In:
Highlights of Astronomy, Cambridge University Press (CUP), Vol. 8 ( 1989), p. 587-588
Abstract:
Identifying the spiral nature of the distribution of gas in the Galaxy has been a subject of much research in the past thirty years. The position of the sun in the disk of the Galaxy presents us with a problem of perspective: how does one identify the cloud system from within the system? Longitude-velocity ( l -v) diagrams have been used to try to determine the distribution of interstellar gas, but problems inherent in the methods have been pointed out previously (Burton 1971). Recent Galactic CO surveys have been used in attempts to map the distribution of molecular cloud complexes in the disk of the Galaxy (Dame, et al . 1986). Here, we use numerical simulations of the molecular cloud system in a spiral galaxy to consider the following question: to what extent can concentrations of emission in the l -v diagram (LVCs) be considered complexes of gas in the disk of the Galaxy (GMCs)?
Type of Medium:
Online Resource
ISSN:
1539-2996
DOI:
10.1017/S1539299600008455
Language:
English
Publisher:
Cambridge University Press (CUP)
Publication Date:
1989
