Table 3: Characteristics of possible late-type field dwarf contaminants from the literaturea.

Spectral		 MI I-J $J-K_{\rm s}$ $n_\odot$ dI=25b
type (mag) (mag) (mag) (10-3 pc-3) (pc)
M3-4 V 9.07 1.83 0.84 19.6 7700
M4-5 V 10.14 1.80 0.86 16.3 5700
M5-6 V 11.91 2.47 0.90 9.81 3100
M6-7 V 12.90 2.72 0.93 4.90 2200
M7-8 V 14.16 3.24 0.98 1.907 1300
M8-9 V 14.68 3.54 1.06 1.285 1100
M9-L0 V 15.23 3.80 1.12 0.768 840
L0-1 V 15.27 3.55 1.27 0.637 820
L1-2 V 15.69 3.50 1.38 0.861 680
L2-3 V 16.19 3.62 1.43 1.000 550
L3-4 V 16.67 3.72 1.49 0.834 450
L4-5 V 17.14 3.81 1.54 0.819 360
L5-6 V 17.61 3.90 1.60 0.869 290
L6-7 V 18.07 4.06 1.66 0.785 240
L7-8 V 18.52 4.12 1.71 0.644 190
L8-9 V 18.90 4.22 1.81 0.462 160
L9-T0 V 18.95 4.40 1.73 0.308 160
T0-1 V 19.01 4.63 1.58 0.220 160
T1-2 V 19.04 4.94 1.17 0.241 150
T2-3 V 19.04 5.19 0.81 0.406 150
T3-4 V 19.07 5.23 0.51 0.788 150
T4-5 V 19.22 5.01 0.29 1.42 140
T5-6 V 19.61 4.76 0.11 2.38 120
T6-7 V 20.35 5.25 0.00 3.45 85
T7-8 V 21.60 5.50 -0.06 4.82 48
a The sources of the MI absolute magnitude, I-J, and $J-K_{\rm s}$ colours, and spatial densities are obtained or derived by us from data in the literature (Kirkpatrick et al. 1994; Dahn et al. 2002; Hawley et al. 2002; Cruz et al. 2003; Tinney et al. 2003; Vrba et al. 2004; Bochanski et al. 2007; Burgasser 2007; West et al. 2008). See the text for further details. b dI=25 is the heliocentric distance of a dwarf with an apparent magnitude I = 25.0 mag, assuming an interstellar extinction proportional to the heliocentric distance. At the end of Sect. 2.4 there is a brief discussion on this assumption.

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