Table B.1
Comparison between several visible spectra available in the literature for the NEAs studied in this paper.
| Object | Reference | Obs. date | Φ [° ] | λ min | λ max | Max. position | Slope | Tax. | Similarity |
|
|
|||||||||
| (2201) | Lazzarin et al. (1996) | Oct. 1994 | 7 | 0.369 | 0.972 | 0.659 | –0.364 | – | 0.371 |
| Hicks et al. (1998) | Nov. 1995 | 16 | 0.524 | 0.947 | 0.715 | –0.143 | E | 0.124 | |
| Binzel et al. (2004) | Dec. 1995 | 27 | 0.435 | 0.925 | 0.724 | –0.307 | Sq | 0.013 | |
|
|
|||||||||
| (4183) | Binzel et al. (2004) | multiple | 17, 38 | 0.435 | 0.925 | 0.710 | –0.327 | Sq | 0.084 |
| Fevig & Fink (2007) | multiple | 5; 22; 44 | 0.456 | 0.966 | 0.682 | –0.372 | – | 0.918 | |
|
|
|||||||||
| (5143) | Binzel et al. (2004) | Apr. 1997 | 13 | 0.435 | 0.917 | 0.698 | –0.485 | O | 0.135 |
| Xu et al. (1995) | Dec. 1991 | 37 | 0.494 | 0.994 | 0.721 | –0.023 | V | –0.301 | |
| Lazzarin et al. (2004) | – | – | 0.400 | 0.955 | 0.723 | –0.253 | Sk | 0.301 | |
Notes. The asteroid number, the article reference, the observation date, the wavelength interval (λmin and λmax), the maximum position, the slope (computed in the spectral interval 0.55−0.9 μm), the taxonomic classification, and the similarity factor in the common interval with our NIR spectrum are shown.
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