COMMISSION 27 OF THE I. A. U.
        INFORMATION BULLETIN ON VARIABLE STARS
                     Number 1313

                                   Konkoly Observatory
                                   Budapest
                                   1977 July 29



                    CD -30d 5135



Photographic magnitudes for this star have been measured on two sets of
UBV plates taken by Mr. A. Kinnander on Feb. 20, 1977, with the Schmidt
telescope at Uppsala Southern Station at Mount Stromlo Observatory,
Australia. The photometric calibration was made by means of a sequence
established by Loden (Ark. Astr. 5, 149, 1968; sequence 5-), about 30'
south of the star. The following values were obtained, with an estimated
error of about +-0.1 mag.


   V = 9.3   B = 10.2    U = 10.6

Thus the star was then 0.3 - 0.4 mag. brighter than when it was observed
by Humphreys in 1974 (PASP 87, 933, 1975).
A low-dispersion spectrogram covering the region 3600 - 5500 Angstrom was kindly
taken for me by Dr. A. Lauberts on Jan. 17, 1977, with the Boller and
Chivens spectrograph at the 1.5 m telescope at ESO, Chile. No significant
changes from the spectra reported by Humphreys (op. cit.) and myself
(IBVS No 1139, 1976) were found, i.e., the spectral type is early F. Hbeta
is present in emission, whereas Hgamma and Hdelta are invisible.

In my previous paper on this star the radial velocity correction to the
sun was inadvertently applied with the wrong sign. Hence all velocities
should be increased by about 30 km/s, the metal line velocity on Dec. 2,
1973, being 159 km/s. However, this only strengthens the conclusion drawn
in that paper, viz., that the observed radial velocity changes were not
caused by the orbital motion of a spectroscopic binary.


                                     GUNNAR WELIN
                                     Astronomiska Observatoriet
                                     Box 515
                                     S-751 20 Uppsala, Sweden