tokens: We found that the best-fitting soft-excess flux predictions are off by at least a factor of two from the values measured by Tripathi et al. ( 2021 ), except for the extinction curve of Czerny et al. ( 2004 ) with E ( B − V ) = 1.0. In this case, the estimated soft excess flux in the 0.3–2 keV is within the range of the fluxes measured by Tripathi et al. ( 2021 ) from the five AstroSat observations. The best-fitting inner radius and accretion rate are 126 R g and of the Eddington rate, respectively. This suggests that the inner disc in IC 4329A could be covered by a warm, optically thick layer, whose emission is consistent with the optical/UV SED and could also explain the observed soft-excess we detect in this source. 5 DISCUSSION AND CONCLUSIONS We present the results from the analysis of UV images of IC 4329A obtained with AstroSat / UVIT observations. These are the highest resolution and deepest images of IC 4329A ever acquired with any telescope in the near and far-UV bands. The UVIT images enabled us to calculate the galaxy radial profile, and unambiguously separate the AGN emission from the extended emission of the host galaxy by fitting the profiles with the appropriate functions. We derived the intrinsic AGN continuum flux after de-reddening for both the Galactic and internal extinctions, and correcting for the contribution of emission lines. The active nucleus is not detected in the FUV band, and we were able to put a conservative 3σ upper limit on the AGN flux in this band. When combined with the AGN flux in the NUV and 5100 Å (taken from past observations), we found that the far-UV/optical, intrinsic emission of the active nucleus in IC 4329A, requires no disc emission below ∼80–170 R g . The superb spatial resolution of UVIT is crucial in this case, specially in the FUV. If we had performed simple aperture photometry in the FUV image, using a 5–10 arcsec radius (as is typically the case), we would have ended with a flux measurement at least seven times larger than the 3σ upper limit we have determined in this band. Since the host galaxy in most templates is assumed to emit very little at these short wavelengths, this measurement would have been assumed to be intrinsic of the active nucleus, and this false result would have critically altered the shape of the intrinsic AGN SED at short wavelengths. X-ray reflection spectroscopy can independently probe the inner accretion discs via the relativistic iron Kα line near ∼6.4 keV and the strength of the reflection. Using XMM-Newton observations of IC 4329A, Nandra et al. ( 2007 ) derived a low-disc reflection fraction of R f ∼0.3 ( R f is defined as the ratio of the X–ray intensity that illuminates the disc to the intensity that reaches the observer; R f = 1 corresponds to a semi-infinite slab subtending 2π solid angle at the X-ray source). Using NuSTAR observations, Brenneman et al. ( 2014 ) detected a moderately broad iron line with a Gaussian σ ∼0.36 keV in addition to narrow iron Kα,
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