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Gravitational wave astronomy pipelines rely on template waveform models forsearches and parameter estimation purposes. For coalescing binary neutron stars(BNS), such models need to accurately reproduce numerical relativity (NR) up tomerger, in order to provide robust estimate of the stars' equation of state -dependent parameters. In this work we present an improved version of theEffective One Body (EOB) model $\tt TEOBResumS$ for gravitational waves fromBNS systems. Building upon recent post-Newtonian calculations, we includesubleading order tidal terms in the waveform multipoles and EOB metricpotentials, as well as add up to 5.5PN terms in the gyro-gravitomagneticfunctions entering the spin-orbit sector of the model. In order to furtherimprove the EOB-NR agreement in the last few orbital cycles before merger, weintroduce next-to-quasicircular corrections in the waveform -- informed by alarge number of BNS NR simulations -- and introduce a new NR-informed parameterentering the tidal sector of our conservative dynamics. The performance of ourmodel is then validated against 14 new eccentricity reduced simulations ofunequal mass, spinning binaries with varying equation of state. A time-domainphasing analysis and mismatch computations demonstrate that the new modeloverall improves over the previous version of $\tt TEOBResumS$. Finally, wepresent a closed-form frequency domain representation of the (tidal) amplitudeand phase of the new model. This representation accounts for mass-ratio,aligned spin and (resummed) spin-quadrupole effects in the tidal phase and --within the calibration region -- it is faithful to the original model.

Analytically improved and numerical-relativity informed effective-one-body model for coalescing binary neutron stars