include a 2D spectrum associated with a 1D spectrum. However, the optimal extraction of the 1D spectrum not being yet implemented in the version 2.8.0 of the pipeline, we extracted the UVB, VIS, and NIR spectra with the task under IRAF [@tody86; @tody93]. We note that most of the targets have little flux in the UVB arm, resulting in low signal-to-noise ratio below 550nm and very little flux (or no flux) below 400nm. We corrected the VIS and NIR spectra for telluric bands/lines with the package distributed by ESO [@kausch15; @smette15][^3] mainly because the telluric standards were not necessarily taken at the same airmass as our targets. The regions corrected are: 625–632, 686–696, 716–732, 758–770, 812–834, 893–920, 928–980nm in the VIS arm and 1105–1220, 1253–1280, 1310–1510, 1730–1995, 2000–2035, 2045–2085, 2200–2470nm in the NIR arm.

The final spectral energy distributions (SEDs) of sdM, esdM, and usdM are displayed in figures in Appendix \[MplusTeff\_sdM:appendix\_model\_fits\]. For display purposes, we shifted the observed spectra to the BT-Settl models because of the large velocities of our subdwarfs taking into account that the wavelength scale of models is in vacuum and the observed spectra in the air system (see Section \[MplusTeff\_sdM:Comparison\]). Our sample increases by a 