Hydrogen. The Balmer series is present in absorption from H12 to H 3. Structures are present from H5 to H 3. The Paschen lines are observed from P 25 to P 12 and P10, 9 and 7. All the lines are in emission and show structure. The underlying absorption lines are only visible sometimes. The spectral type, as derived from the equivalent width of the H6 line, corres-ponds to B 5. The Paschen line emissions are usually found only in earlier types.

Helium. Of the neutral helium series are present the lines of the

and

series. The profiles are generally in clean absorption, except for three lines, which show structures. The line 3889 from the

series is probably also present, as can be judged from the wavelength of the blend He I+ H8.

The helium lines correspond in strength to B7-8 III. It is therefore a surprise to see the He II line 10123, seen only in much hotter objects. (O to B0). No other He II line is seen, and the line was observed only in 1989.

Carbon. Ionized carbon is represented by a weak absorption line 4267 from M.6, whose strength is compatible with B 5 III, and by lines from M.14 and 37.

Nitrogen. Neutral nitrogen is well represented by emission lines from M.1, 7, 8 and 18.

Oxygen. Neutral oxygen is represented by lines from M.1, 3, 4, 8, 10 and 12. M.1, 3, 10 and 12 are seen in absorption, whereas 4 and 8 are seen in emission. Both 7774 (1) as well as 8446 (4) are strongly variable. 8446 appears in emission (as said before) and is stronger than expected, a fact which is due to fluorescence from Lyman beta.

Forbidden neutral oxygen is represented by two rather strong lines from M.1 and 3.

Magnesium. Neutral magnesium is represented by M.1(

4571), 8 (

7878+7898) and 9(

5528) in absorption but with an accompanying emission and by M.23 and 27 in emission.

Ionized magnesium is represented by lines from M.1, 4, 17 and 20. M.1 is in emission, whereas the others are in absorption. Its intensity corresponds to about B5 Ia. The presence of Mg I is therefore unexpected, since it appears in A type stars.

Aluminum. Ionized aluminum is represented by one emission line from M.40. The presence of this element is doubtful.

Silicon. Ionized silicon is represented by absorption lines from M.1, 2, 3 and 5. Their strengths are compatible with a spectral type B 5 III.

Sulphur. Forbidden ionized sulphur is represented by

4068 which exhibits an emission- absorption structure and 4076 which is in absorption, both from M.1.

Calcium. Ionized calcium is represented by lines from M.1 and 2. Whereas the EW of 3933 (M.1) corresponds to about A0, lines of M.2 are not always present and appear in emission. If the Paschen lines are substracted, the lines of M.2 have intensities which correspond to the laboratory intensity. In early type stars such ratios, which indicate an optically thin emitting medium, are unusual.

Titanium. One line from neutral forbidden titanium (

4522) is present. Ionized titanium is represented by emission lines from M.19 and [Ti II] by lines from M.5 and 22.

Chromium. Ionized chromium is represented by three lines from M.44 and one line from M.30 (in absorption) and M.24, 43 and 183 (in emission). The lines of M.44 show absorption/emission structure.

Vanadium. Three lines from M.3 and 4 of forbidden ionized vanadium are present.

Iron. Ionized iron is well represented by absorption lines from M.26, 27, 28, 36, 37, 38, 42, 48, 49, 73, 74 and 186 plus emission lines from M.41. Many lines from M.27, 28, 37, 38, 42 and 49 show structures. Probably even more would show up at higher resolution. [Fe II] is represented by numerous emission lines from M.1, 4, 6, 7, 14, 16, 18, 19, 20, 33, 41 and 44.

Zirconium. Ionized forbidden zirconium is represented by some lines from M.4 and 12.

A summary of the elements present is given in Table 3 (click here), which lists also the elements identified by other authors, namely Houziaux (1961), Doazan (1965) and Hutsemekers (1985). In general the coincidence is as well as can be expected, because the four identification works were not based upon the same wavelength regions. The only cases in which the non detection indicates a possible variability are; C II, O II, [S II] and V II.

PP = present paper. For the wavelength region covered see Table 1 (click here).
H = Houziaux (1961) ll 3642 - 8544.
D = Doazan (1965) ll 3814 - 6678.
Hu = Hutsemekers (1985). ll 1253 - 1937 2011 - 3132. The only emission lines seen correspond to Mg II and Fe II.


	PP	H	D	Hu

H	p	p	p
He I	p	p	p
He II	(p)
C I				p
C II	p			p
C IV				p
N I	p			p
II	p
O I	p	p		p
	p	p		p
O II		p
Na I	p			p
Mg I	p	p	p	p
II	p	p	p	p
Al II	p			p
Al III				p
Si II	p	p	p	p
Si III				p
Si IV				p
S II				p
	p			p
P II				p
P III				p
Ca II	p	p	p
Sc II	p		p
	p?
	p	p	p
Ti III				p
V II	p
Cr II	p	p	p	p
Mn II				p
Fe I		p?
Fe II	p	p	p	p
III				p
Ni II		p?	p	p
Zr II	p	p?

4. The behavior of the elements