Central Bureau for Astronomical Telegrams
IAUC 3308: Prob. N LMC; Poss. H20 MASER NEAR RT Ser; SS 433; MXB1730-335
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Read IAUC 3309
Circular No. 3308
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
PROBABLE NOVA IN THE LARGE MAGELLANIC CLOUD
P. Pesch and N. Sanduleak, Warner and Swasey Observatory, report
the discovery of a probable nova in the LMC on a
Curtis-Schmidt-telescope, thin-prism, IIIa-J plate taken at Cerro Tololo
on Nov. 2. The coordinates are R.A. = 5h01m.0, Decl. = -67o15' (equinox
1975.0). A strong emission feature, presumed to be the blended N1
+ N2 doublet of [O III], is the only feature observed in the
limited spectral range imposed by the use of a GG455 filter. No
continuum is observed (V > 16), which indicates that the nova is
many months past maximum and in the advanced nebular stage.
POSSIBLE H20 MASER NEAR RT SERPENTIS
N. L. Cohen, Department of Astronomy, Cornell University,
writes: "On Nov. 4 a possible H20 maser in the direction of the symbiotic
star/nova RT Ser was observed at the Haystack Observatory.
A single feature at local-standard-of-rest velocity 10.6 km/s appeared
at a peak flux of 2.0 Jy (rms noise ~ 0.51 Jy). Confirmation
of this feature and other recent observations are needed."
SS 433
Further to the note on IAUC 3305, A. Mammano and A. Vittone,
Asiago Astrophysical Observatory, report that a possible hot spot
has been detected spectroscopically; the projected rotational velocity
is 1200 km/s. New data allow reinterpretation of strong intensity
variations in bands at 5800, 5895, 5910, 5930 and 6395 A
as possibly due to changes in the excitation condition for radiation
of [Fe IV], [Mn VI], Fe IV, Mn VI and Mn V.
MXB1730-335
W. H. G. Lewin, L. Cominsky and J. van Paradijs, Massachusetts
Institute of Technology, report that they made SAS-3 observations
of the Rapid Burster on Nov. 16.71 UT for a total continuous exposure
of ~ 500 s. They did not detect any bursts and therefore
conclude that the source has stopped bursting. Periods of burst
activity occur at intervals of ~ 6.5 months and last ~ 2-6 weeks.
The source was last seen to be burst active on Oct. 11 (IAUC 3294).
The next turn-on is expected in 1979 Apr.
1978 November 21 (3308) Brian G. Marsden
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