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The recent fast growth of a population of millisecond pulsars with preciselymeasured mass provides an excellent opportunity to characterize these compactstars at an unprecedented level. This is because the stellar parameter valuescan be accurately computed for known mass and spin rate and an assumed equationof state (EoS) model. For each of the 16 such pulsars and for a set of EoSmodels from nucleonic, hyperonic, strange quark matter and hybrid classes, wenumerically compute fast spinning stable stellar parameter values consideringthe full effect of general relativity. This first detailed catalogue of thecomputed parameter values of observed millisecond pulsars provides a testbed toprobe the physics of compact stars, including their formation, evolution andEoS. We estimate uncertainties on these computed values from the uncertainty ofthe measured mass, which could be useful to quantitatively constrain EoSmodels. We note that the largest value of the central density $\rho_{\rm c}$ inour catalogue is $\sim 5.8$ times the nuclear saturation density $\rho_{\rmsat}$, which is much less than the expected maximum value $13 \rho_{\rm sat}$.We argue that the $\rho_{\rm c}$-values of at most a small fraction of compactstars could be much larger than $5.8 \rho_{\rm sat}$. Besides, we find that theconstraints on EoS models from accurate radius measurements could besignificantly biased for some of our pulsars, if stellar $spinning$configurations are not used to compute the theoretical radius values.

Millisecond radio pulsars with known masses: parameter values and equation of state models