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We make use of two suits of ultra high resolution N-body simulations ofindividual dark matter haloes from the Phoenix and the Aquarius Projects toinvestigate systematics of assembly history of subhaloes in dark matter haloesdiffering by a factor of $1000$ in the halo mass. We have found that realprogenitors which built up present day subhalo population are relatively moreabundant for high mass haloes, in contrast to previous studies claiming auniversal form independent of the host halo mass. That is mainly because ofrepeated counting of the 're-accreted' (progenitors passed through and werelater re-accreted to the host more than once) and inclusion of the 'ejected'progenitor population(progenitors were accreted to the host in the past but nolonger members at present day) in previous studies. The typical accretion timefor all progenitors vary strongly with the host halo mass, which is typicalabout $z \sim 5$ for the galactic Aquarius and about $z \sim 3$ for the clustersized Phoenix haloes. Once these progenitors start to orbit their parenthaloes, they rapidly lose their original mass but not their identifiers, morethan $55$ ($50$) percent of them survive to present day for thePhoenix(Aquarius) haloes. At given redshift, survival fraction of the accretedsubhalo is independent of the parent halo mass, whilst the mass-loss of thesubhalo is more efficient in high mass haloes. These systematics results insimilarity and difference in the subhalo population in dark matter haloes ofdifferent masses at present day.

Assembly history of subhalo populations in galactic and cluster sized dark haloes