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Fig. 10.


Radius-mass diagram for the 12 EOSs used in this paper to accomplish a good coverage of the range from soft to stiff EOSs, while still being in agreement with the tidal deformability test in the GW170817 LIGO/Virgo event (Abbott et al. 2017, 2018) (black curves). The blue dashed line indicates the mass of PSR J0337+1715, and the red dotted line corresponds to the most massive neutron star used in our combined test: PSR J0348+0432 (Antoniadis et al. 2013). The black curves correspond to the following EOSs (from left to right in their intersection with the red dotted line): WFF1, SLy4, WFF2, AP4, BSk20, ENG, SLy9, AP3, BSk25, BSk21, MPA1, BSk22 (see Lattimer & Prakash 2001 and Our stiffest EOS, BSk22, is also in agreement with the (more model dependent) constraint of Mmax ≲ 2.3 M by Rezzolla et al. (2018), Shibata et al. (2019). We have included EOS H4 (grey curve), which is disfavoured by GW170817, and therefore has not been used in Figs. 11 and 12. All these EOSs also agree with the latest constraints from NICER (Miller et al. 2019).

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