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Observationally measuring the location of the H$_{2}$O snowline is crucialfor understanding the planetesimal and planet formation processes, and theorigin of water on Earth. In disks around Herbig Ae stars ($T_{\mathrm{*}}\sim$10,000K, $M_{\mathrm{*}}\gtrsim$ 2.5$M_{\bigodot}$), the position of theH$_{2}$O snowline is further from the central star compared with that aroundcooler, and less massive T Tauri stars. Thus, the H$_{2}$O emission line fluxesfrom the region within the H$_{2}$O snowline are expected to be stronger. Inthis paper, we calculate the chemical composition of a Herbig Ae disk usingchemical kinetics. Next, we calculate the H$_{2}$O emission line profiles, andinvestigate the properties of candidate water lines across a wide range ofwavelengths (from mid-infrared to sub-millimeter) that can locate the positionof the H$_{2}$O snowline. Those line identified have small Einstein $A$coefficients ($\sim 10^{-6} -10^{-3}$ s$^{-1}$) and relatively high upper stateenergies ($\sim$ 1000K). The total fluxes tend to increase with decreasingwavelengths. We investigate the possibility of future observations (e.g., ALMA,SPICA/SMI-HRS) to locate the position of the H$_{2}$O snowline. Since thefluxes of those identified lines from Herbig Ae disks are stronger than thosefrom T Tauri disks, the possibility of a successful detection is expected toincrease for a Herbig Ae disk.

Candidate Water Vapor Lines to Locate the H$_{2}$O Snowline through High-Dispersion Spectroscopic Observations II. The Case of a Herbig Ae Star