The Outer Disks of Spiral Galaxies
BRAINE, J.
Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
Observatoire aquitain des sciences de l'univers [OASU]
Laboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
Observatoire aquitain des sciences de l'univers [OASU]
Laboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
BRAINE, J.
Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
Observatoire aquitain des sciences de l'univers [OASU]
Laboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
< Reduce
Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
Observatoire aquitain des sciences de l'univers [OASU]
Laboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
Language
en
Communication dans un congrès
This item was published in
Astrophysics and Space Science Proceedings 2008, Astrophysics and Space Science Proceedings 2008, 2008, Okinawa. 2008p. 212
English Abstract
Molecular gas, via its CO emisssion, is detectable far out in the Milky Way, M33, NGC 4414, and probably all spirals with extended HI. Metallicity is not a great problem for CO detection in regions with a weak radiation ...Read more >
Molecular gas, via its CO emisssion, is detectable far out in the Milky Way, M33, NGC 4414, and probably all spirals with extended HI. Metallicity is not a great problem for CO detection in regions with a weak radiation field, such as outer disks. The association with HI and star formation is very good but not perfect ?giant molecular clouds can be found in zones with little HI. In the outer Galaxy, there is no sharp decrease in CO line intensity despite the lack of obvious heating sources for outer galaxy clouds.Read less <
Origin
Hal imported