# A homogeneous sample of 34 000 M7-M9.5 dwarfs brighter than $J$=17.5 with accurate spectral types

## TL;DR

This study presents a large, homogeneous sample of 33,665 late M dwarfs (spectral types M7-M9.5) with accurate classifications, derived from combined optical and infrared photometry, to better understand their space density and distribution.

## Contribution

The paper introduces a new, highly complete sample of late M dwarfs with precise photometric classifications calibrated against spectroscopic data, enabling improved studies of their luminosity function and Galactic distribution.

## Key findings

- Sample contains 33,665 M7-M9.5 dwarfs with >100 S/N per source.
- Photometric classifications are accurate within 0.5 spectral subtypes.
- Bias in classification affects about 1% of the sample, mainly rare objects.

## Abstract

The space density of late M dwarfs, subtypes M7-M9.5, is not well determined. We applied the photo-type method to $iz$ photometry from the Sloan Digital Sky Survey and $YJHK$ photometry from the UKIRT Infrared Deep Sky Survey, over an effective area of 3070 $deg^{2}$, to produce a new, bright $J$(Vega) < 17.5, homogeneous sample of 33 665 M7-M9.5 dwarfs. The typical S/N of each source summed over the six bands is > 100. Classifications are provided to the nearest half spectral subtype. Through a comparison with the classifications in the BOSS Ultracool Dwarfs (BUD) spectroscopic sample, the typing is shown to be accurately calibrated to the BUD classifications and the precision is better than 0.5 subtypes rms; i.e. the photo-type classifcations are as precise as good spectroscopic classifications. Sources with large $\chi^2$ > 20 include several catalogued late-type subdwarfs. The new sample of late M dwarfs is highly complete, but there is a bias in the classification of rare peculiar blue or red objects. For example, L subdwarfs are misclassified towards earlier types by approximately two spectral subtypes. We estimate that this bias only affects ~1% of the course. Therefore the sample is well suited to measure the luminsoity function and investigate the softening towards the Galactic plane of the exponential variation of density with height.