Multiplicity amongst the population of the T Tauri stars is well known [Ghez et al. 1993,Leinert et al. 1993,Richichi et al. 1994,Mathieu 1994,Simon et al. 1995]. The separation between components in many of those systems is such that the NIR lines observed might be influenced by the presence of the companion stars. From the 50 stars in the sample presented in this work, the following 19 are, according to the references above, binary or multiple systems with separation between components smaller than the slit width used for the observations reported here. They are: DD Tau, DF Tau, DQ Tau, FS Tau, FX Tau, GG Tau, GH Tau, HP Tau, LkCa7, RW Aur, T Tau, UY Aur, V773 Tau, VY Tau, XZ Tau and ZZ Tau. Of these 16 binary/multiple stars, 11 have Pa Beta in emission, from which 64% are of Type I, 27% are IPC profiles and the remaining 9% are of Type II R; from the 8 displaying Br Gamma in emission, 63% are of Type I and 37% are IPC profiles. Amongst the T Tauristars that are part of a multiple system Type I line profiles are the most common, followed by the IPC profiles. This is in tune with the results obtained for the whole sample, despite the difference in the exact frequencies. Overall, the line profiles of the T Tauri stars in multiple systems do not show any clear preference for a given type of line profile.