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Saravani, Afshordi and Mann \cite{SAM} considered a surface fluid withvanishing energy density on the stretched horizon of a black hole, taken as thenew boundary of spacetime. We show that their entropy per unit area of thefluid does not correspond to the Bekenstein-Hawking entropy, both for aSchwarzschild black hole and for a Kerr-Newman black hole. Due to the lack of ahorizon, we argue that the Unruh effect could not be taken into account and theconcept of local thermodynamic equilibrium is not sustained because of the$\theta$-dependence of the temperature.

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