A measurement of the Shapiro delay in the binary millisecond pulsar PSR J1614−2230 provides a highly precise determination of the neutron star (NS) mass. The observed Shapiro delay, which is an increase in light travel time through curved spacetime near a massive object, allows for the inference of the masses of both the NS and its binary companion. The NS mass of 1.97 ± 0.04 M☉ is the highest measured with such certainty, effectively ruling out the presence of hyperons, bosons, or free quarks at nuclear saturation densities. The companion mass is determined to be 0.500 ± 0.006 M☉, indicating a helium-carbon-oxygen white dwarf. The binary system has an inclination of 89.17° ± 0.02°, making it one of the most edge-on pulsar binaries known. The high inclination and massive companion result in a Shapiro delay amplitude much larger than for most other millisecond pulsars. The timing precision achieved with the Green Bank Telescope and GUPPI instrument provides a high signal-to-noise ratio measurement of the Shapiro delay parameters. The NS mass measurement significantly constrains the NS equation of state (EOS), ruling out many models that predict lower maximum masses. The results also suggest that some neutron stars may be born massive, and that many other millisecond pulsar systems may harbor NSs with masses well above 1.4 M☉. The study highlights the importance of Shapiro delay measurements in constraining NS properties and the EOS of dense matter.A measurement of the Shapiro delay in the binary millisecond pulsar PSR J1614−2230 provides a highly precise determination of the neutron star (NS) mass. The observed Shapiro delay, which is an increase in light travel time through curved spacetime near a massive object, allows for the inference of the masses of both the NS and its binary companion. The NS mass of 1.97 ± 0.04 M☉ is the highest measured with such certainty, effectively ruling out the presence of hyperons, bosons, or free quarks at nuclear saturation densities. The companion mass is determined to be 0.500 ± 0.006 M☉, indicating a helium-carbon-oxygen white dwarf. The binary system has an inclination of 89.17° ± 0.02°, making it one of the most edge-on pulsar binaries known. The high inclination and massive companion result in a Shapiro delay amplitude much larger than for most other millisecond pulsars. The timing precision achieved with the Green Bank Telescope and GUPPI instrument provides a high signal-to-noise ratio measurement of the Shapiro delay parameters. The NS mass measurement significantly constrains the NS equation of state (EOS), ruling out many models that predict lower maximum masses. The results also suggest that some neutron stars may be born massive, and that many other millisecond pulsar systems may harbor NSs with masses well above 1.4 M☉. The study highlights the importance of Shapiro delay measurements in constraining NS properties and the EOS of dense matter.