Hydrogen. The Balmer series is present on our spectra from H $_\alpha$ to H $_{\gamma}$ and the Paschen series from P 11 to P 31.

Of the Balmer emission lines, H $_\alpha$ is broad; at the local mean continuum level it has a width of about 4000 km s^-1. A weak absorption line appears on the left side of H $_\alpha$ , converting the profile into a P Cyg type structure. H $_\beta$ has a width of about 600 km s^-1, no underlying absorption being visible. H $_{\gamma}$ is a relatively weak emission line, with a suggestion of two peaks, V>R. The decrement is therefore extremely strong. The profiles are illustrated in Fig. 2.

$\begin{figure*} \centering \includegraphics[width=11cm]{1499f2.eps}\end{figure*}$

Figure 2: From top to bottom and from left to right. Profile of the H $_\alpha$ line. Profile of the H $_\beta$ line. Profiles of the lines H $_{\gamma}$ and He I 4447 Å. Profiles of the He I lines 4447 and 4471 Å. Profiles of the He I lines 4146 and 4168 Å. Profile of the He I line 5047 Å

Helium. Neutral helium is represented by lines from the series ¹S, ¹D, ³S and ³D. The different lines merit some comments. $\lambda$ 4471 is composed by a faint broad absorption line, upon which two emission components are seen with V<R and separated by 340 km s^-1. In the ³S series, $\lambda$ 4713 is absent but $\lambda$ 4121, shifted by 210 km s^-1, is observed. In the ¹S series, $\lambda$ 5047 is an absorption line flanked by two emission components with V=R and $\Delta =320$ km s^-1. In $\lambda$ 4437 only the red emission is visible, whereas for $\lambda$ 4168 again two peaks are visible, separated by 230 km s^-1. In the ¹D series ${\lambda\lambda}$ 6678 and 4921 are absent and both ${\lambda\lambda}$ 4387 and 4143 are seen as an absorption accompanied by a red emission. Some of the line profiles are illustrated in Fig. 2. Ionized helium is represented by three lines ( ${\lambda\lambda}$ 4200, 4541 and 4685).

Carbon. Ionized carbon is represented by two lines from M.3, although the strong line $\lambda$ 4267 is missing. (M. stands for multiplet in what follows ).

Nitrogen. Neutral nitrogen is well represented by lines from M.1, 2, 3, 5 and 8. Forbidden singly ionized nitrogen is represented by $\lambda$ 6582 from M.1, but $\lambda$ 6545 is missing.

Oxygen. Neutral oxygen is present with lines from M.1, 4, 12 and 20; forbidden neutral oxygen with lines from M.1 and 3 (There might however exist a substantial contribution from the night sky). Singly ionized oxygen by lines from M.2 and doubly ionized oxygen is represented by two lines from M.1 and two from M.2. There exists however an anomaly in the sense that $\lambda$ 4363 is strong and $\lambda$ 4959 doubtful, whereas the inverse is true in most of the stars.

Aluminium. The ionized species is represented by a few lines from M.36, 46 and 94.

Silicium. One line from each M.2 and 5 from ionized silicium and two lines from M.2 of doubly ionized silicium are present.

Sulphur. One line from the neutral element, M.6, a possible line from M.18 of ionized sulphur and lines from S III, M.2 and 7 are present.

Titanium. Ionized titanium is represented by lines from M.20, 41, 50, 93 and 94 and by several lines of [Ti II] from M.15, 20, 21 and 39.

Chromium. Ionized chromium is represented by several lines from M.2 and 44, whereas [Cr II] shows lines from M.11, 13 and 25.

Iron. Ionized iron is represented by a large number of lines (51) from M.27, 33, 35, 37, 38, 42, 43, 73 and 197. Forbidden ionized iron is represented by 19 lines from M.1, 6, 7, 13, 14, 16, 19,21, 22, 30, 31, 32, 33, 36 and 37. Doubly ionized iron is represented by one line from M.4.

Of the elements listed we consider the identifications of Mn and Ni as marginal.

4 Behaviour of the elements