A new comprehensive CO survey of the entire Milky Way has been created by combining data from multiple surveys conducted over two decades using two small millimeter-wave telescopes. The survey includes 488,000 spectra, sampled at a resolution of 1/8° (approximately 1/4°) in latitude and 1/4° in higher latitudes, providing high angular resolution and sensitivity. Compared to previous surveys, this new survey has 16 times more spectra, up to 3.4 times higher angular resolution, and up to 10 times higher sensitivity per unit solid angle. The composite maps reveal detailed information on molecular clouds, suggest relationships between clouds and distant regions, and display the main structural features of the molecular Galaxy. The survey also provides precise kinematic information that will be crucial for many large-scale Galactic studies. The survey was calibrated using a map of molecular column density predicted from far-infrared and 21 cm surveys, showing that only about 2% of the total CO emission at |b| < 32° lies outside the current sampling. The mean molecular column density decreases from ~3×10²⁰ cm⁻² at |b| = 5° to ~0.1×10²⁰ cm⁻² at |b| = 30°, a drop steeper than expected from a plane-parallel layer but consistent with recent measurements. The ratio of the predicted molecular column density map to the observed CO intensity map provides a calibration of the CO-to-H₂ mass conversion factor X. The value of X is consistent across the solar neighborhood, with a mean value of 1.8 ± 0.3 × 10²⁰ cm⁻² K⁻¹ km⁻¹ s⁻¹. The survey covers 45% of the sky within 30° of the Galactic equator, and is likely nearly complete for clouds larger than a few degrees on the sky. The survey includes data from various regions, such as the Taurus and Orion clouds, the λ Orionis ring, and the second quadrant. The composite maps provide a detailed view of the molecular structure of the Galaxy, including the distribution and kinematics of molecular clouds, and reveal large-scale structural features. The survey also shows that the molecular gas is distributed in a complex pattern, with a molecular ring and several spiral arms. The survey highlights the importance of molecular clouds in star formation and the role of CO in studying the interstellar medium. The survey also provides insights into the kinematics of the local molecular gas, including evidence of supershells and the association of local molecular clouds with Gould's Belt. The survey is a valuable resource for understanding the structure and evolution of the Milky Way.A new comprehensive CO survey of the entire Milky Way has been created by combining data from multiple surveys conducted over two decades using two small millimeter-wave telescopes. The survey includes 488,000 spectra, sampled at a resolution of 1/8° (approximately 1/4°) in latitude and 1/4° in higher latitudes, providing high angular resolution and sensitivity. Compared to previous surveys, this new survey has 16 times more spectra, up to 3.4 times higher angular resolution, and up to 10 times higher sensitivity per unit solid angle. The composite maps reveal detailed information on molecular clouds, suggest relationships between clouds and distant regions, and display the main structural features of the molecular Galaxy. The survey also provides precise kinematic information that will be crucial for many large-scale Galactic studies. The survey was calibrated using a map of molecular column density predicted from far-infrared and 21 cm surveys, showing that only about 2% of the total CO emission at |b| < 32° lies outside the current sampling. The mean molecular column density decreases from ~3×10²⁰ cm⁻² at |b| = 5° to ~0.1×10²⁰ cm⁻² at |b| = 30°, a drop steeper than expected from a plane-parallel layer but consistent with recent measurements. The ratio of the predicted molecular column density map to the observed CO intensity map provides a calibration of the CO-to-H₂ mass conversion factor X. The value of X is consistent across the solar neighborhood, with a mean value of 1.8 ± 0.3 × 10²⁰ cm⁻² K⁻¹ km⁻¹ s⁻¹. The survey covers 45% of the sky within 30° of the Galactic equator, and is likely nearly complete for clouds larger than a few degrees on the sky. The survey includes data from various regions, such as the Taurus and Orion clouds, the λ Orionis ring, and the second quadrant. The composite maps provide a detailed view of the molecular structure of the Galaxy, including the distribution and kinematics of molecular clouds, and reveal large-scale structural features. The survey also shows that the molecular gas is distributed in a complex pattern, with a molecular ring and several spiral arms. The survey highlights the importance of molecular clouds in star formation and the role of CO in studying the interstellar medium. The survey also provides insights into the kinematics of the local molecular gas, including evidence of supershells and the association of local molecular clouds with Gould's Belt. The survey is a valuable resource for understanding the structure and evolution of the Milky Way.