Electronic Telegram No. 3139
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 2012cq IN UGC 4792
     Tomoki Morokuma, Institute of Astronomy, University of Tokyo; Nozomu
Tominaga and Kensho Mori, Konan University; Masaomi Tanaka and Nobuharu Ukita,
National Astronomical Observatory of Japan; Shigeyuki Sako, Noriyuki Matsunaga,
Mamoru Doi, Naoto Kobayashi, Takashi Miyata, Nobuyuki Ienaka, Yoshikazu Nakada,
Tsutomu Aoki, Takao Soyano, Kenichi Tarusawa, and Hiroyuki Mito, Institute of
Astronomy, University of Tokyo; Michael W. Richmond, Rochester Institute of
Technology; Yuji Urata, National Central University; and Ryosuke Itoh, Koji S.
Kawabata, Katsutoshi Takaki, Issei Ueno, and Hiroshi Akitaya, Hiroshima
University, report the discovery of an apparent supernova (magnitude 18.2) on
two g-band CCD images (limiting mag 20.5) taken on May 13.52 and 13.56 UT with
the Kiso Wide-Field Camera (field-of-view 2.1 deg x 2.1 deg) on the 1.05-m
Schmidt telescope at Kiso Observatory, in the course of the Kiso Supernova
Survey project.  The new object is located at R.A. = 9h08m05s.46, Decl. =
+20d30'12".5 (equinox 2000.0), which 0".1 south and 4".8 west of the presumed
host galaxy (SDSS J090805.78+203012.6, at z = 0.0256).  Nothing was detected
at this position on reference images taken before Apr. 28 (limiting mag 20.2).
The variable was also detected after discovery with the Lulin 1-m telescope
in Taiwan and the 1.5-m Kanata telescope (+ HOWPol) at Higashi-Hiroshima
Observatory; its g-band magnitude was measured to be 18.1 on May 14.54 and
16.46.  The discovery image is available at the following website URL:
http://www.ioa.s.u-tokyo.ac.jp/kisohp/KISS/images/iauc_J090805.46+203012.5.jpg.

     E. S. Walker, Scuola Normale Superiore (SNS), Pisa; P. A. Mazzali,
Max-Planck-Institut fuer Astrophysik, Garching, and Istituto Nazionale di
Astrofisica (INAF), Padova; E. Pian, SNS, Pisa, and INAF, Trieste; Masaomi
Tanaka, National Astronomical Observatory of Japan; Tomoki Morokuma, Institute
of Astronomy, University of Tokyo; and Nozomu Tominaga and Kensho Mori, Konan
University, report that they obtained a CCD spectrogram (range 350-800 nm) of
2012cq using the DOLORES spectrograph on the Telescopio Nazionale di Galileo
situated on La Palma on May 24.9 UT.  The spectrum shows a series of hydrogen
Balmer features, implying that 2012cq is a type-II supernova.  The hydrogen
features show strong emission components.  SN 2012cq is situated in the galaxy
UGC 4792 and shows a redshift of lines consisted with the redshift of the host
galaxy (z = 0.0256, from Giovanelli et al. 1997, A.J. 114, 122; via the NED
database).  Using the publically available GELATO code (Harutyuyan et al.
2008, A.Ap. 488, 383), 2012cq is most similar to the type-IIn supernova 1998S
at fourteen days after maximum light; this phase after maximum is consistent
with ongoing photometry measurements that show the supernova to be getting
dimmer.


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

                         (C) Copyright 2012 CBAT
2012 June 13                     (CBET 3139)              Daniel W. E. Green