VizieR Online Data Catalog: Follow-up phot. & sp. of SNIa 2020hvf (Jiang+, 2021)

The Tomo-e Gozen camera (Tomo-e), is a wide-field mosaic CMOS sensor imager mounted on the 1.05m Schmidt Telescope at the Kiso Observatory, the University of Tokyo, Japan. The Tomo-e Gozen transient survey was officially launched on 2019 October 1. See Section 2.

SN 2020hvf was discovered by the Asteroid Terrestrial-impact Last Alert System (ATLAS) as a supernova candidate on UT 2020 April 21.38, which was independently discovered by Tomo-e (internally designated as Tomo-e202004aaelb) on UT 2020 April 20.5019 (MJD 58959.5019, ~19.20d before the polynomial-fitted B-band peak epoch). The Tomo-e observation of the SN 2020hvf was continued for 10 days.

We carried out ground-based follow-up observations starting from MJD58963.4, about 3.9d after the Tomo-e discovery with the Seimei 3.8m telescope of Kyoto University and Kanata 1.5m telescope of Hiroshima University. In addition, multiband follow-up observations were performed using several small robotic telescopes from 10 days after the Tomo-e discovery. We used the 35cm telescope DSO-14 located at the Dark Sky Observatory and the 60cm Rapid Response Robotic Telescope (RRRT) located at the Fan Mountain Observatory. In addition we used two 70cm telescopes located at the Sierra Remote Observatory and Spring Brook Observatory which are operated as part of the Thai Robotic Telescope (TRT) network.

The Ultraviolet Optical Telescope (UVOT) installed on the Neil Gehrels Swift Observatory began observing SN 2020hvf on MJD 58961.10, about 1.60d after the Tomo-e discovery. The UVOT observation lasted for about three months (from ~-18 to 60 days after the B-band peak).

SN 2020hvf was spectroscopically identified as an SN Ia by Burke+ (2020TNSCR1105....1B) who took a spectrum of SN 2020hvf by FLOYDS-N installed on the Las Cumbres Observatory 2m telescopes on Haleakala (FTN) on MJD 58961.25, about one day after the ATLAS discovery. In our follow-up observations, a series of spectra of SN 2020hvf have been taken by the Kyoto Okayama Optical Low-dispersion Spectrograph with an integral field unit (KOOLS-IFU; 4000-8900Å, R~500) mounted on the newly built Seimei 3.8m telescope and HOWPol from ~-16 to 208d after the B-band peak.

(4 data files).