We develop new hyperon equation of state ( EoS ) tables for core-collapse supernova simulations and neutron stars .
These EoS tables are based on a density-dependent relativistic hadron field theory where baryon-baryon interaction is mediated by mesons , using the parameter set DD2 from Typel et al .
( 71 ) for nucleons .
Furthermore , light and heavy nuclei along with the interacting nucleons are treated in the nuclear statistical equilibrium model of Hempel and Schaffner-Bielich which includes excluded volume effects .
Of all possible hyperons , we consider only the contribution of \Lambda s. We have developed two variants of hyperonic EoS tables : in the np \Lambda \phi case the repulsive hyperon-hyperon interaction mediated by the strange \phi meson is taken into account , and in the np \Lambda case it is not .
The EoS tables for the two cases encompass wide range of density ( 10 ^ { -12 } to \sim 1 fm ^ { -3 } ) , temperature ( 0.1 to 158.48 MeV ) , and proton fraction ( 0.01 to 0.60 ) .
The effects of \Lambda hyperons on thermodynamic quantities such as free energy per baryon , pressure , or entropy per baryon are investigated and found to be significant at higher densities .

The cold , \beta -equilibrated EoS ( with the crust included self-consistently ) results in a 2.1 M _ { \odot } maximum mass neutron star for the np \Lambda \phi whereas that for the np \Lambda case is 1.95 M _ { \odot } .
The np \Lambda \phi EoS represents the first supernova EoS table involving hyperons that is directly compatible with the recently measured 2 M _ { \odot } neutron stars .