10^-12

^a Taken from Schlegel et al. (1998) dust maps.
^b Heliocentric velocities from NED transformed to the cosmic microwave background frame. To account for peculiar velocities we assume throughout this work an error of 400 km s^-1 for all CMB distances.
References: (1) - Hamuy et al. (1996c); (2) - Riess et al. (1999a); (3) - Jha (2002); (4) - Krisciunas et al. (2000); (5) - Regnault (2000); (6) - Strolger et al. (2002); (7) - Stritzinger et al. (2002); (8) - Krisciunas et al. (2001).

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