COMMISSION 27 OF THE I. A. U. INFORMATION BULLETIN ON VARIABLE STARS NUMBER 372 Konkoly Observatory Budapest 1969 August 29 EMISSION OBJECT MHalpha 328-116 = V 1016 Cyg Spectral observations of V 1016 Cyg = MHalpha 328-116 were carried out in the Cracow Observatory. The spectrograms were taken on July 23, 26, 27, 28 and August 6, 1969 with a 5deg objective prism attached to the 35 cm Maksutov reflector, The dispersion is 320 A/mm at Hgamma. The ZU2 (ORWO-Astro- Special- unsensitized) plates were used. Two plates, from July 23 and August 6, were calibrated photometrically and the intensities of the emission lines being the means of two night values were given in Table 1. All intensity estimates have been reduced for the plate sensitivity. On the spectrum plate taken July 26, the lines FeII (lambdalambda 4582.8, 4583.8), [Fe II] (lambda 4413.8), He I (lambdalambda 4026.1, 3819,6) and He II (lambda 4685.7) appear to be somewhat stronger relative to the hydrogen lines than in the other spectra, especially He I (lambda 4026.1) and He II (lambda 4685.7). In general, the spectrum of V 1016 Cyg = MHalpha 328-116 shows the character described by FitzGerald (1966) and McCuskey (1967). The continuum in extremely weak and on the plates obtained at Cracow it is impossible to find any traces of absorption lines. However, some significant changes can be observed, The line He II (lambda4685.7) was observed by FitzGerald (1968) in July and September 1965 to have a broad and very weak emission feature, later McCuskey (1967) observed it sharp and strong. The present observations of this line show it as a broad and rather weak feature. The [0 III] lines are very strong but, lambda4363.2 mentioned by McCuskey to be considerably stronger relative to lambda 4958.9 and lambda 5006.8 [O III] is at present weaker than, lambda 5006.8, which is extremely intense. The very strong intensity of the forbidden lines [Ne III] is striking, especially at lambda 3868.7. Cracow, August 1969 M. KURPINSKA Astronomical Observatory of the Jagellonian University References Bloch, 1965 I. A. U. Circular No. 1927. FitzGerald, Houk, McCuskey, Hoffleit, 1966, ApJ 144, 1135. [BIBCODE 1966ApJ...144.1135F ] McCuskey 1967 I. A. U. Circular No. 2018. Rosino 1965 I. A. U. Circular 1917. [BIBCODE 1965IAUC.1917....0R ] Table 1 Identification of Emission Lines in V 1016 Cyg Intensity* Suggested identification Element I_Hbeta = 100 3797.9 A H 10 23.5 3819.6 very weak He I ---- 3835.4 H 9 36.8 3868.7 [Ne III] 265.8 3889.0 H 8 62.2 3967.0 \ He I 102.7 3967.5 blend [Ne III] " 3970.1 / Hepsilon " 4026.2 very weak, visible on He I --- July 26 only 4067.9 \ C III 15.3 4068.6 blend [S II] " 4068.9 / C III " 4076.2 [S II] 18.1 4101.7 H delta 44.6 4276.8 \ [Fe II] 9.3 4287.4 line very large [Fe II] " 4305.9 /blended [Fe II] " 4340.5 H 59.9 4363.2 [O III] 116.4 4413.8 \ [Fe II] 7.2 4414.4 band from lambda4413 [Fe II] " 4416.3 /to lambda4416 [Fe II] " 4470.3 \ [Fe II]? 14.0 4471.5 band from lambda4470 [Fe II] " 4472.9 / to lambda4473 [Fe II] " 4582.8 blend, very weak [Fe II] ___ 4583.8 / [Fe II] 4640.6 N III 13.9 4686.7 broad He II 23.1 4713.4 He I 16.2 4861.3 Hbeta 100.0 4921.9 blend He I 91.0 4958.9 / [O III] " 5006.8 [O IIl] 291.4 * intensities of the lines reduced for the plate sensitivity.