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IAUC 8589: 2005dm; 2005dn; 2005 OE_3

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IAUC number

                                                  Circular No. 8589
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 2005dm IN IC 219
     Further to IAUC 8584, M. Baek and W. Li report the LOSS
discovery of an apparent supernova on unfiltered KAIT images taken
on Aug. 26.50 (mag 17.6) and 27.51 UT (mag 17.5).  SN 2005dm is
located at R.A. = 2h18m39s.25, Decl. = -6o54'10".8 (equinox 2000.0),
which is 7".0 east and 1".5 north of the nucleus of IC 219.  A KAIT
image taken on Feb. 2.16 showed nothing at this position (limiting
mag about 19.0).

     Further to IAUC 8549, C. Jacques reports the discovery by C.
Colesanti, E. Pimentel, T. Napoleao, and himself of an apparent
supernova (mag 15.0) on unfiltered images taken on Aug. 27.03 and
28.95 UT with a 0.30-m f/3 Schmidt-Cassegrain telescope at Belo
Horizonte, Brazil, in the course of the survey by the Brazilian
Supernovae Search Team.  The new object is located at R.A. =
20h11m11s.73, Decl. = -48o16'35".5 (equinox 2000.0), which is 0".2
east and 5".6 south of the center of NGC 6861F (Sulentic and Tifft
1973, Revised NGC of Nonstellar Astron. Objects).  Nothing is
visible at this location on a CCD image taken on Apr. 5.23
(limiting mag 19.0) or on a red Palomar Sky Survey image from 1975.

2005 OE_3
     L. A. M. Benner, J. D. Giorgini, S. J. Ostro, and R. F.
Jurgens, Jet Propulsion Laboratory; and M. W. Busch, California
Institute of Technology, report:  "Goldstone 8560-MHz (3.5-cm)
radar observations of 2005 OE_3 (cf. MPEC 2005-P03) during Aug.
21.05200-21.35451 UTC reveal echoes with a visible range depth of
0.5 microsecond (75 m) that are unresolved in Doppler frequency at
a resolution of 0.025 Hz.  If we assume that the true-range extent
is double the visible-range extent, then these results establish
that P/cos(delta) > 150, where delta is the subradar latitude and P
is the rotation period in hours.  If the radar view was at least 10
degrees from the pole, then the upper bound on the bandwidth and a
diameter of 150 m imply a rotation period of at least 100 hr.  Our
radar astrometry collapsed the instantaneous 3-sigma time-delay
uncertainty on Aug. 21.00000 from 0.1 s (15000 km) to 10**-6 s
(0.15 km), reduced the 3-sigma Doppler frequency uncertainty from
1500 to 0.54 Hz, and expanded the interval of reliable close-earth-
approach predictions from the current year to the interval from
1462 to 2440."

                      (C) Copyright 2005 CBAT
2005 August 28                 (8589)            Daniel W. E. Green

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