PESSTO spectroscopic classification of optical transients
ATel #9357; T. Reynolds (Turku), M. Fraser (IoA, Cambridge), S. Mattila (Turku), T.-W. Chen (MPE), J. Anderson (ESO), C. Inserra (QUB), E. Kankare (QUB), K. Maguire (QUB), I. Manulis (Weizmann), S. J. Smartt (QUB), K. W. Smith (QUB), M. Sullivan (Southampton), S. Valenti (UC Davis), O. Yaron (Weizmann), D. Young (QUB), J. Tonry, B. Stalder, L. Denneau., A. Heinze, A. Sherstyuk (IfA, Univ. of Hawaii), A. Rest (STScI), D. Wright (QUB), K. Chambers, H. Flewelling, M. Huber, E. Magnier, J. Tonry, C. Waters, R. J. Wainscoat (IfA, Univ. Hawaii).
on 9 Aug 2016; 22:46 UT
Distributed as an Instant Email Notice Supernovae
Credential Certification: Morgan Fraser (mf@ast.cam.ac.uk)
Subjects: Optical, Cataclysmic Variable, Supernovae, Transient
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 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 ); Gaia; the Pan-STARRS Survey for Transients (see Huber et al., ATel #7153); and the ATLAS survey, see Tonry et al. (2011, PASP, 123, 58) and Tonry et al. (ATel #8680)". We acknowledge ESA Gaia, DPAC and the Photometric Science Alerts Team (http://gsaweb.ast.cam.ac.uk/alerts). All observations were performed on the ESO New Technology Telescope at La Silla on 2016 August 8, using EFOSC2 and Grism 13 (3985-9315A, 18A 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
PS16dqv | SN2016eub | 00:06:25.24 | -00:17:46.0 | 2016-08-03 | PSST | 20.0 | 0.044 | II | +1m | (1)
Gaia16awg | SN2016eij | 04:03:16.69 | -54:35:49.9 | 2016-07-24 | Gaia | 18.5 | 0.075 | Ia | +14d |
PS16drm | SN2016eui | 00:25:44.75 | -02:57:54.9 | 2016-08-05 | PSST | 19.2 | 0.07 | Ia | +7d |
ASASSN-16in | SN2016eso | 04:59:30.04 | -28:51:39.1 | 2016-08-08 | ASAS-SN | 16.9 | 0.017 | IIn | Young | (2)
Gaia16axm | SN2016emx | 06:04:10.99 | -65:14:40.7 | 2016-07-28 | Gaia | 17.9 | 0.05 | Ia | +3d |
Gaia16axi | SN2016emr | 05:59:58.09 | -18:05:22.3 | 2016-07-30 | Gaia | 17.0 | 0.03 | Ia | +7d |
Gaia16awl | SN2016ejf | 05:01:41.80 | +03:34:28.4 | 2016-07-25 | Gaia | 18.6 | 0.028 | Ibc | +14d |
Gaia16axv | AT2016eqh | 07:02:33.30 | -35:54:43.5 | 2016-08-01 | Gaia | 17.7 | ? | ? | ? | (3)
Gaia16aya | AT2016esi | 07:29:21.49 | -35:58:11.3 | 2016-08-03 | Gaia | 16.4 | - | CV? | - | (4)
(1) Spectrum is best matched by several old (~+1 month) IIb SNe, with weak Halpha emission and well-developed metal lines.
(2) The spectrum is blue, with strong narrow unresolved (<1300 km/s) Balmer lines superimposed.
(3) Blue, featureless continuum. There is a possible weak emission feature at 7100 Ang, if this is associated with Halpha then the redshift of the transient is z=0.08, and it would have a magnitude of -20.
(4) Relatively low S/N spectrum with a blue continuum, there is a weak emission feature consistent with Halpha at z=0
