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Spectroscopic Classifications of Optical Transients with Keck II/DEIMOS

ATel #8073; R. J. Foley, Y.-C. Pan (Illinois), A. Rest (STScI), S. W. Jha (Rutgers), D. Scolnic (Chicago/KICP), K. W. Smith, D. Wright, S. J. Smartt (QUB), M. Huber, K. C. Chambers, H. Flewelling, M. Willman, N. Primak, A. Schultz, B. Gibson, E. Magnier, C. Waters, J. Tonry, R. J. Wainscoat (IfA, Hawaii)
on 19 Sep 2015; 17:23 UT
Credential Certification: Ryan Foley (rfoley@illinois.edu)

Subjects: Optical, Star, Supernovae

We report the following classifications of optical transients from spectroscopic observations with the DEIMOS spectrograph (wavelength range 4500 - 9700 A) on the Keck II telescope. Targets were supplied by the Pan-STARRS Survey for Transients (PSST), All-Sky Automated Survey for Supernovae (ASAS-SN), Ken'ichi Nishimura, and the Puckett Supernova Search Team. All observations were made on 2015 Sep 19 UT. Classifications were performed with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024).

 
Name    | RA (J2000)  | Dec (J2000) |  z   | Type | Phase |  Notes
ASASSN-15pe | 17:20:15.35 | +39:15:39.4 | 0.038 | Ia | +14 | (1) ASASSN-15pn | 04:03:26.32 | -05:29:31.3 | 0.038 | Ia | +2 | (2) ASASSN-15pr | 23:06:39.50 | -12:34:22.4 | 0.034 | Ia | -3 | (3) PS15bvr | 20:56:32.93 | -19:22:11.7 | 0.14 | Ia | 0 | (4) PS15cbt | 01:12:35.91 | +14:00:42.7 | 0.053 | ? | | (5) PS15cby | 01:51:39.06 | +12:26:39.1 | 0.136 | II | +7 | PSNJ16495254+5532345 | 16:49:52.54 | +55:32:34.5 | 0 | Star | | (6) PSNJ22343424+0548478 | 22:34:34.24 | +05:48:47.8 | 0.028 | II | +2 |
Notes: (1) See also ATEL #8072. (2) We measure a Si II 6355 velocity of -10,500 km/s. See also ATEL #8072. (3) We measure a Si II 6355 velocity of -13,300 km/s. See also ATEL #8072. (4) We measure a Si II 6355 velocity of -10,500 km/s. (5) Although we detect SN "wiggles," the spectrum is not high enough S/N for a clear classification. (6) Blue continuum and Balmer absorption at -51 +/- 2 km/s. Likely a foreground star (possibly flaring) coincident with galaxy. When the redshift is given to 2 decimal places, it is derived from the SN spectrum. Otherwise, the redshift is determined from the host galaxy.