Central Bureau for Astronomical Telegrams
IAUC 5960: PU Vul; 1992bu; 1994a
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Circular No. 5960
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
Telephone 617-495-7244/7440/7444 (for emergency use only)
TWX 710-320-6842 ASTROGRAM CAM EASYLINK 62794505
MARSDEN@CFA or GREEN@CFA (.SPAN, .BITNET or .HARVARD.EDU)
PU VULPECULAE
H. Nussbaumer and M. Vogel, Institute of Astronomy, Zurich,
write: "International Ultraviolet Explorer observations of the
symbiotic nova PU Vul show that this object has entered an eclipse
(V = 10-11). This is the first eclipse after the fading in 1980,
the cause of which is still debated. The IUE short-wave continuum
has strongly decreased; this is due to the eclipse of the hot
radiation source by the red giant. The broad emission features He
II 164.0-nm, N V 124.0-nm, and N IV 171.8-nm (from the wind of the
hot star) have disappeared, whereas the nebular emission lines are
still present. We estimate that the end of eclipse should occur
between the end of March and end of August 1994. We shall cover
this period with IUE observations, but optical spectroscopy over
this period is strongly desirable. Changes in visual magnitudes
may remain small. However, the broad stellar wind lines should
show a big increase on the way out of eclipse, in particular He II
468.6-nm, N IV 405.8-nm, and N III 464.3-nm, as well as the broad
feet of the Balmer lines. Before going into eclipse, the width of
these lines indicated wind velocities of about 500 km/s."
SUPERNOVA 1992bu IN NGC 3690
D. Van Buren, T. Jarrett, S. Terebey, and C. Beichman, Infrared
Processing and Analysis Center, California Institute of Technology
and Jet Propulsion Laboratory; and M. Shure and C. Kaminski, NASA
Infrared Telescope Facility, Institute for Astronomy, University of
Hawaii, report their discovery of an apparent supernova in NGC 3690
(= Markarian 171) at R.A. = 11h25m42s.0, Decl. = +58o50'10" (equinox
1950.0) on archival images taken in the K (2.2-micron) band as part
of a search for supernovae in starburst galaxies. Offsets from Core
B1 (cf. Wynn-Williams et al. 1991, Ap.J. 377, 426) of the galaxy are
5" east and 3" south. The object appears in ProtoCam data (obtained
at the IRTF, Mauna Kea) for 1992 Mar. 9 UT (when K = 16.6 +/- 0.2),
Apr. 10 (17.2 +/- 0.3), and May 6 (18.1 +/- 0.5). It does not
appear to limiting magnitude K about 19 in NSFCam IRTF images from
1993 Dec. 27.
PERIODIC COMET KUSHIDA (1994a)
Total V CCD magnitudes by H. Mikuz, Ljubljana, Slovenia (0.20-
m reflector): Mar. 4.85 UT, 11.5; 29.86, 13.1.
1994 March 30 (5960) Daniel W. E. Green
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