COMMISSION 27 OF THE I. A. U.
         INFORMATION BULLETIN ON VARIABLE STARS
                     Number 2058

                                 Konkoly Observatory
                                 Budapest
                                 1981 December 17

                                 HU ISSN 0374-0676




         HD 12180: A NEW QUADRUPLE STAR SYSTEM




  The star HD 12180 has long been known as a visual binary
(ADS 1581). In 1971 the brighter component (SAO 167451) was 
recognized as being variable by Bloomer (IBVS Nos. 586, 587). This
star was given the provisional designation BV 1481 and is now
known as AA Ceti. In 1972 Bloomer (IBVS No. 745) determined its
correct period to be 0.5361735d. More recent work by Gronbach
(IBVS No. 890) has confirmed this period. This system is of the
W Ursae Majoris type, and its eclipses appear to be complete.
At maximum light the visual magnitude of AA Ceti is 7.3, and its
spectral type is F2.
The companion of this system is SAO 167450, whose magnitude
is 7.7. It is situated 8.5" from AA Ceti, and most photometric
data for the latter have included this star in the diaphragm.
   Recently spectra were obtained of both of these stars by this
investigator using the 1.0 meter coude feed telescope of Kitt
Peak National Observatory. SAO 167450 proves to be a double-lined
spectroscopic binary. The lines are very sharp, and the spectral
type is F5. Two systems of lines are observed, those displaced to
the violet being somewhat the more intense of the two sets. The
radial velocities obtained from a single plate are as follows:


        Hel. JD         velocity


      2444887.838    -12 +- 2 km/s, +68 +- 1 km/s


The dispersion used was 16.9 A/mm. Two spectrograms were also
taken of AA Ceti on the same night. These show broad, diffuse
lines, strongly affected by rotational broadening. The mean
radial velocity for the two spectrograms, both of which were
taken near primary minimum, is +41 +- 11 km/s, a value which is
in agreement with the center-of-mass velocity which can be 
estimated from the data given for SAO 167450.
  No evidence has been presented that indicates SAO 167450 is
an eclipsing binary. Observations should be made to determine
whether or not this is the case, however, since SAO 167450 is a
double-lined system which will probably be found to have a well-
defined radial velocity curve. If the inclination of the orbit of
this system can be determined, precise masses should be obtainable 
for both components.
  The author wishes to thank Daryl Willmarth of the KPNO staff
for his assistance. He also wishes to acknowledge the support
which he received from a Small Research Grant from the American
Astronomical Society.





              CARLSON R. CHAMBLISS
              Dept. of Physical Sciences
              Kutztown State College
              Kutztown, PA USA