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