Abstract
I consider several aspects of the Galactic HI distribution, kinematics, and morphology at R < R 0, in particular; the rotation curve of the inner few kpc; the variation of HI across the inner disks of the Milky Way and other galaxies; the amount of HI inferred in the disk (with implications for the CO-H2 conversion factor); and lastly, the physical disposition of neutral atomic gas and some consequences of the required structure of HI ‘clouds’ for optical and uv absorption-line profile analysis.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
