Notes. Column 1 reports the name of the POETS targets: the two sources in italic characters have been observed prior of the POETS survey; Cols. 2 and 3 give the trigonometric parallax distance from BeSSeL (available for all but four sources, for which the kinematic distance is reported) and the evaluated bolometric luminosity, respectively: kinematic distances and more uncertain luminosities are given in italic characters, and values which might be severe upper limits are enclosed within brackets; Cols. 4 and 5 give the RA and Dec coordinates, respectively, of the YSO, pinpointed by JVLA, high-angular resolution, radio continuum observations; Cols. 6 and 7 list the number of detected maser cloudlets and the maximum maser separation from the YSO, respectively. ^(a) In a few cases where the continuum emission shows two nearby peaks, we choose the peak closer to most of the water masers. In three objects, G005.88−0.39, IRAS 20126+4104, and AFGL 5142, previously studied at subarcsecond resolution with millimeter and near-infrared interferometers, we have used the position of the YSO identified through continuum or molecular line emissions. ^(b) In this target, the water maser emission has faded away over the VLBI observing epochs, and nor trigonometric parallax distance neither reliable maser proper motions have been measured. ^(c) In this target, the water maser emission comes from two nearby YSOs, resolved through subarcsecond VLA observations, named VLA 3A and VLA 3B. ^(d)In this target, the water maser emission comes from two nearby YSOs, resolved through subarcsecond VLA observations, named VLA-1 and VLA-2.