Probing star formation and ISM properties using galaxy disk inclination - II. Testing typical FUV attenuation corrections out to z ~ 0.7

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Table A.1.

COSMOS z ~ 0.7 UV slope corrections or A_V = 1.

Method	N	k₁	k₂	σ²
No corr	575
A_V =1	575
β (B12)	56
β (W16)	56
A_V = 1 where β	56
β (B12) or A_V = 1	575
No corr	295
A _V =1	295
β (B12)	28
β (W16)	28
A_V = 1 where β	28
β (B12) or A_V = 1	295

Notes. Fits for relations indicated in Fig. A.1. The top half shows the full sample and the bottom half the restricted sample. The “No corr” and and β (B12) methods are repeats of rows 1 and 2 in Table 1 to facilitate comparison.

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