Electronic Telegram No. 3100
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 2012bz = GRB 120422A
[Editor's note:  this replaces the text on CBET 3098 (authors list).]
     D. Malesani, DARK Cosmology Centre, Niels Bohr Institute, University of
Copenhagen; S. Schulze, University of Iceland; T. Kruehler, J. P. U. Fynbo, J.
Hjorth, B. Milvang-Jensen, and D. Watson, DARK Cosmology Centre, Niels Bohr
Institute, University of Copenhagen; A. de Ugarte Postigo, Instituto de
Astrofisica de Andalucia and Dark Cosmology Centre, Niels Bohr Institute,
University of Copenhagen; N. R. Tanvir, University of Leicester; G.
Tagliaferri, Osservatorio Astronomico di Brera; J. Sollerman, Oskar Klein
Centre, Stockholm University; D. Xu, Weizmann institute, Israel; M. D.
Stritzinger, Institute of Physics and Astronomy, Aarhus University; and A. De
Cia, University of Iceland, on behalf of the X-shooter GRB "guaranteed time
observation" collaboration, report on monitoring the afterglow of the
gamma-ray burst GRB 120422A (located at R.A. = 9h07m38s.38, Decl. =
+14d01'07".5, equinox 2000.0; Troja et al., GCN 13243, accessible at website
URL http://gcn.gsfc.nasa.gov/gcn3/13243.gcn3; position and magnitude i = 19.0
via the Gemini-North 8-m telescope on Apr. 22.3 UT from Cucchiara et al., GCN
13245) with the Nordic Optical Telescope (NOT) since the burst.  Imaging that
was secured in the i-band, with the NOT on Apr. 30.90 showed that the
afterglow was found to have re-brightened (to i = 21.3, from i = 22.1 five
days earlier; Malesani et al., GCN 13275).  Subsequent spectroscopy was
secured with the X-shooter spectrograph starting on May 1.0 (8.7 days after
the GRB), for a total exposure time of 80 min in each of the UVB, VIS, and NIR
arms, covering the wavelength range 300-2500 nm.  The slit was aligned to cover
both the galaxy at z = 0.28 (as visible in the Sloan Digital Sky Survey;
Cucchiara et al., GCN 13245; Tanvir et al., GCN 13251) and the optical
counterpart (Cucchiara et al., GCN 13245).  The spectrum exibits a broad
emission peak centred at 630 nm, similar to what was found in a Keck-telescope
spectrum taken on Apr. 27 (Perley et al., GCN 13267).  Blueward of the peak,
the spectrum drops steeply down to around 400 nm, and beyond that there is no
detection of flux.  Comparison with a library of supernova spectra using the
"Supernova Identification" tool (SNID; Blondin and Tonry 2007, Ap.J., 666,
1024) gives good matches with both type-Ib and type-Ic supernovae at about a
week before maximum.


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

                         (C) Copyright 2012 CBAT
2012 May 2                       (CBET 3100)              Daniel W. E. Green