COMMISSION 27 OF THE I. A. U.
        INFORMATION BULLETIN ON VARIABLE STARS
                     Number 1158

                                Konkoly Observatory
                                Budapest
                                1976 July 27


          BV 1616 Lep - A PROBABLE MIRA VARIABLE


    The variability of BV 1616 Lep = CSV 717 = Ross 354 has been
discussed by Markworth (1), Locher (2) and summarised by Bateson
(3). The star varies by about 4 mag on a timescale of a few 
hundred days and was suspected of being a long period eclipsing or
eruptive variable.
    A spectrum of BV 1616 Lep was obtained on May 19.38 (UT)
(JD 2442917.88) at the Anglo-Australian 3.9m Telescope using the
Wampler Robinson Image-Dissector Scanner. The spectrum is shown
together with that of RS Cen, a Mira variable, obtained on the
same night. The wavelength scale is somewhat non-linear and the
intensity scale has not been absolutely calibrated and includes
detector response. Several features due to TiO and VO absorption
and Hgamma and Halpha emission are identified. The spectral type of BV
1616 Lep based on the calibration of Keenan (4) is M5e, with an
uncertainty of two subclasses. The luminosity class could not be
determined. The spectrum is clearly not that of a dwarf nova, or
eruptive variable.

                      [FIGURE 1]

    The effective integrated magnitude of BV 1616 Lep at the
epoch of observation was 15.2 +- 0.6 mag and it was 2.0 +- 0.3 mag
fainter than RS Cen.
    A spectrum of the star 18 arcsec west of BV 1616 Lep was
also obtained since it too was a suspected variable (2). It is
of solar spectral type or later with no special peculiarities,
and about 0.5 + 0.2 mag fainter than BV 1616 Lep but not nearly
as red.
    Considering its probable long period variability, its spectral 
similarity to RS Cen and its Halpha emission, it is very probable 
that BV 1616 Lep is a Mira variable. Whether it eclipses or
not is another matter. A determination of the period and amplitude 
of the light curve would be useful.

    We acknowledge help from D.A. Allen, F.M. Bateson, A.J.
Longmore, K. Locher and S.K. Mayo.


J.A.J. WHELAN                  D.T. WICKRAMASINGHE

Anglo-Australian Observatory   Department of Applied
P.O. Box 296, Epping           Mathematics,
NSW 2121, Australia            Australian National University
                               A.C.T. 2606, Australia



References:
1.   Markworth, N.L. 1974, I.B.V.S. No. 921.
2.   Locher, K. 1975 and 1976, B.B.S.A.G. Bulletins 19,
     20, 21 and 25.
3.   Bateson, F.M. 1976, Circ. M76/3 V.S.S., R.A.S.N.Z.
4.   Keenan, P.C. 1966, ApJ. Suppl. No. 118. [BIBCODE 1966ApJS...13..333K ]