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; Col. 4 lists the number of detected maser features; Cols. 5 and 6 report the average maser distance from the continuum peak and the corresponding standard deviation, respectively; Cols. 8 and 7 give the PA of the major-axis of the maser spatial distribution, and the spread of the maser positions along the major-axis, respectively: if the spread is ≤20 au, the PA of the spatial distribution is not shown; Col. 9 reports the amplitude of the maser V_LSR gradient for the targets in which it is detected; Cols. 10 and 11 list the average PM amplitude and the PA of the preferential direction of the maser PMs (see Sect. 2.4), respectively, using boldface characters for the PA of the preferential direction if the maser PMs are collimated: targets for which these parameters are not reported have zero or just a single PM measured; Col. 12 indicates the PA of the major-axis of the radio continuum emission associated with the water masers, if the deconvolution with the observing beam was succesful; Cols. 13 and 14 give the PA of the major-axis of the circumstellar disk and the PA of the sky-projected jet axis, if a disk and/or a jet have been detected towards the YSO through high angular-resolution observations in thermal (continuum or line) emission; Col. 15 reports the reference index of the literature observations. ^(a) The elongated chain of H₂ 2.2 μm knots (PA ≈ 53°) and the extinction lane in the J-band image (PA ≈127°) are associated with the bright NIR source #1 of Varricatt (2012), which could correspond with our POETS target G236.82+1.98 within the uncertainties in the astrometric calibration of the UKIRT Wide Field Camera NIR images. ^(b) In this target, the water maser emission comes from two nearby YSOs, resolved through subarcsecond VLA observations, named VLA 3A and VLA 3B. ^(c)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. ^(d) In this target, the water maser emission comes from two nearby YSOs, resolved through subarcsecond VLA observations, named VLA-1 and VLA-2.

References. (1) Sollins et al. (2004); (2) Cyganowski et al. (2011); (3) Moscadelli et al. (2016); (4) Sanna et al. (2019b); (5) Massi et al. (in prep.); (6) Trinidad et al. (2004); (7) Varricatt et al. (2010); (8) Fontani et al. (2009); (9) Brown et al. (2016); (10) Qiu et al. (2014); (11) Cesaroni et al. (2013); (12) Goddi et al. (2011b); (13) Ilee et al. (2016); (14) Beltrán et al. (2014); (15) Varricatt (2012).