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ePESSTO spectroscopic classification of optical transients

ATel #10950; F. Onori (SRON/RU), G. Cannizzaro (SRON/RU), Z. Kostrzewa-Rutkowska (SRON/RU), P. G. Jonker (SRON/RU), A. De Cia (ESO), J. Lyman (Warwick), C. Inserra (Southampton), E. Kankare (QUB), K. Maguire (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, H. Weiland (IfA, Univ. of Hawaii), A. Rest (STScI).
on 11 Nov 2017; 12:50 UT
Distributed as an Instant Email Notice Supernovae
Credential Certification: P.G. Jonker (p.jonker@sron.nl)

Subjects: Optical, Supernovae, Transient

Referred to by ATel #: 11013

ePESSTO, the extended 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 the ESA Gaia Photometric Science Alerts Team and DPAC (http://gsaweb.ast.cam.ac.uk/alerts). All observations were performed on the ESO New Technology Telescope at La Silla on 2017, Nov. 10, using EFOSC2 and Grism 13 (3985-9315A, 18A resolution) and Grism 11 (3380-7520A, 16A resolution). Classifications were done with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024) and GELATO (Harutyunyan et al., 2008, A&A, 488, 383). 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 
Gaia16ate   | AT2016eei | 03 04 19.7 | -57 35 01.8 |  20160617  | Gaia   |   18.14  | 0.06  |  SN Type IIn    |       | (1) 
ATLAS17mzy  | 	        | 03 44 12.5 | -26 35 56.5 |  20171001  | ATLAS  |   20.40  | 0.067 |  ?    |       | (2) 
ATLAS17mrm  | AT2017hof | 04 09 16.9 | -20 41 58.8 |  20171024  | ATLAS  |   21.21  | 0.055 |  SN Type Ia ?   |       | (3) 

(1) Redshift estimated from narrow Balmer emission lines.
(2) Redshift from the putative host. Blue featureless continuum.
(1) Redshift from SNID.