We present results of a pulsar population synthesis study that incorporates a number of recent developments and some significant improvements over our previous study .
We have included the results of the Parkes multi-beam pulsar survey in our select group of nine radio surveys , doubling our sample of radio pulsars .
More realistic geometries for the radio and \gamma -ray beams are included in our Monte Carlo computer code that simulates the characteristics of the Galactic population of radio and \gamma -ray pulsars .
We adopted with some modifications the radio beam geometry of Arzoumanian , Chernoff & Cordes ( 2002 ) .
For the \gamma -ray beam , we have assumed the slot gap geometry described in the work of Muslimov & Harding ( 2003 ) .
To account for the shape of the distribution of radio pulsars in the \dot { P } - P diagram , we continue to find that decay of the magnetic field on a timescale of 2.8 Myr is needed .
With all nine surveys , our model predicts that EGRET should have seen 7 radio-quiet ( below the sensitivity of these radio surveys ) and 19 radio-loud \gamma -ray pulsars .
AGILE ( nominal sensitivity map ) is expected to detect 13 radio-quiet and 37 radio-loud \gamma -ray pulsars , while GLAST , with greater sensitivity is expected to detect 276 radio-quiet and 344 radio-loud \gamma -ray pulsars .
When the Parkes multi-beam pulsar survey is excluded , the ratio of radio-loud to radio-quiet \gamma -ray pulsars decreases , especially for GLAST .
The decrease for EGRET is 45 % , implying that some fraction of EGRET unidentified sources are radio-loud \gamma -ray pulsars .
In the radio geometry adopted , short period pulsars are core dominated .
Unlike the EGRET \gamma -ray pulsars , our model predicts that when two \gamma -ray peaks appear in the pulse profile , a dominant radio core peak appears in between the \gamma -ray peaks .
Our findings suggest that further improvements are required in describing both the radio and \gamma -ray geometries .