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tokens: 1, 2, and 3 are A10 , M12 , P17 , respectively; for M 2500 , the relations come from C11 , M12 , P17 , respectively. The agreement or disagreement of M HE with the other mass estimates also highlights a key procedural/mathematical difference between the methods of estimation: we calculate M HE at individual radii, which does not make use of knowledge of the pressure profile across all radii. However, the Y – M mass makes use of Y , a cumulative sum of spherically integrated pressure within R 500 (or R 2500 ). Similarly, M VT is fit across all pressure bins at radii larger than 100 kpc. Physically, we may expect M HE , M VT , and ( Y – M ) A10 (or ( Y – M ) C11 for M 2500 ) to be similar, as they directly or indirectly rely on the assumption of HE. The other Y – M relations, being calibrated to weak lensing or simulations, should encapsulate the total mass without regard to dynamical state. We expect mass estimates that assume HE underestimate the total mass due to the so-called hydrostatic mass bias, which itself encompasses several biases. The primary bias is not actually the HE assumption, but rather that the pressure gradient used only accounts for thermal pressure. Thus the lack of account for non-thermal pressure underestimates the mass by 10%–30% (see also Lau et al. 2013 ; Nelson et al. 2014a ; Biffi et al. 2016 ; Khatri Gaspari 2016 ; Hurier Angulo 2018 ; Ettori et al. 2019 ). 5.3. Residuals An underlying quadrupole is observed in our residual map (Figure 5 ). Modeling the ICM with the same centroid and an ellipsoidal ICM distribution results in very similar residual decrements and removes this quadrupole. Beyond ellipticity in the core of the cluster, the only observed SZ substructure is also in the core of the cluster. The corresponding integrated Y ( Y cyl ) due to the substructure (decrement −25 μ K) is 3.0 × 10 −7 h 70 2/3 Mpc 2 , whereas we find Y cyl ( R 500 ) = 7.3 × 10 −5 h 70 2/3 Mpc 2 for our NP fit; thus substructure accounts for only 0.5% of the SZ signal within θ 500 and is not a significant source of scatter in the mass estimates from Y – M relations for this cluster. Figure 5. Residual map (in μ K) of the Minkasi map with the SZ centroid marked by a red cross, the radio sources marked by tri_up (purple on white), and the Herschel 500 micron centroid by a blue cross; the beam is shown in the bottom left. The black contours are every 2 σ , excluding 0 ( σ = 12.8 μ K). As noted before, the central pressure profile and the central point-source amplitude are degenerate. In addition to the central radio source, a second, nearby radio point source is observed at 4.9 and 8.5 GHz (Giacintucci et al. 2014 ). We find that these two sources contribute to a mild increase in the uncertainties in the inner two pressure profile bins. The spatial coincidence of our residual SZ decrement and the radio minihalo (Figure 6 ) may be suggestive of an underlying link. It would be equally interesting if there is a link between the SZ