We present the results of the “ Cosmogrid ” cosmological N -body simulation suites based on the concordance LCDM model .
The Cosmogrid simulation was performed in a 30Mpc box with 2048 ^ { 3 } particles .
The mass of each particle is 1.28 \times 10 ^ { 5 } M _ { \odot } , which is sufficient to resolve ultra-faint dwarfs .
We found that the halo mass function shows good agreement with the \citet Sheth1999 fitting function down to \sim 10 ^ { 7 } M _ { \odot } .
We have analyzed the spherically averaged density profiles of the three most massive halos which are of galaxy group size and contain at least 170 million particles .
The slopes of these density profiles become shallower than -1 at the inner most radius .
We also find a clear correlation of halo concentration with mass .
The mass dependence of the concentration parameter can not be expressed by a single power law , however a simple model based on the Press-Schechter theory gives reasonable agreement with this dependence .
The spin parameter does not show a correlation with the halo mass .
The probability distribution functions for both concentration and spin are well fitted by the log-normal distribution for halos with the masses larger than \sim 10 ^ { 8 } M _ { \odot } .