In the last few decades many efforts have been made to understand the effect of spiral arms on the gas and stellar dynamics in the Milky Way disc . One of the fundamental parameters of the spiral structure is its angular velocity , or pattern speed \Omega _ { p } , which determines the location of resonances in the disc and the spirals ’ radial extent . The most direct method for estimating the pattern speed relies on backward integration techniques , trying to locate the stellar birthplace of open clusters . Here we propose a new method based on the interaction between the spiral arms and the stars in the disc . Using a sample of around 500 open clusters from the New Catalogue of Optically Visible Open Clusters and Candidates , and a sample of 500 giant stars observed by APOGEE , we find \Omega _ { p } = 23.0 \pm 0.5 km s ^ { -1 } kpc ^ { -1 } , for a local standard of rest rotation V _ { 0 } = 220 km s ^ { -1 } and solar radius R _ { 0 } = 8.0 kpc . Exploring a range in V _ { 0 } and R _ { 0 } within the acceptable values , 200-240 km s ^ { -1 } and 7.5-8.5 kpc , respectively , results only in a small change in our estimate of \Omega _ { p } , that is within the error . Our result is in close agreement with a number of studies which suggest values in the range 20-25 km s ^ { -1 } kpc ^ { -1 } . An advantage of our method is that we do not need knowledge of the stellar age , unlike in the case of the birthplace method , which allows us to use data from large Galactic surveys . The precision of our method will be improved once larger samples of disk stars with spectroscopic information will become available thanks to future surveys such as 4MOST .