一酸化炭素（CO）励起状態を含むそのルビブロビロンスペクトル

The spectroscopic nature of CO plays an essential part in astrophysical applications and the radiation transfer process. While existing databases provide high-accuracy data for ground-state infrared transitions, there is a lack of information on the transitions in the vacuum ultraviolet (VUV) region and high-temperature electronic excitations. We present a comprehensive spectroscopic model for CO that explicitly accounts for eight electronic states (X ¹Σ⁺, A ¹Π, I ¹Σ^-, D ¹Δ, a' ³Σ⁺, a ³Π, d ³Δ and e ³Σ^-), incorporating spin-orbit couplings and electronic angular momentum couplings. The potential energy curves (PECs) of the electronic states are reconstructed by combining the Rydberg-Klein-Rees method and ab initio calculations, providing an effective description for the entire internuclear distances. We demonstrate that while the X ¹Σ⁺-X ¹Σ⁺ transition is the primary transition process for transition frequencies below 40 000 cm^-1, the X ¹Σ⁺-A ¹Π system becomes the dominant radiation transition in the VUV region (above 60 000 cm^-1) as temperatures exceed 3000 K, remaining the same up to 8000 K. By extending the spectral coverage, this work enables more spectroscopic characterization and radiative transfer modeling for high-temperature stellar atmospheres and interstellar VUV observations.