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IAUC 8472: 2005N, 2005O,, 2005P; 2001em

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                                                  Circular No. 8472
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)

SUPERNOVAE 2005N, 2005O, AND 2005P
     Further to IAUC 8470, J. Burket and W. Li report the LOSS
discovery of an apparent supernova on unfiltered KAIT images taken
on Jan. 21.55 (at mag 18.1) and 22.54 UT (mag 18.0).  SN 2005P is
located at R.A. = 14h06m34s.01, Decl. = -5o27'42".6 (equinox 2000.0),
which is 12".6 west and 31".7 south of the nucleus of NGC 5468.  A
KAIT image taken on 2004 July 8.21 showed nothing at this position
(limiting mag 19.5).
     B. Schmidt and M. Salvo, Australian National University,
report that a spectrogram (range 420-1000 nm) of SN 2005O (cf. IAUC
8471), obtained by P. Wood on Jan. 21.70 UT with the ANU 2.3-m
telescope (+ DBS), reveals it to be a type-Ib supernova near
maximum light.  The relatively red spectrum is dominated by He I
lines and the Ca II infrared triplet.
     S. Taubenberger and A. Pastorello, Max-Planck-Institut fuer
Astrophysik, Garching, on behalf of the European RTN collaboration,
report that inspection of a low-S/N spectrogram of SN 2005N (cf.
IAUC 8470), taken on Jan. 22.21 UT by M. Alises with the Calar Alto
2.2-m telescope (+ CAFOS; range 330-880 nm), shows it to be a type-
Ib/c supernova in the nebular phase, about 4 months after the
explosion.  The spectrum is characterized by strong emission lines
of [O I]; features due to [Ca II], Mg I], [Fe II], Na I, O I, and
Ca II are also visible.

SUPERNOVA 2001em IN UGC 11794
     C. J. Stockdale and B. Kaster, Marquette University; L. O.
Sjouwerman and M. P. Rupen, National Radio Astronomy Observatory; I.
Marti-Vidal and J. M. Marcaide, University of Valencia; S. D. Van
Dyk, Spitzer Science Center, California Institute of Technology; K.
W. Weiler, Naval Research Laboratory; B. Paczynski, Princeton
University; and N. Panagia, European Space Agency and Space
Telescope Science Institute, report a test of the proposal by
Paczynski (2001, Acta Astron. 51, 1) and by Granot and Loeb (2003,
Ap.J. 593, L81) that type-Ib/c supernovae may produce late-time
radio jet emission.  A Very Long Baseline Array measurement on 2004
July 1 of the oldest known radio-emitting type-Ib/c supernova, SN
2001em, at age about 1020 days after explosion, shows no extended
radio emission to a 3-sigma limit of 0.3 mJy/beam.  The detected
radio emission at 8.4 GHz of 1.8 +/- 0.2 mJy from SN 2001em appears
unresolved at a resolution of 0".0019 x 0".0008, corresponding to a
radius of < 0.4 +/- 0.2 pc at a distance of 90 Mpc or an average
expansion speed for any detectable radio emitting material of <
150000 km/s (< 0.5c).

                      (C) Copyright 2005 CBAT
2005 January 22                (8472)            Daniel W. E. Green

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