Superluminous supernovae (SLSNe) are the most luminous SNe having mean absolute magnitude ≈ −21.7 mag. SLSNe are very rare, comprising only ∼0.01% of the normal population of the CCSNe (Quimby et al. 2013). Based on the spectroscopic studies, like normal SNe, SLSNe are divided into two categories: hydrogen-poor (SLSNe-I) and hydrogen-rich (SLSNe-II). SLSNe-I are thought to be a subtype of SNe-Ic, because after a few weeks they exhibit spectral features similar to those of Type Ic. SLSNe-I are broadly classified into fast- and slow-decaying categories. We present data and analysis of SN 2010kd, a low-redshift (z = 0.101) H-deficient superluminous supernova, based on the ultraviolet+optical photometry (taken with the Swift-UVOT and ROTSE-IIIb) and the optical spectroscopy (from the Hobby-Eberly Telescope and Keck telescopes) obtained between −28 and +193 days relative to the B-band optical maximum light. Analytical light curve modelling using the Minim code suggests that the bolometric light curve of SN 2010kd cannot be fitted with a single power source and favours models having combined circumstellar matter interaction and heating from radioactive decay for the powering mechanism.