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IAUC 8252: 2003kw; 2003 EH_1, THE QUADRANTIDS

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                                                  Circular No. 8252
Central Bureau for Astronomical Telegrams
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions)
URL http://cfa-www.harvard.edu/iau/cbat.html  ISSN 0081-0304
Phone 617-495-7440/7244/7444 (for emergency use only)

SUPERNOVA 2003kw IN UGC 6314
     Further to IAUC 8245, M. Armstrong reports his discovery of an
apparent supernova (mag 18.5) on unfiltered CCD images taken with a
0.35-m reflector on Dec. 7.143 and 8.206 UT.  The new object is
located at R.A. = 11h18m12s.21, Decl. = +30o23'41".5 (equinox
2000.0), which is approximately 7".8 east and 1".5 south of the
center of UGC 6314.  Nothing was visible on Armstrong's image from
Apr. 1 (limiting mag 19.5) or Palomar Sky Survey red and blue
plates (limiting mag 20.5).

     P. Jenniskens, NASA Ames Research Center, has pointed out that
2003 EH_1 (cf. MPEC 2003-E27) would seem to be a very strong
candidate for the parent of the Quadrantid meteor stream.  The
later orbits, from arcs of up to 48 days (MPO 48330), indicate that
frequent approaches within 0.2-0.3 AU of Jupiter occur, those
during the past century or two evidently increasing q from just
under 1 AU (with other orbital elements also very similar to those
of the Quadrantids) to the present 1.19 AU.  The current
theoretical radiant for 2003 EH_1 (R.A. = 229.9 deg, Decl. = +49.6
deg; V_inf = 41.7 km/s at solar longitude 282.94 deg, equinox
2000.0) is at the center of the Quadrantid radiants measured by
photographic means, the narrow dispersion implying a young (about
500 years) shower age.  From that dispersion, Jenniskens et al.
(1997, Astron. Astrophys. 327, 1242) suspected that the parent was
still among the meteoroids, hiding as a minor planet.  On computing
a parabolic orbit for C/1490 Y1, Hasegawa (1979, Publ. Astron. Soc.
Japan 31, 257) introduced that comet as the likely Quadrantid
parent.  In attempting to link the 2003 observations to those of
1490-1491, Jenniskens, and also B. G. Marsden (Center for
Astrophysics), have found that most of the potential solutions with
the required Jan. 1491 perihelion date yield 0.5 < q < 0.6 AU in
1491, and this is probably too small to fit the data used by
Hasegawa.  Values in the more acceptable range of 0.7 < q < 0.8 AU
(and 0.80 > e > 0.75) certainly arise for 1488 < T < 1494, however,
the desired date being clearly attainable with the help also of a
close approach to the earth or -- more likely -- the presence of
nongravitational forces.  Further light could be shed on the
problem by the recognition of precovery and/or recovery
observations of 2003 EH_1, which is presumably a comet and that
should in any case be considered a high-priority object for further

                      (C) Copyright 2003 CBAT
2003 December 8                (8252)            Daniel W. E. Green

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