The target stars were observed with the Aurélie spectrograph
attached to the Coudé focus of the OHP 1.52 m telescope.
The receiver was a Thomson TH 7852 double barette photocell.
The description and performance of the instrument are given in Gillet et
al. (1994).
A variety of gratings were used in order to obtain high (
),
and intermediate resolution (
) spectra.
In December 1990 we did not observe spectroscopic standard stars
because of the unfavourable weather conditions, the spectra have been
only corrected for the flat field and atmospheric extinction.
In the January 1995 observations we used 
Cet and 109 Vir for
the spectrophotometric calibration;
for the derived stellar fluxes we estimate an accuracy of about 
20%.
In the high resolution spectra we checked the wavelength calibration by measuring the position of the telluric lines. These were particularly useful to improve the precision in near-infrared region (NIR, 994-1014 nm), where the comparison spectrum has very few lines. A typical error 0.5-1 km s-1, was finally obtained for the high resolution, while for the intermediate resolution spectra the accuracy is 5-7 km s-1.
For the present work we paid attention only to hydrogen, helium,
and to a few other lines which appeared to be of particular interest
for displaying a peculiar variability.
The tracings are shown in Figs. 1 (click here) to 3 (click here),
where the wavelengths are normalized to the stellar HRV.
The results of the measurements are reported in
Table 1 where we give the spectral
resolution (
), the equivalent width (in nm),
the width (in km s-1) and the heliocentric radial velocity (HRV, in km s-1) of
the emission and absorption features (e, a).
The uncertainty in the equivalent widths, essentially due to the
choice of the continuum level, is not larger than 5%.
The HRV refer to the line emission peak (or absorption minimum), unless
specified in the notes.
The two exposures of February 1984 were obtained at the ESO CAT-CES.
Figure 1: High resolution observations of the H
region.
All the spectra but EZ CMa are normalised to the continuum.
The narrowest absorptions are telluric lines.
The spectrum of AG Dra
is shown during quiescence (December 1990) and in outburst (January 1995).
For CH Cyg the lower resolution observation is cut at the beginning of the
emission due to saturation.
The vertical bars mark a velocity shift of -500 and -1000 km s-1
with respect to H
Figure 2: Aurélie high resolution observations of the near infrared spectrum of
different stars.
The narrowest absorptions in 
Cas and 
Ori are telluric lines.
The laboratory wavelengths of Fe II 1.00 
m and P
is marked.
The files are corrected for flat field and atmospheric extinction.
UMa and CMi are normalised to the continuum.
In the different panels a vertical offset has been applied to the upper
spectrogram
Figure 3: a) the He I 667.8 nm line in 
Aqr. The smooth line is the fit
with a two-Gaussian (emission plus absorption) profile.
b) The blue spectrum of HD 200775. The weak narrow emissions
are all Fe+ lines.
c) The He I 587.6nm region in CH Cyg.
In the lower plot the high resolution
spectrum is largely affected by the telluric lines.
The laboratory wavelength of the He I and Na I lines is marked.
d-f) Profile variation of H, H and H in CH Cyg
in January 1995. Note the large variation of the blue wings of H
down to 
km s-1 from the line centre, while the other spectral lines
did not show any change.
The vertical bars mark a velocity shift of -1000 and -2000 km s-1
with respect to the Balmer lines
| star | date | range1 | resolution | line |  2 | width3 | e/a | HRV | notes |
| EZ CMa | 1995 Jan. 15.94 | 653-660 | 60000 | He II 656 | 640:: | e | +29 | 4 | |
|
Cas | 1990 Dec. 27 | 996-1014 | 50000 | Fe II 999 | 14.4 | 580z | e | -127, +134 | |
| P | 20.3 | 450z | e | -78, +106 | |||||
| N I 1011 | 4.9: | e | -34 | 10 | |||||
| 1995 Jan. 13 | 996-1014 | 50000 | Fe II 999 | 20.9 | 580z | e | -125, +103 | ||
| P | 27.1 | 530z | e | -87, +89 | |||||
| N I 1011 | 3.2 | e | 0 | 10 | |||||
| 1995 Jan. 13 | 653-660 | 60000 | H | 326.8 | e | +52 | |||
| e | -95,-15,+123 | 5 | |||||||
|
Aqr | 1990 Dec. 27 | 653-673 | 21000 | H | 179.3 | 750z | e | -79, +154 | |
| a | +49: | ||||||||
| He I 667 | 20 | 500h | e | +48 | |||||
| 15 | 323h | a | +53 | ||||||
| HD 200775 | 1995 Jan. 15 | 445-491 | 10000 | H | e | -67, +125 | |||
| a | +26 | ||||||||
|
CMi | 1990 Dec. 27 | 996-1014 | 50000 | P | a | +106 | |||
|
Ori | 1984 Feb. 4 | 653-660 | 50000 | H | 3.0 | 77h | e | +110 | 6, ESO |
| 5.7 | 144h | a | +27 | 7 | |||||
| C I 657.8 | 2.2 | a | +61 | ||||||
| C I 658.3 | 1.6 | a | +61 | ||||||
| 1990 Dec. 28 | 996-1014 | 50000 | Fe II 999 | 0.8 | 54h | e | +29 | ||
| P | 24 | a | +30 | ||||||
| HR 8752 | 1995 Jan. 13 | 653-660 | 60000 | H | e | -219, -83 | |||
| e | -16, +29 | ||||||||
| e | -137 | 5 | |||||||
| a | -181,-69,+8 | ||||||||
| [N II] 654.8 | 1.3: | e | -48: | 4, 10 | |||||
| [N II] 658.4 | 3.4 | 110z | e | -49 | 4, 10 | ||||
| AG Dra | 1990 Dec. 27 | 653-673 | 21000 | H | e | -260 | 5 | ||
| 191.4 | 810z | e | -147 | 10 | |||||
| e | -108 | ||||||||
| He I 667 | 6.0 | e | -148 | ||||||
| 1995 Jan. 16 | 653-660 | 60000 | H | e | -201 | 5 | |||
| 1085.0 | 1600z | e | -152 | 10 | |||||
| e | -115 | ||||||||
| R Aqr | 1990 Dec. 27 | 653-673 | 21000 | H | 4.0 | e | +44 | ||
| star | date | range1 | resolution | line | 2 | width3 | e/a | HRV | notes |
| CH Cyg | 1990 Dec. 28 | 585-594 | 50000 | He I 587 | 1.0: | a | -10: | 10 | |
| 1995 Jan. 14 | 570-657 | 5000 | He I 587 | 47 | e | -62 | |||
| Na D | e | -10 | 6 | ||||||
| a | -90 | 7 | |||||||
| M star | a | -50 | 9 | ||||||
| 1995 Jan. 14.2 | 570-657 | 5000 | H | a | -900, -570 | 7 | |||
| 1995 Jan. 16.2 | 653-660 | 60000 | H | 205.1 | e | -94, -19 | |||
| e | -204 | 5 | |||||||
| a | -860, -600 | 7 | |||||||
| [N II] 658 | 8.6 | e | -82 | ||||||
| 1995 Jan. 14.8 | 445-491 | 10000 | H | e | -145,-98,-7 | ||||
| a | -70 | ||||||||
| e | -406 | 5 | |||||||
| a | -1100,-540 | 7 | |||||||
| 1995 Jan. 15.8 | 445-491 | 10000 | H | e | -98, -10 | ||||
| a | -63 | ||||||||
| e | -206 | 5 | |||||||
| a | -600 | 7 | |||||||
| 1995 Jan. 11.8 | 405-450 | 7000 | H | e | -126, -15 | ||||
| e | -290, -200 | 5 | |||||||
| a | -70 | ||||||||
| a | -520 | 7 | |||||||
| 1995 Jan. 12.2 | 405-450 | 7000 | H | e | -120, -19 | ||||
| e | -290, -210 | 5 | |||||||
| a | -70, | ||||||||
| a | -510 | 7 | |||||||
| 1995 Jan. 15.2 | 405-450 | 7000 | H | e | -154, -16 | ||||
| e | -287 | 5 | |||||||
| a | -70, | ||||||||
| a | -600 | 7 | |||||||
| 1995 Jan. 11.8 | 405-450 | 7000 | H | e | -245,-126,-10 | ||||
| a | -70, | ||||||||
| a | -510 | 7 | |||||||
| 1995 Jan. 12.2 | 405-450 | 7000 | H | e | -15 | ||||
| e | -230, -127 | 5 | |||||||
| a | -480 | 7 | |||||||
| 1995 Jan. 15.2 | 405-450 | 7000 | H | e | -150, -10 | ||||
| a | -70, | ||||||||
| a | -740, -430 | 4, 7 | |||||||
| KQ Pup | 1984 Feb. 3 | 653-660 | 50000 | H | 25.4 8 | e | -16, +59 | ESO | |
| a | +14 | ||||||||
| M star | a | +39 | 9 | ||||||
| 1990 Dec. 28 | 996-1014 | 50000 | Fe II 999 | 0.68 | 15h | e | +25 | 10 | |
| M star | a | +34 | 9 | ||||||
| 1995 Jan. 16 | 996-1014 | 50000 | Fe II 999 | 0.62 | 15h | e | +18 | 10 | |
| M star | a | +23 | 9 | ||||||
| 653-660 | 60000 | H | 107.8 8 | e | -32, +48 | ||||
| a | +19 | ||||||||
| M star | a | +24 | 9 | ||||||
|
|
1 Spectral range in nm.
2 Equivalent width in 10-2 nm.
3 h: FWHM of gaussian fit, z: FWZI, in km s-1.
4 Broad, flat-topped line.
5 Hump in the line profile.
6 Emission component of P Cygni profile.
7 Absorption component of P Cygni profile.
8 Integrated over the whole profile.
9 Mean HRV of the M-star absorptions.
10 line barycentre.