Romero, Charles E.Charles E.RomeroSievers, JonathanJonathanSieversGHIRARDINI, VITTORIOVITTORIOGHIRARDINIDicker, SimonSimonDickerGiacintucci, SimonaSimonaGiacintucciMroczkowski, TonyTonyMroczkowskiMason, Brian S.Brian S.MasonSarazin, CraigCraigSarazinDevlin, MarkMarkDevlinGASPARI, MASSIMOMASSIMOGASPARIBattaglia, NicholasNicholasBattagliaHilton, MatthewMatthewHiltonBulbul, EsraEsraBulbulLowe, IanIanLoweStanchfield, SaraSaraStanchfield2021-11-262021-11-2620200004-637Xhttp://hdl.handle.net/20.500.12386/31163The galaxy cluster Zwicky 3146 is a sloshing cool core cluster at z=0.291 that in X-ray imaging does not appear to exhibit significant pressure substructure in the intracluster medium (ICM). The published M500 values range between 3.88+0.62−0.58 to 22.50±7.58×10^14 M⊙, where ICM-based estimates with reported errors <20% suggest that we should expect to find a mass between 6.53+0.44−0.44×10^14 M⊙ (from Planck, with an 8.4σ detection) and 8.52+1.77−1.47×10^14 M⊙ (from ACT, with a 14σ detection). This broad range of masses is suggestive that there is ample room for improvement for all methods. Here, we investigate the ability to estimate the mass of Zwicky 3146 via the Sunyaev-Zel'dovich (SZ) effect with data taken at 90 GHz by MUSTANG-2 to a noise level better than 15 μK at the center, and a cluster detection of 104σ. We derive a pressure profile from our SZ data which is in excellent agreement with that derived from X-ray data. From our SZ-derived pressure profiles, we infer M500 and M2500 via three methods -- Y-M scaling relations, the virial theorem, and hydrostatic equilibrium -- where we employ X-ray constraints from \emph{XMM-Newton} on the electron density profile when assuming hydrostatic equilibrium. Depending on the model and estimation method, our M500 estimates range from 6.23±0.59 to 10.6±0.95×10^14 M⊙, where our estimate from hydrostatic equilibrium, is 8.29+1.93−1.24 (±19.1\% stat) +0.74−0.68 (±8.6\% sys, calibration) ×10^14 M⊙. Our fiducial mass, derived from a Y-M relation is 8.16+0.44−0.54 (±5.5% stat) +0.46−0.43 (±5.5\% sys, Y-M) +0.59−0.55 (±7.0% sys, cal.) ×10^14 M⊙.STAMPAenArticle10.3847/1538-4357/ab6d70https://iopscience.iop.org/article/10.3847/1538-4357/ab6d702020ApJ...891...90RFIS/05 - ASTRONOMIA E ASTROFISICA