the optical the SN remains much brighter than the underlying light so contamination was negligible. An aperture correction (based on an average PSF in [*Swift*]{} CALDB) as well as zeropoints from @poole08 was applied to put the magnitudes on the UVOT photometric system. The UVOT magnitudes are listed in Table \[tab:uvotsn\].

From +5d to +416d, the follow-up of SN 2008in in optical broadband Johnson $UBV$ and Cousins $RI$ was performed with the 1-m Sampurnanand Telescope (ST) at ARIES, Nainital[^2]. An identification chart showing the field of the galaxy M61 along with the locations of  as well as the local standards is presented in Figure \[fig:snid\]. The photometry is performed using standard tasks of IRAF [^3] and [*DAOPHOT*]{} [^4] as described in the paper by @roy11. Bias subtraction and flat fielding were performed on the raw frames and the cosmic removal was done using LACOSMIC routine [@dokkum01]. As the SN lies in the outskirts of the galaxy on a relatively faint and smooth background, the photometry at the initial phases (mostly during the plateau phase when the SN is bright) is estimated using the profile fitting method. During nebular phases, when the SN becomes faint, the true SN flux is estimated 