We have calculated the two-point correlation functions in redshift space , \xi ( \sigma, \pi ) , for galaxies of different spectral types in the 2dF Galaxy Redshift Survey .
Using these correlation functions we are able to estimate values of the linear redshift-space distortion parameter , \beta \equiv \Omega _ { m } ^ { 0.6 } / b , the pairwise velocity dispersion , a , and the real-space correlation function , \xi ( r ) , for galaxies with both relatively low star-formation rates ( for which the present rate of star formation is less than 10 % of its past averaged value ) and galaxies with higher current star-formation activity .
At small separations , the real-space clustering of passive galaxies is very much stronger than that of the more actively star-forming galaxies ; the correlation-function slopes are respectively 1.93 and 1.50 , and the relative bias between the two classes is a declining function of radius .
On scales larger than 10 h ^ { -1 } Mpc there is evidence that the relative bias tends to a constant , b _ { passive } / b _ { active } \simeq 1 .
This result is consistent with the similar degrees of redshift-space distortions seen in the correlation functions of the two classes – the contours of \xi ( \sigma, \pi ) 
require \beta _ { active } = 0.49 \pm 0.13 , and \beta _ { passive } = 0.48 \pm 0.14 .
The pairwise velocity dispersion is highly correlated with \beta .
However , despite this a significant difference is seen between the two classes .
Over the range 8 - 20 h ^ { -1 } Mpc , the pairwise velocity dispersion has mean values 416 \pm 76 { km s } ^ { -1 } and 612 \pm 92 { km s } ^ { -1 } for the active and passive galaxy samples respectively .
This is consistent with the expectation from morphological segregation , in which passively evolving galaxies preferentially inhabit the cores of high-mass virialised regions .