A detailed analysis of H2O emission in the JWST-MIRI spectra of 8 millimeter-compact disks

H2O is one of the key ingredients for habitability. While it is not yet fully understood how forming planets obtain their H2O reservoirs, the molecule has a striking imprint on the mid-infrared spectrum of planet-forming disks. With many ro-vibrational (below 10 micron) and pure rotational (above 10 micron) transitions distributed throughout the 4.9-27.5 micron wavelength range observed by JWST/MIRI-MRS, the available H2O reservoirs in the inner disks can be investigated. Disks that are compact in the dust millimeter emission are especially interesting targets for the characterisation of their H2O reservoirs. As their compactness is thought to be the result of efficient radial drift, a larger reservoir of H2O near its snowline may be expected compared to their large, structured counterparts. In this talk, I will present the first results of an extensive analysis of the H2O emission of 8 compact disks around isolated stars, all part of the MINDS GTO program. These results will highlight the trends seen in the H2O emission, include full descriptions of the rotational H2O spectra using both power-law and multiple component slab models, and demonstrate the likeliness of an enhanced cold (T=150-180 K) reservoir, due to the efficient radial drift, through promising line ratios.