COMMISSION 27 OF THE I. A. U. INFORMATION BULLETIN ON VARIABLE STARS Number 2679 Konkoly Observatory Budapest 5 March 1985 HU ISSN 0374 - 0676 SEARCH FOR PECULIAR STARS IN THE REGION OF THE ASSOCIATION CASSIOPEIA OB 14 The search for peculiar stars can provide valuable information concerning their evolutionary status. Up to now this kind of work has been mostly restricted to accidental discoveries in different regions of the sky. The point is to look for indications of a possible preference of such special objects to certain stellar groups. In this respect, more observational data are desirable about the presence of these stars in star clusters and associations. A program, initiated by us, of objective prism spectral classification in the regions of five OB-associations (in press), gave us the opportunity to reveal a great number of new peculiar or otherwise astrophysically interesting stars. A list of 90 stars, 73 of which - new-recognised as peculiar, in the region of the associations Cygnus OB 4, Cepheus-Lacerta OB 1 and Cassiopeia OB 9, has been published earlier (Radoslavova Ts., 1978, Astron.Tsirk., No. 979, 5). The present list contains the results of an objective prism inspection for peculiar stars in a region of about 60 square degrees, centered at the association Cassiopeia OB 14. The plates are taken with the 70 cm meniscus telescope of the Abastumani Astrophysical Observatory (USSR) using an 8deg-objective prism. The reciprocal dispersion at H_gamma is 166 A/mm and the spectra are widened to 0.4 mm. Each plate has a diameter of 4d50', with high-quality images to the extreme edge. The exceptional seeing at Abastumani together with the purity of the spectra allows peculiar star discoveries with a great certainty (Kharadze E.K., Bartaya R.A., 1973, IAU Symp., 50, 91). The Table lists the stars suspected in peculiarity, together with their positions (1950) and magnitudes given in the Bonner Durchmusterung. The stars sufficiently bright to be listed in the HD-catalogue are designated by their HD-numbers and magnitudes. There are several stars of about 9.5 to 10 photographic magnitude which are not present in the BD; for them the approximate coordinates are indicated, as calculated by us. In the last column the observed peculiarities in the spectra are noted; the semicolon indicates weak characteristics of the type. Table I ------------------------------------------------------------------- HD or BD R.A. Decl. m Remarks and type ------------------------------------------------------------------- - 00h04.7m 63d49' - Ap ;lambda4128 - 00 09.4 59 47 - Ap ;lambda lambda4128,4077 962 00 11.4 60 27 7.76 A+G comp. +63d0020 00 13.8 64 08 9.5 Am +65d0032 00 16.4 65 53 9.2 Ap ;lambda lambda4128,4077 +61d0045 00 18.2 62 30 9.4 Ap or Am ; 4128,4070,4030 - 00 20.4 62 24 - Ap ; lambda4128 2032 00 22.4 62 55 8.8 Am ; SAO 11176 +63d0044 00 22.9 63 33 9.4 Ap;; lambda4128 - 00 26.6 62 31 - Ap ; lambda4128 +64d0051 00 26.9 65 08 9.3 Ap:; lambda4128 +65d0065 00 28.0 65 52 9.2 Ap ; lambda4128 +59d0081 00 32.4 60 11 9.3 Am or F0p +61d0126 00 32.5 62 17 9.4 Am : +62d0154 00 43.7 63 05 8.5 Am +61d0180 00 51.5 61 37 9.3 Ap ; lambda4128 +63d0109 00 51.8 64 16 9.3 Ap ;lambda lambda4128,4077 +65d1981 23 58.3 66 22 9.2 Ap ; lambda4128 ------------------------------------------------------------------ The low dispersion used did not permit us to give a more precise type of peculiarity; it is even possible some stars classified as Am to prove to be Ap, or vice versa, So, the interpretation of our discoveries is not straightforward. A higher resolution study of the objects in the list is obviously desirable, as well as information about their membership in the association, that should be acknowledged by the author. TSVETANKA RADOSLAVOVA Department of Astronomy with National Astronomical Observatory Bulgarian Academy of Sciences 72, bld. Lenin, 1784, Sofia Bulgaria