VizieR Online Data Catalog: UV and optical obs. of type Ic SN 2020oi (Gagliano+, 2022)

We obtained archival HST images of the central region of M100 using the Hubble Legacy Archive and the Mikulski Archive for Space Telescopes (MAST). These observations span nearly three decades. We present a detailed summary of the HST observations in Table 1.

We observed SN 2020oi with the Las Cumbres Observatory Global Telescope Network (LCO) 1m telescopes and LCO imagers from 2020-Jan-8 to Feb-05 in g'r'i' bands. SN 2020oi was also observed with the Nickel 1m telescope at Lick Observatory, Mt Hamilton, California, in BVr'i' bands from 2020-Jan-31 to Aug-08. Observations of SN 2020oi were also obtained with the Thacher 0.7m telescope located at Thacher Observatory, Ojai, California, from 2020-Jan-14 to Dec-21 in griz bands. We further observed SN 2020oi with the Swope 1m telescope at Las Campanas Observatory, Chile, starting on 2020-Jan-21 through Mar-15 in uBVgri bands. In addition to the photometry listed above, we include observations obtained from the forced-photometry service of the Zwicky Transient Facility (ZTF). These data, which began on 2020-Jan-07 (δt=2days) and continued through 2020-Apr-26 (δt=111days), were obtained using the Palomar 48 inch telescope. See Section 2.2.

To obtain ultraviolet (UV) photometry for SN 2020oi, we leverage the extensive observations made of M100 by the Neil Gehrels Swift Observatory. The earliest of these was obtained in 2005-Nov. Observations were collected for SN 2020oi from 2 to 53 days post-explosion. See Section 2.3.

We obtained deep X-ray observations of SN 2020oi with the Advanced CCD imaging spectrometer (ACIS) instrument on board the Chandra X-ray Observatory (CXO) on 2020 February 15 and March 13, 40 and 67 days since explosion, respectively, (PI Stroh, IDs 23140, 23141) under an approved DDT program 21508712. We do not find evidence for statistically significant X-ray emission at the location of the SN in either observations or in the co-added exposure. We note the presence of diffuse soft X-ray emission from the host galaxy at the SN site. See Section 2.4.

We have obtained 12 spectra from δt~3.3 to δt~41days post-explosion. Two spectra were obtained with the Goodman High Throughput Spectrograph at the Southern Astrophysical Research (SOAR) Telescope. Six were obtained with the FLOYDS spectrograph on the Faulkes 2m telescopes of the Las Cumbres Observatory Global Telescope Network (LCOGT), two with the Low-Resolution Imaging Spectrometer (LRIS) on the Keck I telescope, and two with the Kast spectrograph on the 3m Shane telescope at Lick Observatory. See Section 2.5.

(4 data files).