  Since 2013 the mass of pulsar PSR J0348+0432 ($M = 2.01\,M_{\odot}$) has
provided a tight constraint on neutron star equation of state. However, a
number of different analyses of the recently detected BNS merger (GW170817)
point to a maximum neutron star mass around $2.16\,M_{\odot}$. In addition, a
recent study determined the mass of the millisecond pulsar PSR J2215+5135 to be
$2.27^{+0.17}_{-0.15}\,M_{\odot}$. In this work we investigate the presence of
hyperons in neutron star matter in light of these new mass measurements using
equations of state calculated in the relativistic mean-field approximation.
Particular attention is paid to the use of the available empirical data from
the study of hypernuclei and that of the SU(3) symmetry relations in fixing the
meson-hyperon coupling constants. We find that hyperonic equations of state
with reasonable choices for the meson-hyperon coupling constants can satisfy
these new mass constraints, with hyperons potentially accounting for more than
10% of the baryons in the core of a neutron star.
