COMMISSION 27 OF THE I. A. U.
         INFORMATION BULLETIN ON VARIABLE STARS
                      NUMBER 886

                                  Konkoly Observatory
                                  Budapest
                                  1974 May 7


                      GL TAURI


 The star GL Tauri has been classified in the G.C.V.S. (B.V. 
Kukarkin et al. 1970) as an irregular variable connected with an
emission nebula, showing rapid light variations (Ins?). The range
of the photographic magnitudes, as determined by W. Gotz (MVS 361,
1958), is from 15.7 to 17.5.
 Fourteen plates obtained in B (103a-O + GG 13) and five in infrared
(1N + RG 5) during the period between JD 2439763 and 2439860
with the 65/90/210 cm Schmidt telescope of the Asiago Astrophysical
Observatory were examined for a study of the interconnection 
between the star and the nebula.
 At minimum in blue GL Tauri appears as a star-like object fainter
than determined by Gotz. During the period covered by the present
observations its brightness fluctuated between 18.6 and <19.0. The
small nebula (17" diameter) in which the star is embedded showed
also variations of blue brightness in some points of its surface,
particularly in the northern part. Its appearance was therefore
changing, but apparently without connection with the variations of
the star-like object.
 The star is invisible in infrared, except for one plate where it
is barely visible, near the plate limit. The nebulosity does not
appear in infrared.
 Photographs of the same region obtained in blue light with the
short focus 40/50/100 cm Schmidt telescope of Asiago show that the
integrated blue magnitude of the nebula is about 17.6. For this 
reason we think that the minimum observed by Gotz was mostly due to
the brightness of the nebula rather than to the star.
 The small emission nebulosity surrounding the star-like nucleus
suggests that the variable object GL Tauri may be in an intermediate
stage between Herbig-Haro objects and T Tauri variables.
 We are indebted to Prof. P. Maffei for the use of the plates for
this variable.



                            G. ROMANO
                        Istituto di Astronomia
                       dell'Universita di Padova