Table 4
Slopes and intercepts of the linear least-square fits.
| Correlated parameters | Intercept | Slope |
|
r | |
| (mÅ) | (mÅ/E(B−V)) | ||||
|
|
|||||
| W(5780) – EB−V | 2.7 ± 3.3 | 462.0 ± 12.7 | 10.8 | 0.79 | |
| W(5797) – EB−V | −5.0 ± 1.1 | 159.0 ± 4.1 | 4.0 | 0.92 | |
| W(6196) – EB−V | 3.8 ± 0.4 | 35.2 ± 1.8 | 6.0 | 0.72 | |
| W(6379) – EB−V | −1.5 ± 0.8 | 88.5 ± 0.8 | 5.6 | 0.85 | |
| W(6613) – EB−V | −2.2 ± 1.2 | 177.8 ± 4.6 | 6.4 | 0.86 | |
|
|
|||||
| W(5780)σ – EB−V | 3.0 ± 7.8 | 640.2 ± 43.6 | 3.3 | ||
| W(5780)ζ – EB−V | −23.8 ± 5.0 | 419.2 ± 13.7 | 9.3 | ||
| W(5797)σ – EB−V | −1.7 ± 1.8 | 127.0 ± 9.6 | 2.8 | ||
| W(5797)ζ – EB−V | −0.5 ± 1.9 | 153.3 ± 5.3 | 5.1 | ||
Notes. Uncertainties in both coordinates are taken into account. Non-detections and upper limits were excluded from the fit procedure. The fits were not forced to go through the origin, though it can be noted that in most cases the derived intercept is within 2σ of the origin. These relations can be used to derive estimates for the (interstellar) line-of-sight reddening from measurements of the diffuse band strengths.
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