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The infrared spectral energy distributions (SEDs) of $z\gtrsim 5$ quasars canbe reproduced by combining a low-metallicity galaxy template with a standardAGN template. The host galaxy is represented by Haro 11, a compact, moderatelylow metallicity, star-bursting galaxy that shares typical features of high-$z$galaxies. For the vast majority of $z\gtrsim 5$ quasars, the AGN contributionis well modeled by a standard empirical template with the contamination of starformation in the infrared subtracted. Together, these two templates canseparate the contributions from the host galaxy and the AGN even in the case oflimited data points, given that this model has only two free parameters. Usingthis method, we re-analyze 69 $z\gtrsim 5$ quasars with extensive Herschelobservations, and derive their AGN luminosities $L_{\rm AGN}$ in a range $\sim(0.78-27.4) \times10^{13}\, L_{\odot}$, the infrared luminosities from starformation $L_{\rm SF,IR} \sim (<1.5-25.7)\times10^{12}\, L_{\odot}$, and thecorresponding star formation rates ${\rm SFR}\sim (<290-2650)\, M_\odot/{\rmyr}$. The average infrared luminosity from star formation and the average totalAGN luminosity of the $z\gtrsim5$ quasar sample follows the correlation definedby quasars at $z < 2.6$. We assume these quasar host galaxies maintain aconstant average SFR ($\sim620\, M_\odot/{\rm yr}$) during their mass assemblyand estimate the stellar mass that could form till $z\sim5-6$ to be $\langleM_* \rangle \sim(3-5)\times10^{11} M_\odot$. Combining with the black hole (BH)mass measurements, this stellar mass is adequate to establish a BH-galaxy massratio $M_{\rm BH}/M_{*}$ at 0.1-1%, consistent with the local relation.

The Contribution of Host Galaxies to the Infrared Energy Output of $z\gtrsim5.0$ QUASARS