[IAUC] CBET 4168: 20151115 : SUPERNOVA 2015W IN UGC 3617 = PSN J06574303+1334457

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                                                  Electronic Telegram No. 4168
Central Bureau for Astronomical Telegrams
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SUPERNOVA 2015W IN UGC 3617 = PSN J06574303+1334457
     Further to CBET 4026, H. Kim, W. Zheng, and A. V. Filippenko, University
of California at Berkeley, report the LOSS discovery of a supernova in UGC
3617 on unfiltered KAIT images:

 SN      2015 UT       R.A. (2000.0) Decl.      Mag.      Offset
 2015W   Jan. 12.276  6 57 43.03  +13 34 45.7   16.8    31".5 W, 15".0 N

A finding chart was posted by the discoverers at the following website URL:
http://astro.berkeley.edu/~zwk/findingchart/PSN_J06574303+13344573.jpg.  The
variable was designated PSN J06574303+1334457 when it was posted at the
Central Bureau's TOCP webpage and is here designated SN 2015W based on the
spectroscopic confirmation reported below.  Additional CCD magnitudes for
2015W:  2014 Dec. 14, [18.5 (KAIT); 2015 Jan. 13.31 UT, 16.8 (KAIT); 13.800,
16.8 (G. Masi and P. Catalano; remotely using a 43-cm telescope at Ceccano,
Italy; position end figures 43s.04, 45".7); 16.346, 17.1 (J. Brimacombe,
Cairns, Australia; remotely using a 51-cm RCOS telescope + STXL-6303 camera
at the New Mexico Skies observatory near Mayhill, NM, USA; position end
figures 43s.05, 45".7); 18.201, 17.1 (Brimacombe; position end figures
43s.05, 45".7).  Brimacombe posted his images at the following website URL:
https://www.flickr.com/photos/43846774@N02/16384233825/.

     W. Zheng, J. Mauerhan, H. Yuk, K. I. Clubb, and A. V. Filippenko,
University of California, Berkeley, report that a CCD spectrogram (range
350-1000 nm) of PSN J06574303+1334457 = SN 2015W was obtained on Jan. 28.212
UT with the Shane 3-m reflector (+ Kast spectrograph) at Lick Observatory.
The spectrum shows that 2015W is a type-IIP supernova at the redshift (z =
0.013) of the host galaxy, UGC 3617.  Cross-correlation with a library of
supernova spectra using the "SuperNova Identification" code (SNID; Blondin
and Tonry 2007, Ap.J. 666, 1024) indicates a similarity with several type-IIP
supernovae about 3 weeks after maximum brightness.


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                         (C) Copyright 2015 CBAT
2015 November 15                 (CBET 4168)              Daniel W. E. Green