PESSTO spectroscopic classification of optical transients

ATel #6399; N. Elias-Rosa, L. Tartaglia (INAF-Padova), L. Tomasella (INAF-Padova), A. Morales-Garoffolo (ICE-CSIC/IEEC), A. Pastorello (INAF-Padova), M. T. Botticella (INAF-OAC), C. Inserra (QUB), K. Maguire (ESO), S. Smartt (QUB), K. W. Smith (QUB), M. Sullivan (Southampton University), S. Valenti (LCOGT), O. Yaron (Weizmann), D. Young (QUB), I. Manulis (Weizmann), C. Baltay, N. Ellman, E. Hadjiyska, R. McKinnon, D. Rabinowitz, S. Rostami, E. S. Walker (Yale University), U. Feindt, M. Kowalski (Universitat Bonn), P. Nugent (LBL Berkeley), L. Wyrzykowski (Warsaw Observatory, Poland)
on 17 Aug 2014; 17:08 UT
Credential Certification: Lina Tomasella (lina.tomasella@oapd.inaf.it)

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PESSTO, the Public ESO Spectroscopic Survey for Transient Objects (see Valenti et al., ATel #4037; http://www.pessto.org ), reports the following supernova classifications. Targets were supplied by the La Silla-Quest (see Baltay et al., PASP, 2013, 125, 683), the ASAS-SN (http://www.astronomy.ohio-state.edu/~assassin/index.shtml) and the OGLE (http://ogle.astrouw.edu.pl/ogle4/transients/transients.html) surveys. All observations were performed on the ESO New Technology Telescope at La Silla in the night starting on 2014 Aug 16 UT, 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). Spectra can be obtained from http://www.pessto.org (via WISeREP).

 
 Name                         | RA (J2000)  | Dec (J2000) | Disc. Date  | Disc. Source       | Disc Mag  |  z   | Type  | Phase | Notes
 
 ASASSN-14fo                  | 20:34:06.43 | -01:58:03.5 | 20140816    | ASASSN             |   15.8    | 0.02 |  Ia   | +2d   |  
 LSQ14drn                     | 20:39:04.63 | -61:10:27.0 | 20140724    | LSQ                |   18.5    | 0.07 |  Ia   | +14d  |  
 LSQ14drx                     | 21:47:10.18 | -49:36:53.7 | 20140726    | LSQ                |   17.0    | 0.07 |  IIn  | +34d  | (1)  
 LSQ14dsj                     | 21:53:25.57 | -19:21:07.3 | 20140710    | LSQ                |   18.1    | --   | M-star| --    | (2) 
 LSQ14dss                     | 23:02:57.76 | -55:57:03.0 | 20140726    | LSQ                |   19.1    | --   |  CV   | --    | (3) 
 LSQ14dud                     | 22:25:06.94 | +00:31:49.4 | 20140713    | LSQ                |   19.0    | 0.11 |  Ia   | +8d   | (4) 
 LSQ14dvq                     | 21:03:10.63 | -60:30:28.9 | 20140724    | LSQ                |   18.5    | --   |  CV   | --    | (5) 
 LSQ14dvx                     | 20:38:43.63 | -41:08:53.8 | 20140724    | LSQ                |   19.8    | 0.05 |  II   | +15d  | (6) 
 LSQ14dxa                     | 22:08:39.89 | -56:09:24.9 | 20140724    | LSQ                |   19.2    | 0.04 |  Ia   | +90d  | 
 LSQ14ecb                     | 21:53:41.32 | -13:17:27.4 | 20140725    | LSQ                |   18.9    | 0.05 |  Ia   | +18d  | 
 LSQ14edn                     | 21:58:10.26 | -44:55:41.6 | 20140801    | LSQ                |   20.2    | 0.11 |  Ia   | +1d   | 
 LSQ14eer                     | 22:48:14.65 | +07:10:06.5 | 20140802    | LSQ                |   19.4    | 0.03 |  II   | max   | (7) 
 OGLE-2014-SN-046             | 01:09:06.73 | -74:30:46.4 | 20140703    | OGLE               |   18.9    | 0.04 |  IIP  | +50d  | (8) 
 

(1) Best match with Type-IIn SNe, in particular with SN 2010jl.
(2) Spectrum of Galactic late-type dwarf.
(3) The spectrum reveals Balmer and possible HeI 6678 Ang emission lines superimposed on a normal accretion disk continuum and absorption troughs underlying the Balmer emissions, which are a general feature of a dwarf nova in the decline of an eruption (Liu et al. 1999, ApJS 122, 243).
(4) Best match with the peculiar Ia SN 2006gz.
(5) The spectrum reveals Balmer, HeI and HeII 4686 Ang sharp emissions, at rest wavelength, onto a blue continuum, characteristic of CVs (cf Liu et al. 1999, ApJS 122, 243; Liu et al. 1999, ApJS 122, 257).
(6) Noisy spectrum with broad P-Cygni H.
(7) The spectrum is characterised by a very blue continuum, essentially featureless, with no absorption bands and no detectable emission lines, resembling a black-body energy distribution. This is compatible with a very young type-II supernova; further observations are required to better classify it.
(8) Spectrum has broad P-Cygni H and metal lines in the blue. The photometry from LSQ allows us to classify it as a Type-IIP.

PESSTO, the Public ESO Spectroscopic Survey for Transient Objects