We study the dark and luminous mass distributions , circular velocity curves ( CVC ) , line-of-sight kinematics , and angular momenta for a sample of 42 cosmological zoom simulations of galaxies with stellar masses from 2.0 \times 10 ^ { 10 } M _ { \odot } ~ { } h ^ { -1 } to 3.4 \times 10 ^ { 11 } M _ { \odot } ~ { } h ^ { -1 } .
Using a temporal smoothing technique , we are able to reach large radii .
We find that : ( i ) The dark matter halo density profiles outside a few kpc follow simple power-law models , with flat dark matter CVCs for lower-mass systems , and rising CVCs for high-mass haloes .
The projected stellar density distributions at large radii can be fitted by Sérsic functions with n \mathrel { \hbox to 0.0 pt { \lower 3.0 pt \hbox { $ \mathchar 536 $ } \hss } \raise 2.0 pt% \hbox { $ \mathchar 318 $ } } 10 , larger than for typical early-type galaxies ( ETG s ) .
( ii ) The massive systems have nearly flat total ( luminous plus dark matter ) CVCs at large radii , while the less massive systems have mildly decreasing CVCs .
The slope of the circular velocity at large radii correlates with circular velocity itself .
( iii ) The dark matter fractions within the projected stellar half mass radius { R _ { e } } are in the range 15 - 30 \% and increase to 40 - 65 \% at 5 { R _ { e } } .
Larger and more massive galaxies have higher dark matter fractions .
The fractions and trends with mass and size are in agreement with observational estimates , even though the stellar-to-total mass ratio is \sim 2-3 times higher than estimated for ETG s. ( iv ) The short axes of simulated galaxies and their host dark matter haloes are well aligned and their short-to-long axis ratios are correlated .
( v ) The stellar root mean square velocity v _ { rms } ( R ) profiles are slowly declining , in agreement with planetary nebulae observations in the outer haloes of most ETG s. ( vi ) The line-of-sight velocity fields { \bar { v } } show that rotation properties at small and large radii are correlated .
Most radial profiles for the cumulative specific angular momentum parameter \lambda ( R ) are nearly flat or slightly rising , with values in [ 0.06 ,~ { } 0.75 ] from 2 { R _ { e } } to 5 { R _ { e } } .
A few cases show local maxima in | { \bar { v } } | / \sigma ( R ) .
These properties agree with observations of ETG s at large radii .
( vii ) Stellar mass , ellipticity at large radii \epsilon ( 5 { R _ { e } } ) , and \lambda ( 5 { R _ { e } } ) are correlated : the more massive systems have less angular momentum and are rounder , as for observed ETG s. ( viii ) More massive galaxies with a large fraction of accreted stars have radially anisotropic velocity distributions outside { R _ { e } } .
Tangential anisotropy is seen only for galaxies with high fraction of in-situ stars .