COMMISSION 27 OF THE I. A. U. INFORMATION BULLETIN ON VARIABLE STARS Number 2041 Konkoly Observatory Budapest 1981 November 12 HU ISSN 0374-0676 SPECTROSCOPIC OBSERVATIONS OF SYMBIOTIC STARS IN JULY AND SEPTEMBER 1981 The visible spectra of the following symbiotic stars were recorded on July and September 1981 with the 80 cm Telescope at the Observatoire de Haute Provence. The spectrograph was equipped with an R.C.A. tube and the spectrum was recorded on IIaO plates. The spectral range is from Lambda3600A to Lambda5300A and the reciprocal dispersion is 92.8 A/mm at Hgamma. We report here the most conspicuous features in the following tables. R. GRAVINA Observatoire de Lyon 69230 Saint-Genis-Laval Elements (O III) (Ne III)HeII FeII (FeII) FeIII (FeV) (FeVII) N III HI HeI C III I.P. 54.9 ev 63.4 54.4 16.2. 16.2 30.7 75 103 47.5 13.6 24,4 47.9 Stars L4363 L4959 L5007 L3868 L4686 L3760 L4640 ----------------------------------------------------------------------------------------------------------- CI Cyg x x s s s w w x 1 Z And w s w w x x 2 BF Cyg x x s s w w x x w 3 AX Per x x s s s w w x x w 4 AG Peg w w x s x x x 5 AG Dra s w x 6 YY Her s w w x w x 7 V 1016 Cyg s s s s s x x x x s x x x x 8 EG And x x x x 9 TX CVn x 10 T CrB x x x x 11 CH Cyg x x x 12 HBV 475 x x s x s x x x x x w 13 ----------------------------------------------------------------------------------------------------------- x: Present s: Strong w: Weak L: Lambda Elements TiO alpha system Stars 4761 4804 4954 5167 ----------------------------------------------- CI Cyg Z And x x x BF Cyg x AX Per x x x AG Peg x x AG Dra YY Her V 1016 Cyg EG And x x x x TX CVn s s s s T CrB x x s s CH Cyg x x HBV 475 ----------------------------------------------- x : Present s : Strong 1. The circumstellar nebula is certainly strong. H_gamma and (OIII) 4363 A have the same intensity. In September 1981, the blue red region is similar to that of Z And. 2. The cool giant type dominates and high excitation lines are very weak. 3. In July 1981, in the blue red region the spectrum is very similar to CI Cygni. 4. The TiO bands are stronger than in the spectrum of BF Cygni. Absorption line Ca I at Lambda4227 A appeared in September 1981. 5. The absorption bands of TiO (4954 and 5157) are little developed. He II Lambda4686 A is much stronger than H_beta. 6. Strong continuum is visible at Lambda<3600 A and. Lambda> 4600 A 7. The high excitation lines from optical range are in agreement with U V observations. 8. This star is characterized by high excitation lines due to a very hot source of radiation. 9. Absorption line CaI at Lambda4227 A is present in September 1981. An overlying continuum is visible at Lambda>4400 A. 10. The TiO absorption bands are stronger than in the spectrum of T CrB. The continuum in the blue red region is very strong. 11. The bands of TiO and some atomic lines Lambda4326 A, Lambda4404 A of FeI are strongly developed in absorption. 12. Absence of high excitation lines. The M spectrum dominates in the blue red region. 13. The (OIII) line Lambda5007 is much stronger than Lambda4363 A. The nebular component in the system is much developed.