VizieR Online Data Catalog: Optical and NIR spectra and LCs of SN2016ija (Tartaglia+, 2018)

In this paper we describe the highly obscured, nearby Type II SN DLT16am (SN 2016ija), the first SN discovered by the Distance Less Than 40 (DLT40) Mpc supernova search. DLT16am was discovered on 2016 November 21.19 UT in the nearby galaxy NGC 1532. The goal of DLT40 survey is not to find many SNe, but ~10 nearby SNe per year within ~1day from explosion. Fully operational since late summer 2016, we observe ~300-600 galaxies per night using a PROMPT 0.4m telescope (PROMPT5) at the Cerro Tololo Inter-American Observatory (CTIO), achieving a typical single-epoch depth of r~19-20mag with filterless observations and a 45s integration time. The field of view is 10x10arcmin². See section 2 for further explanations.

The spectral sequence of DLT16am is shown in Figure 3, while the log of the spectroscopic observations in the optical and NIR domains is reported in Table 1. Optical spectra were mainly provided by Public ESO Spectroscopic Survey for Transient Objects (PESSTO) using the ESO 3.58m New Technology Telescope (NTT) with the ESO Faint Object Spectrograph and Camera (v.2, EFOSC2), and the Las Cumbres Observatory network of telescopes, using the 2m Faulkes north and south telescopes with FLOYDS. Early-phase spectra were also provided using the 10m South African Large Telescope (SALT) with the Robert Stobie Spectrograph (RSS), and the 2.56m Nordic Optical Telescope (NOT) with Andalucia Faint Object Spectrograph and Camera (ALFOSC). Most NIR spectra were provided by PESSTO using the NTT with the SOFI spectrograph. Two NIR spectra were obtained using the Gemini NIR Spectrograph (GNIRS) at Gemini North. An NIR spectrum was also obtained using the 6.5m Magellan Baade Telescope with the Folded-port InfraRed Echellette (FIRE). Multi-wavelength (300-2500nm) intermediate resolution spectra were obtained using the ESO Very Large Telescope (VLT) with X-shooter, mounted at the Cassegrain focus of the 8m VLT UT2 telescope.

Photometric data are shown in Figure 4 and reported in Tables 2-4. See section 3 for further explanations.

(5 data files).