  Solar activity, in particular coronal mass ejections (CMEs), are often
accompanied by bursts of radiation at metre wavelengths. Some of these bursts
have a long duration and extend over a wide frequency band, namely, type IV
radio bursts. However, the association of type IV bursts with coronal mass
ejections is still not well understood. In this article, we perform the first
statistical study of type IV solar radio bursts in the solar cycle 24. Our
study includes a total of 446 type IV radio bursts that occurred during this
cycle. Our results show that a clear majority, $\sim 81 \%$ of type IV bursts,
were accompanied by CMEs, based on a temporal association with white-light CME
observations. However, we found that only $\sim 2.2 \%$ of the CMEs are
accompanied by type IV radio bursts. We categorised the type IV bursts as
moving or stationary based on their spectral characteristics and found that
only $\sim 18 \%$ of the total type IV bursts in this study were moving type IV
bursts. Our study suggests that type IV bursts can occur with both `Fast'
($\geq 500$ km/s) and `Slow' ($< 500$ km/s), and also both `Wide' ($\geq
60^{\circ}$) and `Narrow' ($< 60^{\circ}$) CMEs. However, the moving type IV
bursts in our study were mostly associated with `Fast' and `Wide' CMEs ($\sim
52 \%$), similar to type II radio bursts. Contrary to type II bursts,
stationary type IV bursts have a more uniform association with all CME types.
