Circular No. 8233
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
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SUPERNOVA 2003jf IN MCG +11-22-9
     Further to IAUC 8226, T. Boles reports the discovery, on
unfiltered CCD images taken on Oct. 26.785 and 27.750 UT, of an
apparent supernova (mag 18.4) located at R.A. = 17h53m33s.45, Decl.
= +64o10'12".1 (equinox 2000.0), which is approximately 4".0 east
and 11".1 south of the center of MCG +11-22-9.  SN 2003jf is not
present on his images from Sept. 13, 25, and Oct. 16 (limiting mag
19.5) or on Palomar Sky Survey red or blue plates.


SUPERNOVA 2003jc IN MCG -01-58-18
     T. Matheson, P. Challis, and R. Kirshner, Harvard-Smithsonian
Center for Astrophysics, report that a spectrum (range 370-750 nm)
of SN 2003jc (cf. IAUC 8232), obtained by M. Calkins on Oct. 26.22
UT with the F. L. Whipple Observatory 1.5-m telescope (+ FAST
spectrograph), shows a blue, almost featureless continuum.  There
are nascent P-Cyg lines of hydrogen and helium, implying that this
is an early type-II supernova.


1937 UB (HERMES)
     P. Pravec and P. Kusnirak, Ondrejov Observatory; B. Warner,
Colorado Springs, CO, U.S.A.; R. Behrend, Geneva Observatory; A. W.
Harris, Space Science Institute; A. Oksanen, Jyvaskyla, Finland; D.
Higgins, Canberra, Australia; R. Roy, Blauvac, France; C. Rinner,
Ottmarsheim, France; C. Demeautis, Village-Neuf, France; F. van den
Abbeel, Vesqueville, Belgium; A. Klotz, Guitalens, France; N.
Waelchli, Observatoire Francois-Xavier Bagnoud, St-Luc, Switzerland;
T. Alderweireldt, 's-Gravenwezel, Belgium; V. Cotrez, St-Helene,
France; and L. Brunetto, Pitalugue, France, report that their
photometric observations obtained during Oct. 16-26 show a light-
curve period for Hermes of 13.892 +/- 0.006 hr with amplitude 0.07
+/- 0.01 mag.  A smooth shape of the lightcurve with only a single
confirmed periodicity suggests that it is most likely the combined
rotational lightcurve of two bodies synchronously locked to the
orbital period (cf. IAUC 8227).  The low amplitude implies that the
two components seen by radar are physically separate orbiting
bodies.  No attenuations caused by mutual occultation/eclipse
events were detected, implying that the mutual orbital plane was
inclined to both the line of sight and the direction to the sun, or
much less likely, that the orbital period is different from the
detected rotation period.  Continued monitoring for mutual
occultations, as the viewing geometry changes, is warranted.  The
system's total absolute magnitude is H = 17.55 +/- 0.10.

                      (C) Copyright 2003 CBAT
2003 October 27                (8233)            Daniel W. E. Green