  We present a detailed analysis of a cool-core galaxy cluster Abell 3017, at a
redshift of z=0.219, which has been identified to be merging with its companion
cluster Abell 3016. This study has made use of X-ray Chandra, UV (GALEX),
optical (ESO/VLT), mid-infrared (WISE), and radio uGMRT observations of this
cluster. Using various image processing techniques, such as unsharp masking,
2-d fits using Beta models, contour binning and the use of surface brightness
profiles, we show the existence of a pair of X-ray cavities, at a projected
distance of $\sim$20'' (70 kpc) and $\sim$16'' (57 kpc), respectively from the
core of Abell~3017. We also detect an excess of X-ray emission located at 25''
$\sim$(88 kpc) south of the centre of Abell 3017, is likely due to the bulk
motions in the ICM either by gas sloshing or ram-pressure striping due to a
merger. We find that the radio lobes are responsible for the observed X-ray
cavities detected in this system. The lower values of the mid-IR WISE colour
[W1-W2] and [W2-W3] imply that the central BCG of Abell~3017 is a star-forming
galaxy. The current star formation rate of the central BCG, estimated from the
${\rm H\alpha}$ and GALEX FUV luminosities, are equal to be $\sim 5.06\pm 0.78$
Msun yr$^{-1}$ and $\sim 9.20\pm 0.81$ Msun yr$^{-1}$, respectively. We detect,
for the first time, a radio phoenix $\sim$150 kpc away from the radio core,
with a spectral index of ($\alpha \!\leq\! -1.8$). We also report the detection
of $\rm~Pa_\alpha$ emission in this cluster using ESO VLT SINFONI imaging data.
