The paper presents a new library of high-resolution synthetic stellar spectra generated using the PHOENIX stellar atmosphere code. The library covers a wide range of stellar parameters, including effective temperatures from 2300 K to 12000 K, surface gravities from 0.0 to +6.0, metallicities from -4.0 to +1.0, and alpha element abundances from -0.2 to +1.2. The spectra are available at a wavelength range from 500 Å to 5.5 μm with resolutions of $R = 500\,000$ in the optical and near IR, $R = 100\,000$ in the IR, and $\Delta \lambda = 0.1\,\text{Å}$ in the UV. The library is designed to be flexible and can be extended to higher effective temperatures up to 25000 K. The authors describe the methods used to create the model atmospheres and synthetic spectra, including a new self-consistent method for describing micro-turbulence. They also discuss the improvements in the new library compared to previous versions of PHOENIX, particularly in terms of chemical equilibrium and element abundances. The library is available for download and can be used for a wide range of applications, such as spectral analysis and stellar parameter synthesis.The paper presents a new library of high-resolution synthetic stellar spectra generated using the PHOENIX stellar atmosphere code. The library covers a wide range of stellar parameters, including effective temperatures from 2300 K to 12000 K, surface gravities from 0.0 to +6.0, metallicities from -4.0 to +1.0, and alpha element abundances from -0.2 to +1.2. The spectra are available at a wavelength range from 500 Å to 5.5 μm with resolutions of $R = 500\,000$ in the optical and near IR, $R = 100\,000$ in the IR, and $\Delta \lambda = 0.1\,\text{Å}$ in the UV. The library is designed to be flexible and can be extended to higher effective temperatures up to 25000 K. The authors describe the methods used to create the model atmospheres and synthetic spectra, including a new self-consistent method for describing micro-turbulence. They also discuss the improvements in the new library compared to previous versions of PHOENIX, particularly in terms of chemical equilibrium and element abundances. The library is available for download and can be used for a wide range of applications, such as spectral analysis and stellar parameter synthesis.