Sr, Y, and Ba yields from AGB stars as a function of initial stellar mass. The yields are weighted by the P. Kroupa et al. (1993) IMF. Different colors represent different metallicities of the progenitor star. The solid lines show the yields used in this work, with the gray dotted lines showing the yields of A. I. Karakas & M. Lugaro (2016) and A. I. Karakas et al. (2018) for comparison. In the bottom panel, the dashed blue lines show the best-fit Ba yields used in dlR22.