Notes. ^(a) Position angles of bipolar outflows and outflow opening angles, measured counterclockwise from the north, taken from the literature. If the red- and blueshifted lobes have different position angles, we average them together. Hull et al. (2017b), Aso et al. (2019), Tychoniec et al. (2019) and Le Gouellec et al. (2019) for Serpens Emb 6, Emb 8 and Emb 8(N). Tobin et al. (2019) for BHR71 IRS1 and IRS2. Takahashi & Ho (2012) and Hull et al. (2014) for OMC3 MMS6. Hull et al. (2014), Velusamy et al. (2014) and Tobin et al. (2018) for L1448 IRS2 and B335. Santangelo et al. (2015a), Ching et al. (2016) and Tobin et al. (2018) for IRAS4A. Santangelo et al. (2015b) and Murillo et al. (2018) for VLA 1623. Yeh et al. (2008), Kristensen et al. (2013), Girart et al. (2014) and van der Wiel et al. (2019) for IRAS 16293. ^(b) Thickness of the equatorial planes, fit by eye. ^(c)Thickness of outflow cavity walls, fit by eye. ^(d)We show the average values of e and c obtained from the observations at the three different wavelengths. ^(e)Both outflows are from IRAS 16293A; IRAS 16293B does not have any detected outflow. The parameters e and c have been determined by eye thanks to the previously published CO emission. Furthermore, IRAS 16293B lies within one of the outflow cones of IRAS 16293A; however, we consider it to be envelope emission. ^(f) VLA1623A/B do not have clearly identifiable outflow cavities in the polarized dust emission. Therefore we consider all the emission of this source to be coming from the envelope. However, we keep the parameters e and c (determined by eye thanks to the CO emission) in this table and the white-dotted lines in Fig. B.2 to simply indicate the location and shape of the outflow. ^(g)We report e and c for the two datasets separately, as they have very different angular resolutions. ^(h) We report values separately for the two protostars in this core, IRAS4A1 and IRAS4A2.