Reimagining the Water Snowline

Water is a molecule that tightly related to many facets of star and planet formation. Water's abundance distribution, especially the location it's snowline has thus been subject much study. While water seen be abundant in inner region proto-planetary disks infrared spectroscopy, detections disk sub-millimeter are rare, with only one detection towards AS 205. Here we put multitude non-detections single into context recent physico-chemical models. We find 321.2257 GHz (10(2,9) - 9(3,6)) line 205 inconsistent normal temperature structure observed must masing. Furthermore, emitting area derived from width, together published analyses on around T-Tauri stars implies surface at same as mid-plane. propose this caused by vertical mixing continuously sequestering warm layers cold midplane.