Table 5:

Spectral indices and classifications for  Indi Ba, Bb.

Source	H2O-J	CH4-J	H2O-H	CH4-H	CH4-K	Direct	M1	M2
Spectra smoothed to R =150
Indi Ba	0.650 (T0.0)	0.656 (T0.0)	0.592 (T0.0)	0.873 (T2.0)	0.587 (T2.0)	T1.0	T1.0	...
Indi Bb	0.172 (T6.0)	0.305 (T6.5)	0.308 (T5.5)	0.295 (T6.0)	0.178 (T5.5)	T6.0	T6.0	...
Spectra smoothed to R =500
Indi Ba	0.652 (.../...)	0.657 (T1.0/T1.5)	0.589 (T1.0/T0.5)	0.872 (T2.0/T2.0)	0.588 (T2.0/T2.0)	T1.0	T1.5	T1.5
Indi Bb	0.171 (T6.0/T6.0)	0.302 (T6.0/T6.0)	0.303 (T6.0/T6.0)	0.290 (T6.0/T6.0)	0.180 (T5.5/T5.5)	T6.0	T6.0	T6.0
Unsmoothed spectra
Indi Ba	0.645	0.660	0.589	0.870	0.589	T1.0	...	...
Indi Bb	0.171	0.307	0.299	0.287	0.178	T6.0	...	...

The spectra have been smoothed to two resolutions to emulate the observations of the spectral standard stars defined by Burgasser et al. (2006b). The indices derived from our unsmoothed data have been included to quantify the uncertainty when measuring indices from spectra at different resolutions. M1 refers to method 1 of Burgasser et al. where the measured spectral indices are compared to that of each of the standard stars, and M2 refers to their method 2 where the measured spectral indices are compared to a range of values for each spectral type. Direct classification compares the overall spectral shape to the standard star spectra. The spectral type derived from each index is shown in parentheses after each measurement with only M1 being defined for a resolution of R=500. The average spectral type from each method is shown on the right-hand side. Only direct classification is possible for our unsmoothed spectra. The range of the H₂O-J index is ill-defined for the earliest T dwarfs and is therefore omitted for   Indi Ba.