Central Bureau for Astronomical Telegrams
IAUC 4555: 4U 0115+63; 1986l; MOLECULES IN EXTERNAL GALAXIES
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Read IAUC 4556
Circular No. 4555
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 617-495-7244/7440/7444
4U 0115+63
H. Mendelson and T. Mazeh, Wise Observatory, report: "The
optical counterpart of the x-ray pulsar 4U 0115+63 is probably going
into another eruption. Between Feb. 5 and 10 the stellar I magnitude
was observed to be 12.15 +/- 0.1, similar to the observed magnitude
at the peak of the previous optical and x-ray eruption of
1987 Feb. (IAUC 4342, 4350). Optical spectroscopic and x-ray
observations are strongly urged."
COMET WILSON (1986l)
S. M. Larson, Lunar and Planetary Laboratory, writes that
broad, red-band CCD images with the 1.5-m Catalina reflector by D.
Levy and himself on Feb. 23.4 UT confirm that the comet has split
(cf. IAUC 4552). The well-defined secondary was more diffuse than
field stars. A 300-560 nm CCD spectrum showed only continuum.
J. V. Scotti, University of Arizona, reports the following
data obtained with the 0.92-m SPACEWATCH camera at Kitt Peak: Feb.
13.27 UT, principal nucleus m2 = 17.7, second nucleus m2 = 19.6,
separation 8".4 in p.a. 117 deg.
D. Jewitt and J. Luu, Massachusetts Institute of Technology,
report that observations with the McGraw-Hill 2.4-m telescope (+
Mascot CCD camera, Mould r filter) on Feb. 22.22 UT show that the
secondary nucleus is 8".7 east and 4".7 south (+/- 0".6) of the main
nucleus, and that the secondary is fainter than the primary by 2.0
+/- 0.2 mag. The secondary appears broader than stellar images.
MOLECULES IN EXTERNAL GALAXIES
C. Henkel, R. Mauersberger, and P. Schilke, Max-Planck-Institut
fur Radioastronomie, Bonn, write: "We report the first detection
of extragalactic CN, HNC, and C2H, and the tentative detection
of extragalactic HC3N from measurements carried out with the IRAM
30-m telescope. CN emission (mapped in the N = 1-0 or N = 2-1
transition toward NGC 258, IC 342, and M82) is spatially confined
to the nuclear regions (</= 40"). HNC was observed in IC 342, C2H in
M82, and HC3N may have been detected in IC 342 and M82. A
preliminary comparison with H2 column densities indicates that either
abundances are higher than in typical galactic cloud cores or peak
H2 column densities are larger than those derived from CO data."
1988 February 25 (4555) Daniel W. E. Green
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