Central Bureau for Astronomical Telegrams
IAUC 3532: SN IN NGC 6946; Sats OF SATURN; HD 44179; W Hya
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Circular No. 3532
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
SUPERNOVA IN NGC 6946
Paul Wild, Astronomical Institute, Berne University, reports
his discovery of a supernova 280" east and 166" south of the nucleus
of NGC 6946 (R.A. = 20h34m.4, Decl. = +59o56', equinox 1950.0). The
photovisual magnitude on Oct. 28 was 13. The discovery was confirmed
by R. Barbon at the Asiago Astrophysical Observatory on Oct.
29. Supernovae 1917A, 1939C, 1948B and 1968D were also located in
NGC 6946.
SATELLITES OF SATURN
B. A. Smith and the Voyager Imaging Science Team report the
discovery from Voyager 1 of two new satellites, 1980 S 26 and 1980
S 27, just outside and just inside the F ring. First detected in
mid-October, the objects were particularly well observed during a
10-hr sequence on Oct. 25. 1980 S 26 has an orbital radius of
142.0 Mm (= 2.37 Rs; P = 0.630 day), 1980 S 27 one of 139.5 Mm
(= 2.33 Rs; P = 0.614 day). As seen from the earth, the objects
would be of mag ~ 15, the former slightly brighter than the
latter.
HD 44179
E. M. Leibowitz and M. Livio, Wise Observatory, report: "Photometric
measurements of the 'red triangle' (HD 44179) on four nights
in Sept. and one night in Oct. show the object to be stable within
0.02 mag in its UBV magnitudes. The measured colors are the same
as found by Cohen et al. (1975, Ap.J. 196, 179)."
W HYDRAE
A. M. Gomez Balboa and J. R. D. Lepine, Observatorio Nacional,
Sao Paulo, report that observations made on Oct. 25 with the
Itapetinga radio telescope revealed that the usually strong H2O-maser
emission at 22 GHZ from the long-period variable W Hya (R.A. = 10h43m.4,
Decl. = -27o52', equinox 1900.0) is currently not detectable, to a
limit of detection of ~ 20 Jy. This result is surprising because
the star is currently near its optical maximum, and the SiO-maser
lines at 43 GHz are intense, as would be expected at this phase.
Such a phenomenon has not occurred before in a five-year monitoring
of the periodic variability of the H2O emission of this star.
1980 October 31 (3532) Brian G. Marsden
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