VizieR Online Data Catalog: UV-Opt light curves of the type Ic SN 2018gep (Ho+, 2019)

ZTF18abukavn was discovered in an image obtained at UT 2018 September 9 03:55:18 (start of exposure) as part of the ZTF extragalactic high-cadence partnership survey (Ho+ 2018ATel12030....1H).

We triggered ultraviolet (UV) and optical observations with the UV/Optical Telescope (UVOT) aboard the Neil Gehrels Swift Observatory, and observations began 10.2hr after the ZTF discovery. From Δt~1day to Δt~60days, we conducted a photometric follow-up campaign at UV and optical wavelengths using Swift/UVOT, the Spectral Energy Distribution Machine (SEDM) mounted on the automated 60 inch telescope at Palomar (P60), the optical imager (IO:O) on the Liverpool Telescope (LT), and the Lulin 1m Telescope (LOT).

The first spectrum was taken 0.7 day after discovery by the Spectrograph for the Rapid Acquisition of Transients (SPRAT) on the LT. Twenty-three optical spectra were obtained from Δt=0.7-61.1days using SPRAT, the Andalusia Faint Object Spectrograph and Camera (ALFOSC) on the Nordic Optical Telescope (NOT), the Double Spectrograph (DBSP) on the 200 inch Hale telescope at Palomar Observatory, the Low Resolution Imaging Spectrometer (LRIS) on the Keck I 10m telescope, and the Xinglong 2.16m telescope (XLT+BFOSC) of NAOC, China. Swift obtained three UV-grism spectra between UT 2018 September 15 3:29 and 6:58 (Δt~6.4days) for a total exposure time of 3918s.

We observed the field of SN2018gep with the Karl G. Jansky Very Large Array (VLA) on three epochs: on 2018 September 14 UT under the Program ID VLA/18A-242 (PI: D. Perley; Ho+ 2018ATel12056....1H), and on 2018 September 25 and 2018 November 23 UT under the Program ID VLA/18A-176 (PI: A. Corsi). The source was detected in the first two epochs, but not in the third. We also obtained three epochs of observations with the AMI large array (AMI-LA), on UT 2018 September 12, 2018 September 23, and 2018 October 20. All three observations resulted in null detections with 3σ upper limits. Finally, we observed at higher frequencies using the Submillimeter Array (SMA) on UT 2018 September 15 under its target-of-opportunity program. The project ID was 2018A-S068. See Section 2.5.

We observed the position of SN2018gep with Swift/XRT from Δt~0.4-14days. The source was not detected in any epoch. We obtained two epochs of observations with the Advanced CCD Imaging Spectrometer on the Chandra X-ray Observatory via our approved program (Proposal No. 19500451; PI: Corsi). The first epoch began at 9:25 UTC on 2018 10 October (Δt~15days) under ObsId 20319 (integration time 12.2ks), and the second began at 21:31 UTC on 2018 December 4 (Δt~70days) under ObsId 20320 (integration time 12.1ks). No X-ray emission is detected at the location of SN2018gep in either epoch. See Section 2.6.

(2 data files).