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PESSTO spectroscopic classification of optical transients

ATel #9597; C. Frohmaier (Southampton), S. Prajs (Southampton), G. Dimitriadis (Southampton), R. Cartier (Southampton), J. Anderson (ESO), K. Maguire (QUB), C. Inserra (QUB), E. Kankare (QUB), S. J. Smartt (QUB), K. W. Smith (QUB), M. Sullivan (Southampton), S. Valenti (UC Davis), O. Yaron (Weizmann), D. Young (QUB), I. Manulis (Weizmann), J. Tonry, B. Stalder, L. Denneau., A. Heinze, A. Sherstyuk, K. Chambers, H. Flewelling, M. Huber, E. Magnier, C. Waters, R. J. Wainscoat (IfA, Univ. of Hawaii), A. Rest (STScI), and L. Wyrzykowski (Warsaw Observatory, Poland).
on 5 Oct 2016; 18:08 UT
Distributed as an Instant Email Notice Supernovae
Credential Certification: Regis Cartier (rgcartier@gmail.com)

Subjects: Optical, Supernovae

PESSTO, the Public ESO Spectroscopic Survey for Transient Objects (see Smartt et al. 2015, A&A, 579, 40 http://www.pessto.org ), reports the following supernova classifications. Targets were supplied by the ATLAS survey, see Tonry et al. (2011, PASP, 123, 58) and Tonry et al. (ATel #8680), and by OGLE-IV Real-time Transient Search (Wyrzykowski et al., 2014 arxiv:1409.1095; http://ogle.astrouw.edu.pl/ ). We acknowledge ESA Gaia, DPAC and the Photometric Science Alert Team (http://gsaweb.ast.cam.ac.uk/alerts). ASASSN-16lc is from the All Sky Automated Survey for SuperNovae ASAS-SN (see Shappee et al. 2014, ApJ, 788, 48 and http://www.astronomy.ohio-state.edu/~assassin/index.shtml ). All observations were performed on the ESO New Technology Telescope at La Silla on 2016 October 2nd, 3rd, and 4th using EFOSC2 and Grism 13 (3985-9315A, 18A resolution). Classifications were done with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024). Classification spectra and additional details can be obtained from http://www.pessto.org (via WISeREP) and the IAU Transient Name Server.

 
Survey Name | IAU Name  | RA (J2000)  | Dec (J2000) | Disc. Date | Source | Disc Mag |  z    | Type    | Phase    | Notes 
            | SN2016grk | 21:19:41.31 | +21:57:56.3 | 20160930   | POSS   | 18.70    | 0.018 | II      | at max   | (1) 
ATLAS16czo  | AT2016gsi | 19:42:40.93 | -26:05:48.3 | 20160928   | ATLAS  | 16.76    |       | Star    |          | (2) 
ASASSN-16lc | SN2016gtr | 19:29:01.20 | -51:58:13.8 | 20160930   | ASASSN | 16.00    | 0.014 | Ia      | at max   | 
SMT16yox    |           | 22:36:40.82 | -06:14:28.5 | 20160827   |        | 20.44    | 0.075 | II      | at max   | 
MASTERJ0134 |           | 01:34:15.04 | -17:48:43.4 | 20160924   | MASTER | 17.50    | 0.046 | Ia      | at max   | 
OGLE16ead   |           | 02:19:21.79 | -64:05:26.3 | 20160923   | OGLE   | 20.98    | 0.076 | Ia      | -7 to -4 | (3) 
            | SN2016gqv | 04:02:48.52 | +01:58:15.6 | 20160928   |        | 19.50    | 0.012 | Ic      | > +20    | (4) 
OGLE16bsy   |           | 00:34:55.34 | -66:26:31.7 | 20160718   | OGLE   | 20.77    | 0.145 | IIn     | at max   |  
PS16elh     |           | 02:05:14.93 | -04:48:51.6 | 20160925   | PS1    |          | 0.161 | unknown |          | (5) 
Gaia16bkr   | SN2016guu | 23:54:57.92 | -63:27:13.3 | 20160930   | Gaia   | 18.31    | 0.07  | Ia      | +4 to +7 | 
PTSS-16ppi  | AT2016gvg | 03:13:12.85 | +02:08:37.5 | 20161003   | PTSS   | 17.90    | 0.048 | Ia      | +4 to +7 | 
Gaia16bjk   | AT2016gkq | 21:35:37.96 | -36:46:34.8 | 20160920   | Gaia   | 18.99    | 0.58  | QSO     |          | (6) 

(1) Similar to SN 1979C showing weak Halpha, redshift consistent with the galaxy UGC 11722 (z=0.016525) close to the SN position.
(2) Shows blue continuum and the Balmer series at zero redshift in absorption, very weak Halpha.
(3) Similar to SN 1991T.
(4) Very red spectrum, SNID yields best match to SN 2004aw. Redshift consistent with the galaxy UGC 02936 (z=0.013) close to the SN position.
(5) Faint transient with strong galaxy contamination. Transient is likely blue, no strong SN features and it appears to be at the same position of SN2006as (within 0.5 arcsec) which was classified as a type II by Leibundgut et al. 2006, CBET 772 (at z=0.23). Further work is needed to determine if they are physically associated.
(6) Shows broad Mg II and Hbeta lines, and narrow [O III] 5007 line.