Central Bureau Electronic Telegrams, 2011, 1 (2009/November-0)
Supernovae 2009kn, 2009ko, 2009kq, and 2009kr.
STEELE T.N., COBB B. and FILIPPENKO A.V.
Abstract (from CDS):
T. N. Steele, B. Cobb, and A. V. Filippenko, University of California, Berkeley, report that inspection of a CCD spectrum (range 345-1000 nm), obtained on Nov. 9 UT with the 3-m Shane reflector (+ Kast) at Lick Observatory, shows that 2009kr (CBET 2006) is a young type-II supernova with a very blue continuum and weak P-Cyg profiles of the hydrogen Balmer series; the narrow Balmer emission lines mentioned by Tendulkar et al. (at website URL http://www.astronomerstelegram.org/?read=2291
) appear to be produced by a superposed H II region, and the apparent width of the H-alpha emission line is caused by blending with [N II] lines at 654.8 and 658.3 nm. SN 2009kq (CBET 2005) is a normal type-Ia supernova near maximum light; cross- correlation with a library of supernova spectra using the "SuperNova IDentification" code (SNID; Blondin and Tonry 2007, Ap.J. 666, 1024) indicates that it is most similar to SN 2003cg at two days before maximum light, while on the previous night, Tendulkar et al. (op.cit.) suggested that SN 2009kq was about one week prior to maximum. SN 2009kn (CBET 1997) is a type-IIn supernova, with the hydrogen Balmer emission lines being very strong and exhibiting a rather flat decrement. These same emission lines also exhibit a narrow absorption line within the emission profiles, indicating an outflowing circumstellar medium; the H-alpha emission line has a FWHM of 1900 km/s. SN 2009ko (CBET 1998) is a normal type-Ia supernova about a week after maximum light; cross-correlation using SNID indicates that it is most similar to SN 1994M at about 8 days after maximum.
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