  We study slowly rotating accretion flow at parsec and sub-parsec scale
irradiated by a low luminosity active galactic nuclei. We take into account the
Compton heating, photoionization heating by the central X-rays. The
bremsstrahlung cooling, recombination and line cooling are also included. We
find that due to the Compton heating, wind can be thermally driven. The power
of wind is in the range $(10^{-6}-10^{-3}) L_{\rm Edd}$, with $L_{\rm Edd}$
being the Eddington luminosity. The mass flux of wind is in the range $(0.01-1)
\dot M_{\rm Edd}$ ($\dot M_{\rm Edd}= L_{\rm Edd}/0.1c^2$ is the Eddington
accretion rate, $c$ is speed of light). We define the wind generation
efficiency as $\epsilon = P_W/\dot {M}_{\rm BH}c^2$, with $P_W$ being wind
power, $\dot M_{\rm BH}$ being the mass accretion rate onto the black hole.
$\epsilon$ lies in the rage $10^{-4}-1.18$. Wind production efficiency
decreases with increasing mass accretion rate. The possible role of the
thermally driven wind in the active galactic feedback is briefly discussed.
