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The rate of tidal disruption events (TDEs), $R_\text{TDE}$, is predicted todepend on stellar conditions near the super-massive black hole (SMBH), whichare on difficult-to-measure sub-parsec scales. We test whether $R_\text{TDE}$depends on kpc-scale global galaxy properties, which are observable. Weconcentrate on stellar surface mass density, $\Sigma_{M_\star}$, and velocitydispersion, $\sigma_v$, which correlate with the stellar density and velocitydispersion of the stars around the SMBH. We consider 35 TDE candidates, withand without known X-ray emission. The hosts range from star-forming toquiescent to quiescent with strong Balmer absorption lines. The last (oftenwith post-starburst spectra) are overrepresented in our sample by a factor of$35^{+21}_{-17}$ or $18^{+8}_{-7}$, depending on the strength of the H$\delta$absorption line. For a subsample of hosts with homogeneous measurements,$\Sigma_{M_\star}=10^9$-$10^{10}~{\rm M_\odot / kpc^2}$, higher on average thanfor a volume-weighted control sample of Sloan Digital Sky Survey galaxies withsimilar redshifts and stellar masses. This is because: (1) most of the TDEhosts here are quiescent galaxies, which tend to have higher $\Sigma_{M_\star}$than the star-forming galaxies that dominate the control, and (2) thestar-forming hosts have higher average $\Sigma_{M_\star}$ than the star-formingcontrol. There is also a weak suggestion that TDE hosts have lower $\sigma_v$than for the quiescent control. Assuming that $R_{\rm TDE}\propto\Sigma_{M_\star}^\alpha \times \sigma_v^\beta$, and applying a statisticalmodel to the TDE hosts and control sample, we estimate $\hat{\alpha}=0.9 \pm0.2$ and $\hat{\beta}=-1.0 \pm 0.6$. This is broadly consistent with$R_\text{TDE}$ being tied to the dynamical relaxation of stars surrounding theSMBH.

A dependence of the tidal disruption event rate on global stellar surface mass density and stellar velocity dispersion