We performed a comprehensive analysis of the Herschel spectra of BHR71, an embedded Class 0 protostar. We recover 66 lines in the central spaxel, and more than 700 lines are detected in all spaxels in PACS, and SPIRE. The CO rotational diagram analysis shows four excitation temperature components, 51 K, 153 K, 408 K, and 1053 K. Low-J CO lines trace the outflow while the high-J CO lines are centered on the infrared source. The emissions of H2O traces the outflow on large scales, while H2O emissions populate along the equatorial plane on small scale scales. We model the structure of envelope using dust radiative transfer with Hyperion to fit the spectral energy distribution (SED) observed by Spitzer and Herschel. The model incorporates rotational collapse and an outer static envelope as well as outflow cavity and disk. Our exploration of parameter space shows that the evolution of collapsing envelope can be constrained by Herschel spectra and the structure of outflow cavity plays a critical role in the shorter wavelength. We found that the density profile of cavity with a power law with a constant inner region is necessary to reproduce the observations. The high central luminosity in the best-fit model shows a hint of a higher accretion rate than the rate derived from collapse model. Our model constrains BHR71 to have an age of 26000 years and a total dust mass of 0.06 Solar mass.