Notes. Supercluster members and their properties compared to observations. All masses are in units of 10¹⁴ M_⊙ and X-ray Luminosities are given in units of 10⁴³erg/s/h², measured in the 0.1 to 2.4 keV band if not specified otherwise. The base catalog for these properties are B,B1,M and MO. Where data was incomplete we used (Piffaretti et al. 2011) (*) and (Ikebe et al. 2002) (†) to supplement information. The dynamical masses are obtained from Tully (2015) with supplementary data from Pinzke et al. (2011) (‡), Mendel et al. (2008) (◊), Makarov & Karachentsev (2011) (§), M (♭) and MO (Hercules supercluster). Each subsection of the table lists the most massive or main member first. The blue shading in the names column indicates whether the member is bound to the supercluster core according to the method described by Section 3.3. The probabilities (p) in the last column represent the probability that a given supercluster member is identified purely by chance as introduced in Section 2.5. The main halos of the regions do not have an associated probability with this method. We refer to Hernández-Martínez et al. (2024) for the significance of these matches. The probability for A2147, the only main halo in this work not identified by Hernández-Martínez et al. (2024) is computed according to the method outlined in that study, see also Section 3.1.6. This is indicated by the violet color.