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In the context of whether a massive compact object recently observed in theGW190814 event is a neutron star (NS) or not, we have studied the role of theparameters $\kappa$ and $\Lambda_c$ of the Eddington-inspired Born-Infeld(EiBI) gravity theory on the NS mass-radius relation, moment of inertia, andtidal deformability. The results are compared to recent observation constraintsextracted from the analysis of NS observation data. The NS core equation ofstate (EoS) is calculated using the relativistic mean-field model with the G3parameter set. In the hyperon sector, the SU(3) and hyperon potential depthsare used to determine the hyperon coupling constants. For the inner and outercrusts, we use the crust EoS from Miyatsu et al. (2013). We also maintain thesound speed to not exceed $c$/$\sqrt{3}$ at high densities. We have found that,in general, the NS mass significantly depends on the value of $\kappa$, and theradius $R$ is sensitive to the value of $\Lambda_c$. Moreover, as $\Lambda_c$is equal to zero or less than the accepted bound of the cosmological constant,the NS within the EiBI theory is compatible with observation constraints,including $2.0 M_\odot$ mass, canonical radius $R_{1.4 M_{\odot}}$, moment ofinertia, and tidal deformation. Our investigation also reveals that the $2.6M_\odot$ mass compact object and current observational constraint of canonicalradius $R_{1.4 M_{\odot}}$ can simultaneously be satisfied only when the$\Lambda_c$ value is unphysically too large and negative. Therefore, within thespesific EoS employed in this work, we conclude that the secondary object with$2.6 M_\odot$ observed in the GW190814 event is not likely a static (or aslow-rotating) NS within the EiBI gravity theory.

$2.6 M_\odot$ Compact Object and Neutron Stars within Eddington-Inspired Born-Infeld Theory of Gravity