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Table 4

Coefficients of the polynomial fit.

Magnitude a 0 a 1 a 2 a 3 a 4

Excluding known and possible binaries
M J 11.140  ±  0.052 0.556  ±  0.032 3.74  ±  0.62  ×  10-2 –9.49  ±  0.45  ×  10-3 3.69  ±  0.11  ×  10-4
M H 10.486  ±  0.051 0.590  ±  0.031 –3.80  ±  0.61  ×  10-3 –4.35  ±  0.44  ×  10-3 2.15  ±  0.11  ×  10-4
M K 10.180  ±  0.056 0.375  ±  0.035 2.31  ±  0.67  ×  10-2 –5.03  ±  0.49  ×  10-3 2.11  ±  0.12  ×  10-4

Excluding known binaries
M J 10.957  ±  0.053 0.736  ±  0.032 –5.53  ±  0.61  ×  10-3 –6.31  ±  0.44  ×  10-3 2.96  ±  0.11  ×  10-4
M H 10.292  ±  0.052 0.778  ±  0.031 –4.77  ±  0.60  ×  10-2 –1.13  ±  0.43  ×  10-3 1.41  ±  0.10  ×  10-4
M K 10.005  ±  0.056 0.548  ±  0.034 –1.84  ±  0.64  ×  10-2 –1.93  ±  0.46  ×  10-3 1.38  ±  0.11  ×  10-4

Notes. The fits are defined as in Liu et al. (2006): ai  ×  (SpT)i where XX indicates J, H or K-band magnitude and the spectral types are defined following the convention SpT = 1 for L1, SpT = 9 for L9, SpT = 10 for T0 etc. The fit is valid for spectral types from L0 to T9. Infrared spectral types are used for both L and T dwarfs.

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