The high sensitivity Parkes and Swinburne Multibeam pulsar surveys have nearly doubled the number of known pulsars and revealed many more distant pulsars with high dispersion measures .
These data allow us to investigate in more detail the statistical parameters and distribution of pulsars , especially in the central regions of the Galaxy , which was almost impossible in previous low-frequency and less-sensitive surveys .
To estimate the distances to pulsars we used the new NE2001 Galactic electron density model .
We study the Galactic distribution of normal pulsars with 1400 MHz luminosities greater than 0.1 mJy kpc ^ { 2 } refining the shape and parameters of the radial distribution of pulsars . The maximum galactocentric distribution of pulsars is located at 3.2 \pm 0.4 kpc and the scale-length of this distribution is 3.8 \pm 0.4 kpc for the assumed distances to the Galactic center R _ { \odot } = 8.5 kpc .
The surface density of pulsars near the Galactic center is equal to or slightly higher than that in the solar neighborhood . For observable normal pulsars with luminosities \geq 0.1 mJy kpc ^ { 2 } , we also re-estimate their local surface density and birth-rate : 41 \pm 5 pulsars kpc ^ { -2 } and 4.1 \pm 0.5 pulsars kpc ^ { -2 } Myr ^ { -1 } respectively .
For the total number of potentially observable pulsars in the Galaxy , we obtain ( 24 \pm 3 ) \times 10 ^ { 3 } and ( 240 \pm 30 ) \times 10 ^ { 3 } before and after applying beaming correction according the Tauris & Manchester ( 1998 ) beaming model .
Within the limits of errors of estimations these results are in close agreement with the results of the previous studies of Lyne et al .
( 1998 ) ( hereafter LML98 ) . The dependence of these results on the NE2001 model and recommendations for further improvement of electron density distribution are discussed .