A mapping study of 71 Planck cold clumps was made with ^12^CO(1-0), ^13^CO(1-0), and C^18^O(1-0) lines at the 13.7m telescope of Purple Mountain Observatory. For all the clumps, ^12^CO(1-0) and ^13^CO(1-0) emissions were detected, while for 55 of them, C^18^O(1-0) emissions were detected. Of the 71 Clumps, 34 are in the Taurus Complex, 24 in the California Complex, and 13 are in the Perseus Complex. In the 76 velocity components, 38 cores are found in 27 clumps; 19 of these cores are in the Taurus Complex, 16 in the California Complex, and 3 in the Perseus Complex. We acquired V_lsr_, T_A_ and FWHM of lines. Physical parameters including T_ex_, N_H2_, {sigma}_Therm_, {sigma}_NT_, and {sigma}_3D_were calculated. Generally, the cores are of T_ex_=2-16K, N_H2_/cm2, and {sigma}_3D_=0.2-1.0km/s. In the Taurus Complex, the cores are less dense on average and have smaller {sigma}_Therm_than the cores in the Perseus and California Complexes. Two of the three cores in the Perseus Complex are revealed to have larger T_ex_, N_H2_, and {sigma}_3D_ than the mean values in the other two regions. Most of the cores have {sigma}_NT_larger than {sigma}_Therm_, suggesting a dominance of turbulence in our cores. The majority of the cores have M_vir_/M_LTE_{Gt} 1, which indicates these cores are not bound and will disperse. By comparing our results with the dust properties revealed by the Planck Early Release Cold Cores Catalog, we investigated the coupling of gas and dust components. We found that most of the cores have dust temperatures higher than their gas temperatures. The stellar objects associated with our sources were checked and 90% of the cores were found to be starless.