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THE ASTRONOMER Electronic Circular No 2153      2005 Sep 15 09.18UT
Ed:Guy M Hurst, 16,Westminster Close, Kempshott Rise,  Basingstoke,
Hants, RG22 4PP,England.Telephone/FAX(01256)471074Int:+441256471074
INTERNET: GUY@TAHQ.DEMON.CO.UK             GMH at AST.STAR.RL.AC.UK
WORLD WIDE WEB                         http://www.theastronomer.org
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EDITORIAL ABSENCE
I shall be away again from this afternoon (Sept 15) and will resume 
editorial duties on the morning of Tuesday September 20. During this 
period Nick James will be issuing any circulars required and, together 
with Denis Buczynski, will deal with any discovery claims. Contact 
details for both appear on the 'officials page' of each magazine issue.

SUPERNOVA 2005dt IN MCG -03-59-6
Discovery by LOSS of a possible supernova (IAUC 8594):
SN      2005 UT      R.A.  (2000.0)  Decl.    Mag.     Offset
2005dt  Sep.  1.36  23 23 38.32  -19 00 24.5  18.5    2.6"W, 11.7"N

POSSIBLE NOVA In SMALL MAGELLANIC CLOUD
The Central Bureau advises that the object reported by J. D. McNeill in 
the SMC (cf IAUC 8593 and E2152) is apparently the same object reported 
earlier by Bill Liller on IAUC 8582 (E2137).

V1047 CENTAURI (=NOVA CENTAURI 2005)
The object found by Bill Liller and reported on TA E-Circular 2150, has 
been designated V1047 Centauri according to a report from N. N. Samus of 
the Institute of Astronomy, Russian Academy of Sciences.

2003 UB313
J.-M. Petit, Observatoire de Besancon; M. Holman, Harvard-
Smithsonian Center for Astrophysics; and B. Gladman, University of
British Columbia, report on IAUC 8596 photometric observations of 2003 
UB313 (cf. TA E-Circular 2134).

Holman obtained 120-240-s exposures during July 30.285-30.437 and 
31.322-31.420 UT with the 6.5-m Baade telescope (+ Inamori Magellan 
Areal f/4.3 Camera and Spectrograph + Bessell R filter) at Las Campanas. 
Gladman obtained 30-120-s exposures during Aug.
2.278-2.435 and 3.330-3.382 with the 8.2-m UT-1 Very Large Telescope (+ 
FORS2 camera + specialized Bessell R filter) at Cerro Paranal.  This 
shows variability at the 0.015-mag level and may be due to rotation with 
a period exceeding 8 hours but other effects may have caused these 
results such as unknown colour terms.

Guy M Hurst