A number of photospheric lines are seen in absorption in the observed Pa ${\rm\beta }$ and Br ${\rm\gamma }$ spectra of several T Tauri stars (see Folha & Emerson 1999, hereafter FE99). Some of the narrow photospheric absorption lines fall on top of the Pa ${\rm\beta }$ line, changing its intrinsic profile. Correct analysis of the line profiles require the photospheric component of the observed spectra to be removed. This was achieved, after computing the veiling in the observed wavelength ranges, by following the procedure described in Edwards et al. (1994) to obtain "residual'' profiles (see FE99 for results on near infrared veiling).

$\begin{figure} \includegraphics[angle=-90,width=16cm]{ms10083f1a.eps}\end{figure}$

Figure 1: Pa ${\rm\beta }$ line profiles. Spectra are presented by the type of the line profile and for each type by alphabetical order. Spectra with error bars in each spectral point are from the UT9410 observing run. Stars for which more than one line profile is presented have the lines arranged by observing date

Figures 1 and 2 show the Pa ${\rm\beta }$ and Br ${\rm\gamma }$ spectra of the observed T Tauri stars, arranged by the type of the line profile, from type I to type IV (as defined in Sect. 4 below) and for each type by alphabetical order of the name of the star. For the stars for which the veiling could be determined (FE99) the line profiles presented here are "residual'' profiles, as defined by Edwards et al. (1994). The small number of profiles obtained in UT94 are not "residual'' profiles, as veiling measurements were not possible with that data set.

Inspecting the line profiles one concludes that of the 49 stars observed at Pa ${\rm\beta }$ , 42 show the line in emission and of the 36 stars observed at Br ${\rm\gamma }$ , 30 show the line in emission. The stars without Pa ${\rm\beta }$ in emission are: DI Tau, FN Tau, Hubble 4, LkCa 7, V773 Tau, VY Tau and ZZ Tau, of which DI Tau, Hubble 4, LkCa 7 and V773 Tau are classified as Weak Line T Tauri stars (hereafter WTTS) in the Herbig & Bell Catalogue (Herbig & Bell 1988). The stars without Br ${\rm\gamma }$ in emission are: DN Tau, FP Tau, GI Tau, Hubble 4, LkCa 7 and V807 Tau of which Hubble 4 and LkCa 7 are WTTS.

From the stars observed both at Pa ${\rm\beta }$ and Br ${\rm\gamma }$ some display emission in one line but not in the other. Those with emission at Pa ${\rm\beta }$ but not at Br ${\rm\gamma }$ are DN Tau, FP Tau, GI Tau and V807 Tau. V773 Tau displays emission at Br ${\rm\gamma }$ but not at Pa ${\rm\beta }$ . While the former is not surprising, the latter would be puzzling if it were not for the highly variable characteristics of V773 Tau (Feigelson et al. 1994).

The lines that appear in emission display a variety of profiles. Although no two profiles are the same, many show similar properties and it is useful to separate them according to the general shape of the line profile.

Table 2: Classification of the Pa ${\rm\beta }$ emission line profiles according to the classification scheme developed by Reipurth et al. (1996) for the observed T Tauri stars
Type % No. Stars Star name

I 53% 20 AA Tau BM And CY Tau

DD Tau DE Tau DF Tau

DG Tau DK Tau DL Tau

DN Tau GG Tau Haro 6-13

Haro 6-37 HL Tau HK Tau

T Tau UY Aur V1331 Cyg

V807 Tau XZ Tau

II B 3% 1 CW Tau

II R 5% 2 DR Tau GW Ori

III B 0% 0 -

III R 5% 2 RY Tau SU Aur

IV B 0% 0 -

IV R 34% 13 BP Tau DO Tau DS Tau

FM Tau FP Tau FS Tau

GI Tau GK Tau GM Aur

HP Tau IQ Tau RW Aur

YY Ori

Type	%	No. Stars	Star name
I	53%	20	AA Tau BM And CY Tau
			DD Tau DE Tau DF Tau
			DG Tau DK Tau DL Tau
			DN Tau GG Tau Haro 6-13
			Haro 6-37 HL Tau HK Tau
			T Tau UY Aur V1331 Cyg
			V807 Tau XZ Tau
II B	3%	1	CW Tau
II R	5%	2	DR Tau GW Ori
III B	0%	0	-
III R	5%	2	RY Tau SU Aur
IV B	0%	0	-
IV R	34%	13	BP Tau DO Tau DS Tau
			FM Tau FP Tau FS Tau
			GI Tau GK Tau GM Aur
			HP Tau IQ Tau RW Aur
			YY Ori

3 The line spectra