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AMI-LA 15.5 GHz Observations of the Nearby Supernova SN2020oi

ATel #13401; Itai Sfaradi (HUJI), David Williams (Oxford), Assaf Horesh (HUJI), Rob Fender (Oxford), Dave Green, David Titterington (MRAO, Cambridge) and Yvette Perrott (VUW)
on 12 Jan 2020; 13:38 UT
Credential Certification: Assaf Horesh (assafh@mail.huji.ac.il)

Subjects: Radio, Supernovae, Transient

Referred to by ATel #: 13448

We observed the field of the nearby Type Ic Supernova SN2020oi (TNS report 58241; ATel #13393; ATel #13391; ATel #13396; ATel #13398; ATel #13400; TNS AstroNote 2020-8; 2020-9; 2020-10) with the Arcminute Microkelvin Imager Large Array (AMI-LA; Zwart et al. 2008; Hickish et al. 2018).

The observation was conducted on the 2020-01-11.13 for 4 hours at a central frequency of 15.5 GHz. The custom pipeline REDUCE_DC (e.g. Perrott et al. 2015) was used to calibrate and flag the data, with 3C286 as the absolute flux calibrator and J1215+1654 as the interleaved phase calibrator.

We detect an unresolved source at the phase center and fitted it with the CASA task IMFIT. The peak flux was ~10 mJy/beam at RA: 12:22:54.972, Dec: +15 49 21.574. Given the large size (~30 arcseconds) of the AMI beam, we can not separate, at this time, the supernova emission from the emission of two previously detected FIRST radio sources, which are located a few arcseconds from the position of SN2020oi. However, given the cataloged flux of the FIRST sources at 1.4 GHz compared to the flux level we detect with AMI, we conclude that a significant fraction of the emission detected by AMI originates from SN2020oi. We continue to monitor the source and are in search of flux variations.

We would like to thank the MRAO staff for carrying out these observations.