Electronic Telegram No. 368
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
M.S. 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
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CBAT@CFA.HARVARD.EDU (science)
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SUPERNOVAE 2006F AND 2006G
     N. Morrell, G. Folatelli, M. Hamuy, and M. M. Phillips, on behalf of
the Carnegie Supernova Project, report spectroscopic observations (range
400-1020 nm) of SN 2006F (cf. IAUC 8658) and SN 2006G (cf. CBET 365)
obtained on Jan 16.05 and 16.07 UT, respectively, with the European
Southern Observatory 3.6-m New Technology Telescope (+ EMMI spectrograph).
     SN 2006F is a type-Ib supernova about ten days after maximum light.
The spectrogram shows prominent He I lines with P-Cyg profiles.  Assuming
the NED recession velocity of 4142 km/s for the host galaxy (from Giovanardi
and Salpeter 1985, Ap.J. Suppl. 58, 623), an expansion velocity of 11000
km/s is derived from the absorption minima of He I 597.6-, 667.8-, and
706.5-nm and O I 777.4-nm.
     SN 2006G is a type-II supernova with a strong H_alpha P-Cyg feature and
some metallic lines.  Weak H_beta is detected in absorption, indicating an
expansion velocity of 10000 km/s, if one assumes the NED recession velocity
of 5018 km/s for the host galaxy (from Huchra et al. 1999, Ap.J. Suppl. 121,
287).  The presence of Fe II 516.9-nm and the high expansion velocity
derived from H_beta suggest that the supernova is 2-3 weeks old.


NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
      superseded by text appearing later in the printed IAU Circulars.

                         (C) Copyright 2006 CBAT
2006 January 16                  (CBET 368)               Daniel W. E. Green