VizieR Online Data Catalog: SN 2018agk spectra and NIR-UV light curves (Wang+, 2021)

The Type Ia SN 2018agk was discovered with the CTIO 4m Blanco DECam camera on 2018-March-10 at 07:06:06 UTC (MJD 58188.296).

Throughout this paper, we use the Milky Way extinction of E(B-V)_MW=0.034 from the extinction map as described in Schlafly & Finkbeiner (2011ApJ...737..103S).

We obtained ground-based photometry with the CTIO 4m Blanco telescope with DECam in g and i bands, the Swope 1.0m telescope at Las Campanas Observatory in uBVgri bands, the 60/90cm Schmidt telescope on Piszkesteto Mountain Station of Konkoly Observatory in BVRI bands, the 1.3m telescope at the Cerro Tololo Inter-American Observatory (CTIO) in RIJHK bands, and the PS1 1.8m telescope at Haleakala on Maui, Hawai'i in gri bands. We also include photometric data from the Global Supernova Project taken with Las Cumbres Observatory previously published in Baltay+ (2021PASP..133d4002B).

IC 0855 was included as a Campaign 17 target through "The K2 ExtraGalactic Survey (KEGS) for Transients" (PI Rest) and the "Multi-Observatory Monitoring of K2 Supernovae" (PI Foley) programs as part of the K2 SCE (internal Kepler EPIC ID 228682548). We retrieved the IC 0855 Kepler data through the Mikulski Archive for Space Telescopes (MAST) after the end of K2 Campaign 17. See Section 2.2.

We obtained a total of 17 spectra for SN 2018agk from ground-based observatories: one spectrum with the Gemini Multi-Object Spectrograph (GMOS) on the Gemini-North telescope (GN-2018A-LP-13, PI: Garnavich); four spectra with ESO Faint Object Spectrograph and Camera (EFOSC2) on the ESO New Technology Telescope; one spectrum with the Kast spectrograph (KAST) on the Lick Shane telescope (2018A-S023, PI: Foley); two spectra with the Low-Resolution Imaging Spectrometer (LRIS) on the Keck I telescope (U240, PI: Foley); one spectrum with the Goodman High Throughput Spectrograph at the Southern Astrophysical Research (SOAR) Telescope (2018A-0277, PI: Foley); five optical spectra with the twin FLOYDS spectrographs mounted on Las Cumbres Observatory's 2m Faulkes Telescopes North (FTN) at Haleakala Observatory in Hawai'i and Faulkes Telescopes South (FTS) at Siding Spring Observatory in Australia; and two spectra with the Low Resolution Spectrograph-2 (LRS2) on the 10m Hobby-Eberly Telescope (HET) at McDonald Observatory, where the UV and Orange arms of the Blue Integral Field Unit were applied, resulting in a spectrum between 3640 and 6970Å. We additionally use the publicly available classification spectrum, posted on the Transient Name Server (TNS), obtained with the Wide-Field CCD (WFCCD) of the 2.5m du Pont Telescope at Las Campanas Observatory. See Section 2.3.

We triggered Hubble Space Telescope (HST) follow-up of SN2018agk on 2018 March 16 (GO-15274, PI Garnavich). On the second visit, STIS CCD spectra using the G430L and G750L gratings were obtained, providing wavelength coverage from 170 to 1010nm. See Section 2.4.

This paper also uses data obtained with ANDICAM mounted to the 1.3m telescope at the Cerro Tololo Inter-American Observatory (CTIO) and operated by the SMARTS Consortium under program NOAO-18A-0047 (PI: Galbany).

(5 data files).