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IAUC 5672: 1992bm; 1992t; Corrs

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                                                  Circular No. 5672
Central Bureau for Astronomical Telegrams
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

     Jean Mueller reports her discovery of an apparent supernova
(blue mag about 18) located 11" south of the nucleus of a galaxy at
R.A. = 7h29m30s.40, Decl. = +50 34'51".8 (equinox 1950.0).  The
supernova's position has end figures 30s.41, 38".4.  SN 1992bm was
found on a plate taken Nov. 25 UT by C. Brewer and Mueller with the
1.2-m Oschin Telescope in the course of the second Palomar Sky
Survey. N. Reid observed the object Dec. 1 with the Palomar 1.5-m
telescope (+ CCD camera) and reports that the object has very blue
colors V = 18.3, V-I = +0.04.

     J. G. Hills, Los Alamos National Laboratory, notes:  "The
nongravitational forces observed on this comet and the intensity and
long duration of its meteor stream suggest that large amounts of
material have been shed from this object.  At the comet's next
return, the earth may pass large pieces of comet debris as it
approaches the central core of the Perseid meteor stream.  At an
impact velocity of 60 km/s, calved pieces about 100 m in diameter
could cause airblast damage at the earth's surface.  Particularly
after perihelion, observers should search for evidence of calved
pieces along the orbit of the comet, especially near the point
where the earth is predicted to cross the orbit of the comet in
2126 (Delta(T) about +15 days)."
     U. Fink, University of Arizona, writes:  "Narrow-band filter
imaging and long-slit spectroscopy of P/Swift-Tuttle were obtained
during Nov. 24-29 UT by M. Hicks, U. Fink, M. Hoffmann, and N.
Chanover with the 1.54-m Catalina Site Telescope (+ Lunar and
Planetary Laboratory CCD and spectrometer system) of the University of
Arizona Observatories.  The comet showed three secondary nuclei (B,
C, D), whose rough separation, position angle, and magnitude
difference with respect to the primary nucleus (A) are:  B, 12".4
(11 900 km), 44 deg, 3.2; C, 19".5 (18 600 km), 70 deg, 5.2; D,
25".6 (24 500 km), 42 deg, 6.2.  Over the six days of observation,
no motion with respect to the primary nucleus could be discerned.
In addition to the secondary nuclei, very strong jet activity was
observed.  The secondary nuclei showed their own distinct comae and
associated jet structure."

On IAUC 5558, title, for  '340-G38'  read  'ESO 340-G38'; on IAUC
5660, 'Supernova 1992bl in ESO 291-G11', line 12, for  1992bk  read

1992 December 8                (5672)            Daniel W. E. Green

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