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tokens: were done using the software flagcal , developed for automatic flagging and calibration for the GMRT data (Prasad Chengalur 2012 ). The calibrated data were imaged using AIPS task imagr . The flux density and errors are obtained from Gaussian fit to the SN position using the task jmfit . The details of GMRT observations and the flux densities of the SN are presented in Table 1 . The GMRT radio light curves at 1.39, 0.61, and 0.33 GHz spanning ∼10–1136 d post-explosion are shown in Fig. 1 . Figure 1. GMRT light curves of ASASSN-16fp at frequencies 0.325, 0.610, and 1.40 GHz. The days since explosion are calculated assuming the date of explosion as 2016 May 25.9 ( ut ). The inverted triangle denotes 3 σ upper limits. Majority of the error bars in the figure (see Table 1) are smaller than the marker size. Table 1. Details of GMRT observations of ASASSN-16fp. a The age is calculated assuming 2016 May 25.9 ( ut ) as the date of explosion (see Section 1 ). b The errors in the flux density are from the task jmfit . 3.2 JVLA observations We observed ASASSN-16fp with the Karl G. Jansky Very Large Array (JVLA) on 2017 February 17.65, 17.67, and 25.8 (project code 17A-167) spanning a frequency range 2.2–9.7 GHz. The observations were done in the standard continuum mode with a bandwidth of 2 GHz split into 16 spectral windows. We used 3C 286 and 3C 48 as the flux density calibrators, and J2139+143 as the phase calibrator. We also analysed the publicly available archival JVLA data of ASASSN-16fp at five epochs from 2016 June 03.44 ( ut ) to 2016 September 07.15 ( ut ), spanning a frequency range 2–25 GHz. The JVLA observations at each frequency were carried out with a bandwidth of ≈2 GHz split into 16 spectral windows. 3C 286 and 3C 48 were observed for the flux density calibration, and J2139+143 was observed as the phase calibrator. The data analysis was done using standard packages within the Common Astronomy Software Applications package ( casa ; McMullin et al. 2007 ). We split the data into four sub-bands, each of ∼0.5-GHz bandwidth during the data reduction. The details of VLA observations and the flux densities of the SN at various epochs are summarized in Table 2 . We plot the full VLA data set in Fig. 2 . Figure 2. JVLA spectra of ASASSN-16fp on day 8 to 276 d post-explosion spanning a frequency range frequencies ∼2–24 GHz. The days since explosion are calculated assuming the date of explosion as 2016 May 25.9 ( ut ). The error bars in the figure (see Table 2) are smaller than the marker size. Table 2. Details of JVLA observations of ASASSN-16fp. a The age is calculated assuming 2016 May 25.9 ( ut ) as the date of explosion (see Section 1 ). b The errors in the flux density are from the task jmfit . 4 A RADIO MODEL Radio emission from core-collapse SNe is synchrotron in origin (Chevalier 1982a , b ), produced due to the interaction of SN ejecta with the CSM created by the stellar wind of the progenitor star. According to the standard