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Spectroscopic Classifications of SN 2018pv

ATel #11278; M. Yamanaka, M. Kawabata, T. Nakaoka, and R. Huang (Hiroshima Univ.)
on 8 Feb 2018; 19:02 UT
Distributed as an Instant Email Notice Supernovae
Credential Certification: Masayuki Yamanaka (masyamanaka@hiroshima-u.ac.jp)

Subjects: Optical, Supernovae

We performed the spectroscopic observations of SN 2018pv using the 1.5-m Kanata telescope attached with the Hiroshima One-shot Wide-field Polarimeter (HOWPol; Kawabata et al. 2008) on Feb 8.7. This SN was discovered at 15.1 mag on Feb. 3 by the amateur astronomer M. Tsuboi, Hiroshima, Japan. The spectrum resembles with that of a normal Type Ia supernova (SN Ia) at the pre-maximum stage. Using the automatic SN classification tool, GELATO (Harutyunyan et al., 2008, A&A, 488, 383), the spectrum would be similar to that of SN 1992A at the 5 days before maximum. We identified the absorption lines of the CaII IR triplet, OI 7774, SiII 6355, SiII 5972, SII W-shape feature, and Fe II multiplet in our spectrum. The CaII IR triplet, OI 7774, and SiII 6355 line velocities were measured to be ~16500, ~16500, and ~13000 km/s, respectively. The SiII 5972 absorption line was significantly deeper than that of SN 1992A, suggesting that this SN might be a more subluminous event. We measured the equivalent width (EW) of the NaID line as to 0.9 angstrom, suggesting that the host galactic extinction could be very large (A_V~0.5-2.0). Even if the extinction is corrected for, this SN could be still in the rising phase. Follow-up observations could be encouraged.