  It is widely believed that the cool gas clouds traced by MgII absorption,
within a velocity offset of 5000 km/s relative to the background quasar are
mostly associated with the quasar itself, whereas the absorbers seen at larger
velocity offsets towards us are intervening absorber systems and hence their
existence is completely independent of the background quasar. Recent evidence
by Bergeron et al. (2011, hereinafter BBM) has seriously questioned this
paradigm, by showing that the number density of intervening MgII absorbers
towards the 45 blazars in their sample is nearly 2 times the expectation based
on the MgII absorption systems seen towards normal QSOs. Given its serious
implications, it becomes important to revisit this finding, by enlarging the
blazar sample and subjecting it to an independent analysis. Here, we first
report the outcome of our re-analysis of the available spectroscopic data for
the BBM sample itself. Our analysis of the BBM sample reproduces their claimed
factor of 2 excess of dN/dz along blazar sightlines, vis-a-vis normal QSOs. We
have also assembled a ~3 times larger sample of blazars, albeit with moderately
sensitive optical spectra. Using this sample together with the BBM sample, our
analysis shows that the dN/dz of the MgII absorbers statistically matches that
known for normal QSO sightlines. Further, the analysis indicates that
associated absorbers might be contributing significantly to the estimated dN/dz
upto offset speeds \Delta v ~0.2c relative to the blazar.
