Electronic Telegram No. 3894
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 2014bk
     On behalf of the Kiso Supernova Survey (KISS) collaboration, T. Morokuma,
Institute of Astronomy, University of Tokyo; T. Shibata and E. Matsumoto,
Konan University; D. Tsvetkov and N. Pavlyuk, Sternberg Astronomical
Institute, Lomonosov Moscow State University; S. Fukuda, Hiroshima, Japan; N.
Tominaga, Konan University; and M. Tanaka, National Astronomical Observatory
of Japan, report the discovery of an apparent supernova (mag 17.9) on a g-band
CCD image (limiting mag 20.3) taken on May 28.51 UT with the Kiso Wide Field
Camera (KWFC; field-of-view 2.1 deg x 2.1 deg) on the 1.05-m Kiso Schmidt
telescope at the Kiso Observatory.  The new object is located at R.A. =
13h54m02s.42, Decl. = +20d00'24".3 (equinox 2000.0), which is 0".1 east and
0".2 north of the center of the galaxy SDSS J135402.41+200024.0.  Nothing is
seen at this position in an image taken on May 25.50 (limiting mag 20.9).
The object was confirmed in the R band with the 0.7-m telescope at the
Sternberg Astronomical Institute on June 2.83.

     On behalf of the KISS collaboration, M. Stritzinger and E. Hsiao,
Department of Physics and Astronomy, Aarhus University; F. Taddia, Oskar Klein
Centre, Stockholm University; and A. Pastorello, Osservatorio Astronomico di
Padova, INAF, report they obtained a visual-wavelength spectrogram of 2014bk
on June 5.1 UT with the Nordic Optical Telescope (+ Alfosc).  The spectrum
consists of a relatively blue continuum superposed with a number of
conspicuous narrow emission features.  The most prevalent features that are
not associated with nebular emission lines are attributed to He I at 447.1,
501.6, 587.6, and 706.5 nm, all of which display narrow- and intermediate-
width components.  The overall nature of the spectrum suggests that 2014bk is
a type-Ibn supernova with about a week after explosion.  Comparison with
spectra of other type-Ibn supernovae reveals that 2014bk closely resembles
the early-phase spectrum of SN 2000er (Pastorello et al. 2008, MNRAS 389,
113).  Measurements of various nebular emission lines suggest a redshift of
z = 0.0697.


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      superseded by text appearing later in the printed IAU Circulars.

                         (C) Copyright 2014 CBAT
2014 June 14                     (CBET 3894)              Daniel W. E. Green