We compared the number of faint stars detected in deep survey fields with the current stellar distribution model of the Galaxy and found that the detected number in the H band is significantly smaller than the predicted number .
This indicates that M-dwarfs , the major component , are fewer in the halo and the thick disk .
We used archived data of several surveys in both the north and south field of GOODS ( Great Observatories Origins Deep Survey ) , MODS in GOODS-N , and ERS and CANDELS in GOODS-S .
The number density of M-dwarfs in the halo has to be 20 \pm 13 \% relative to that in the solar vicinity , in order for the detected number of stars fainter than 20.5 mag in the H band to match with the predicted value from the model .
In the thick disk , the number density of M-dwarfs must be reduced ( 52 \pm 13 \% ) or the scale height must be decreased ( \sim 600 pc ) .
Alternatively , overall fractions of the halo and thick disks can be significantly reduced to achieve the same effect , because our sample mainly consists of faint M-dwarfs .
Our results imply that the M-dwarf population in regions distant from the Galactic plane is significantly smaller than previously thought .
We then discussed the implications this has on the suitability of the model predictions for the prediction of non-companion faint stars in direct imaging extrasolar planet surveys by using the best-fit number densities .