[IAUC] CBET 3666: 20131003 : SUPERNOVA 2013fr IN MCG +04-10-24 = PSN J04080235+2317394

[quai en eps.harvard.edu]

                                                  Electronic Telegram No. 3666
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 en eps.harvard.edu (alternate cbat en iau.org)
URL http://www.cbat.eps.harvard.edu/index.html
Prepared using the Tamkin Foundation Computer Network


SUPERNOVA 2013fr IN MCG +04-10-24 = PSN J04080235+2317394
     S. Howerton, Arkansas City, KS, U.S.A.; A. J. Drake, S. G. Djorgovski,
A. Mahabal, M. J. Graham, and R. Williams, California Institute of Technology;
J. L. Prieto, Princeton University; M. Catelan, Pontificia Universidad
Catolica de Chile; and E. Christensen and S. M. Larson, Lunar and Planetary
Laboratory, University of Arizona, report the Catalina Real-time Transient
Survey discovery of an apparent supernova in public images from the Catalina
Sky Survey (CSS).

 SN       2013 UT       R.A. (2000.0) Decl.       Mag.      Offset
 2013fr   Sep. 28.42   4 08 02.35  +23 17 39.4   16.2    4".6 W, 4".9 N

The variable was designated PSN J04080235+2317394 when it was posted at the
Central Bureau's TOCP webpage and is here designated SN 2013fr based on the
spectroscopic confirmation reported below.  Additional CCD magnitudes for
2013fr:  Sept. 1.42 UT, [20.0 (CSS); Sept. 29.718, 16.3 (Joseph Brimacombe,
Cairns, Australia; 41-cm RCOS telescope and STL6K camera + infrared filter;
bandpass > 700 nm; position end figures 02s.41, 38".8; image posted at website
URL http://www.flickr.com/photos/43846774@N02/10010606686/).

     P. Challis, R. Kirshner, and K. Mandel, Harvard-Smithsonian Center for
Astrophysics (CfA), on behalf of the CfA Supernova Group, report that a
spectrogram (range 340-740 nm) of PSN J04080235+2317394 = SN 2013fr was
obtained on Sept. 29 UT by K. Rines with the F. L. Whipple Observatory 1.5-m
telescope (+ FAST).  Cross-correlation with a library of supernova spectra
using the "Supernova Identification" code (SNID; Blondin and Tonry 2007, Ap.J.
666, 1024) shows that the best fit for 2013fr is a type-IIn supernova at a
phase of about a week after explosion.


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      superseded by text appearing later in the printed IAU Circulars.

                         (C) Copyright 2013 CBAT
2013 October 3                   (CBET 3666)              Daniel W. E. Green