We select E+A candidates from a spectroscopic dataset of \sim 800 field galaxies and measure the E+A fraction at 0.3 < z < 1 to be 2.7 \pm 1.1 % , a value lower than that in galaxy clusters at comparable redshifts ( 11 \pm 3 % ) . HST/WFPC2 imaging for five of our six E+A ’ s shows they have a heterogeneous parent population : these E+A ’ s span a range in half-light radius ( 0.8 < r _ { 1 / 2 } < 8 h ^ { -1 } kpc ) and estimated internal velocity dispersion ( 50 \lesssim \sigma _ { est } \lesssim 220 km s ^ { -1 } ) , and they include luminous systems ( -21.6 \leq M _ { Bz } -5 logh \leq - 19.2 ) . Despite their diversity in some aspects , the E+A ’ s share several common characteristics that indicate the E+A phase is an important link in the evolution of star-forming galaxies into passive systems : the E+A ’ s are uniformly redder than the blue , star-forming galaxies that make up the majority of the field , they are more likely to be bulge-dominated than the average field galaxy , and they tend to be morphologically irregular . We find E+A ’ s make up \sim 9 % of the absorption line systems in this redshift range , and estimate that \gtrsim 25 % of passive galaxies in the local field had an E+A phase at z \lesssim 1 .