Electronic Telegram No. 2997 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION CBAT Director: Daniel W. E. Green; Hoffman Lab 209; Harvard University; 20 Oxford St.; Cambridge, MA 02138; U.S.A. e-mail: cbatiau@eps.harvard.edu (alternate cbat@iau.org) URL http://www.cbat.eps.harvard.edu/index.html Prepared using the Tamkin Foundation Computer Network SUPERNOVA 2011kb = PSN J07211428-6205308 L. A. G. Monard, Calitzdorp, Western Cape, South Africa, reports his discovery of an apparent supernova (mag 16.8) on several unfiltered CCD images taken on 2011 Dec. 16.026 UT. The new object is located at R.A. = 7h21m14s.28, Decl. = -62d05'30".8 (equinox 2000.0), which is 8" east and 4" north of the core of the presumed host galaxy. The variable was designated PSN J07211428-6205308 when it was posted at the Central Bureau's TOCP webpage and is here designated SN 2011kb based on the spectroscopic confirmation reported below. Additional CCD magnitudes for 2011kb (unfiltered unless noted otherwise): 2011 May 30.72, [18.5 (Monard); Oct 8.108, 16.1 (Monard); Nov. 7.163, 16.1 (Monard); 25.956, 16.4 (Monard); Dec. 16.026, 16.8 (Monard); 28.984, 18.2 (Monard); 29.914, 18.1 (Monard); 31.720, 17.0 (Joseph Brimacombe, Cairns, Australia; 41-cm RCOS telescope + STL6K camera + infrared filter; range > 700 nm; position end figures 14s.34, 31".2; image posted at website URL http://www.flickr.com/photos/43846774@N02/6610070865/); 2012 Jan. 5.667, 16.9 (Brimacombe; position end figures 14s.23, 31".5; image posted at website URL http://www.flickr.com/photos/43846774@N02/6729145569/). N. Morrell, Las Campanas Observatory, on behalf of the Carnegie Supernova Project, reports that optical spectroscopy (range 430-1000 nm), obtained on 2012 Jan. 16 UT with the 6.5-m Magellan I (Baade) telescope (+ IMACS), shows that PSN J07211428-6205308 = SN 2011kb is a type-II supernova several months after explosion. SNID suggests for 2011kb a redshift of 0.010 (similar to the neighboring galaxy NGC 2369B) and gives good matches with a variety of type-II supernovae between 4 and 6 months after maximum brightness. Combining this information with the discovery date, it is possible to infer that the best reliable match is with the type-II-P supernova 2004et at 147 days after maximum light. NOTE: These 'Central Bureau Electronic Telegrams' are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2012 CBAT 2012 January 26 (CBET 2997) Daniel W. E. Green