The paper presents a new set of model atmosphere grids for low-mass stars with effective temperatures ranging from 3000 K to 10000 K. These LTE models are calculated using the PHOENIX code, which includes detailed treatments of atomic and molecular line opacities. The models cover a wide range of metallicities and surface gravities, and are designed to be consistent with the VLMS part of the NextGen grid for stellar evolution calculations and spectral analysis. The LTE models serve as a starting point for a larger grid of NLTE model atmospheres, which will be used for more accurate analysis of cool star spectra. The authors compare their models to the Kurucz 1994 grid and standard stars like Vega and the Sun, demonstrating good agreement for solar-type stars and reasonable agreement for stars up to about 10000 K. They also discuss the importance of NLTE effects, which become significant for effective temperatures above 7000 K, and present detailed NLTE models for Vega to illustrate these effects. The paper concludes by emphasizing the need for NLTE models for higher effective temperatures and the importance of spherical geometry for main sequence stars with effective temperatures above 18000 K.The paper presents a new set of model atmosphere grids for low-mass stars with effective temperatures ranging from 3000 K to 10000 K. These LTE models are calculated using the PHOENIX code, which includes detailed treatments of atomic and molecular line opacities. The models cover a wide range of metallicities and surface gravities, and are designed to be consistent with the VLMS part of the NextGen grid for stellar evolution calculations and spectral analysis. The LTE models serve as a starting point for a larger grid of NLTE model atmospheres, which will be used for more accurate analysis of cool star spectra. The authors compare their models to the Kurucz 1994 grid and standard stars like Vega and the Sun, demonstrating good agreement for solar-type stars and reasonable agreement for stars up to about 10000 K. They also discuss the importance of NLTE effects, which become significant for effective temperatures above 7000 K, and present detailed NLTE models for Vega to illustrate these effects. The paper concludes by emphasizing the need for NLTE models for higher effective temperatures and the importance of spherical geometry for main sequence stars with effective temperatures above 18000 K.