Extended Data Fig. 10: Modeled radial velocity dispersion profiles produced by propagating sound waves.
From: Disentangling multiple gas kinematic drivers in the Perseus galaxy cluster
(a) Assuming conserved energy flux Fsw ( ≡ αFagn) of the sound waves starting from the cluster radius r0 powered by the central AGN (Fagn = 5 × 1044 erg s−1). (b) Assuming sound waves compensate a fraction (β) of cooling loss everywhere within the radius \({r}_{\max }\). Red points are our measured velocity dispersion, same as in Fig. 2.
