Dense gas is the direct material feeding star formation. Understanding the properties of dense gas tracers is important for the calculation of dense gas mass. HC\({}_{3}\)N has great potential to serve as a dense gas tracer because of its low optical depth in the interstellar medium. We propose to observe HC\({}_{3}\)N \(J=2-1\) in a sample of massive star forming regions with the Ku band receiver onboard TIANMA 65-m telescope. The relation between HC\({}_{3}\)N2-1 intensity and star formation rate will be analyzed using the 65-m data. This study will provide a new way to estimate the dense gas mass and help us better understand the relation between dense gas and the history of star formation in molecular clouds.