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Table 2
Pearson correlation coefficients between polarization, extinction, and element abundances in the dust phase.
| Parameters and figure | N stars | rcorr. | Comment |
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| log P vs. [Fe(rest)/H]d/ [Fe/H] cosmic, Fig. 2 | 91 | –0.638 | Polarizing grains are not iron-rich non-silicates |
| log P/E(B − V) vs. [Fe(rest)/H]d/ [Fe/H] cosmic, Fig. 3 | 91 | –0.104 | No correlation |
| log P/AV vs. [Fe(rest)/H]d/ [Fe/H] cosmic | 69 | 0.137 | ′′ |
| log P vs. [Fe/H]d/ [Fe/H] cosmic, Fig. 4 | 121 | 0.351 | Weak correlation |
| log P/E(B − V) vs. [Fe/H]d/ [Fe/H] cosmic | 121 | 0.013 | No correlation |
| log P/AV vs. [Fe/H]d/ [Fe/H] cosmic | 98 | –0.117 | ′′ |
| log P vs. [Mg/H]d/ [Mg/H] cosmic, Fig. 5 | 130 | 0.296 | Weak correlation |
| log P/E(B − V) vs. [Mg/H]d/ [Mg/H] cosmic | 130 | –0.050 | No correlation |
| log P/AV vs. [Mg/H]d/ [Mg/H] cosmic | 94 | –0.174 | ′′ |
| log P vs. [Si/H]d/ [Si/H] cosmic, Fig. 6 | 34 | 0.736 | Polarizing grains are silicates |
| log P/E(B − V) vs. [Si/H]d/ [Si/H] cosmic | 34 | 0.116 | No correlation |
| log P/AV vs. [Si/H]d/ [Si/H] cosmic | 16 | 0.013 | ′′ |
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