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Spectroscopic Classification of Five Optical Transients

ATel #12478; S. Gomez, P. Blanchard, G. Hosseinzadeh, E. Berger (Harvard/CfA), M. Nicholl (ROE, Edinburgh)
on 6 Feb 2019; 18:43 UT
Distributed as an Instant Email Notice Supernovae
Credential Certification: Sebastian Gomez (sgomez@cfa.harvard.edu)

Subjects: Optical, AGN, Supernovae, Transient

We obtained optical spectroscopic observations of four transients discovered by the Pan-STARRS Survey for Transients (PSST; Huber et al., ATel #7153), the Asteroid Terrestrial-impact Last Alert System (ATLAS; Tonry et al. 2011; ATel #8680), and the Zwicky Transient Facility (ZTF; Bellm & Kulkarni 2017; ATel #11266). For all observations, we used the IMACS Spectrograph (Dressler et al. PASP 123, 288) mounted on the Magellan Baade 6.5-m Telescope with a spectral coverage of 4000-9500 Angstroms. The classifications, shown below, were determined by cross-correlating spectra of known supernovae using SNID (Blondin & Tonry, 2007, ApJ, 666, 1024) and Superfit (Howell et al. 2005, ApJ, 634, 1190). The redshifts and spectral phase listed below are inferred from the best fitting templates unless otherwise specified. The spectra are available on the Transient Name Server. We thank Yuri Beletsky for carrying out the observations.

  
|      Nam     |  RA (J2000) |  DEC (J2000) | Disc. Date | Disc. mag   | Redshift | Class  | Spectral Phase | Obs. date  | 
|--------------|-------------|--------------|------------|-------------|----------|--------|----------------|------------| 
| SN2018lfe*   | 09:33:29.56 | +00:03:08.39 | 2018-12-31 | 19.7 (w)    | 0.350    | SLSN-I | ~ 45 days      | 2019-01-30 | 
| SN2019sw     | 09:57:18.91 | +04:35:07.50 | 2019-01-11 | 19.8 (cyan) | 0.12     | SN Ia  | ~ 14 days      | 2019-01-30 | 
| SN2019go     | 08:25:09.27 | +19:10:14.74 | 2019-01-03 | 19.6 (g)    | 0.10     | SN Ia  | ~ 23 days      | 2019-01-30 | 
| ZTF19aaapoxs | 11:49:18.69 | -04:16:50.30 | 2019-01-04 | 18.7 (r)    | 0.085    | AGN    |                | 2019-01-30 | 
* redshift determined from host emission lines, and spectral phase consistent with ZTF light curve, where the brightest absolute magnitude corresponds to -22.