Indications of M-dwarf Deficits in the Halo and Thick Disk of the Galaxy

TL;DR

This study reveals that M-dwarfs are less prevalent in the Galaxy's halo and thick disk than models predict, based on deep survey data showing fewer faint stars than expected.

Contribution

The paper provides new estimates of M-dwarf densities in the halo and thick disk, challenging existing Galactic models with observational data.

Findings

M-dwarf density in the halo is about 20% of local values.

Thick disk M-dwarf density is approximately 48% of local values.

Implications for star count predictions in exoplanet imaging surveys.

Abstract

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+/-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+/-13%) or the scale height must be decreased (~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.