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IAUC 3549: 1980 WF; Sats OF SATURN; CH Cyg

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IAUC number


                                                  Circular No. 3549
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
TWX 710-320-6842 ASTROGRAM CAM     Telephone 617-864-5758


1980 WF
     C. Kowal, California Institute of Technology, provides the
following precise positions of a fast-moving asteroidal object,
discovered by him on plates taken at Palomar:

     1980 UT             R. A. (1950) Decl.         mpg
     Nov. 29.21111     3 50 13.43   +16 05 26.5    15.5
          29.26319     3 50 23.02   +16 03 01.4
     Dec.  1.20972     3 57 17.81   +14 29 23.6    15.5
           1.26181     3 57 28.07   +14 26 50.1


SATELLITES OF SATURN
     H. J. Reitsema, Lunar and Planetary Laboratory, informs us
that his observations of 1980 S 13, reported on IAUC 3466, should
be revised as follows: Apr. 8.31764 UT, 46".5 west; 8.35208, 45".2
west.  His calculations, utilizing also the identifications and
observations given on IAUC 3534, give a period of 1.9997 days, in
close agreement with the orbit given there and with orbit I on IAUC
3545.  Orbit II on IAUC 3545 seems to be ruled out, and it appears
that the Mar. 16 and May 19 images reported there do not belong to
the object; they are thus to be designated 1980 S 29 and 1980 S 30,
respectively.


CH CYGNI
     B. W. Bopp, Department of Physics and Astronomy, University of
Wyoming; and S. F. Smith and P. V. Noah, Department of Physics and
Astronomy, University of Toledo, write: "Though four years have
elapsed since the last reported visual outburst of CH Cyg, the
spectrum of this symbiotic star continues its dramatic evolution.
Recent observations with the Toledo 1-m and Wyoming 2.3-m reflectors
show the emission lines in the 570-670-nm region (H I, He I, Fe II,
[O I]) to be much stronger than in 1978-79.  The absorption lines of
the M star in the red are now heavily veiled by an overlying
continuum.  The D lines of Na I show sharp emission cores.  In the
infrared (2-25 um) the energy distribution is consistent with that of an
M6III star, although our observations show CH Cyg to be some tenths
of a magnitude brighter in the infrared than previously reported.
Above 5 um the energy distribution shows the silicate emission excess.
In the infrared CH Cyg resembles a Mira or SRa variable."


1980 December 11               (3549)              Brian G. Marsden

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