Table 4:

Kolmogorov-Smirnov tests of the consistency of different CCSN distributions with two exponential disk models.

Sample
(1)	(2)	(3)	(4)	(5)
Full sample	0.002	0.010	0.895	0.010
Sa-Sbc	0.040	0.028	0.749	0.012
Sc-Sd	0.044	0.602	0.328	0.166
Sa-Sbc (SNe Ib/c)	0.000	0.016	0.003	0.091
Sc-Sd   (SNe Ib/c)	0.111	0.944	0.335	0.973
Sa-Sbc (SNe II)	0.434	0.021	0.229	0.001
Sc-Sd   (SNe II)	0.219	0.252	0.693	0.106
Sa-Sd   (without bars)	0.006	0.194	0.302	0.208
Sa-Sd   (with bars)	0.157	0.036	0.814	0.013
Sa-Sbc (without bars)	0.037	0.162	0.703	0.387
Sa-Sbc (with bars)	0.298	0.296	0.390	0.006
Sc-Sd   (without bars)	0.036	0.965	0.428	0.566
Sc-Sd   (with bars)	0.873	0.265	0.686	0.259
	0.003	0.733	0.039	0.947
	0.359	0.007	0.055	0.000
	0.064	0.396	0.940	0.055
	0.023	0.049	0.676	0.125
	0.032	0.889	0.059	0.532
	0.029	0.005	0.797	0.003
SNe Ib	0.019	0.302	0.160	0.840
SNe Ic	0.002	0.109	0.042	0.523
SNe Ib/c	0.000	0.105	0.014	0.621
SNe II	0.102	0.006	0.496	0.001

Notes: Column 1: sample; Col. 2: KS test probabilities that CCSN subsamples have isophotal radius - normalized distributions consistent with the Freeman disk; Col. 3: same as Col. 2, but with scale-length normalization; Col. 4: same as Col. 2, but for the host stellar disk; Col. 5: same as Col. 4, but with scale-length normalization. CCSN distributions inconsistent with these exponential models are highlighted in bold.