Issue |
Astron. Astrophys. Suppl. Ser.
Volume 120, Number 1, November II 1996
|
|
---|---|---|
Page(s) | 41 - 56 | |
DOI | https://doi.org/10.1051/aas:1996273 | |
Published online | 15 November 1996 |
Deep H
survey of the Milky Way.
III. The l = 338 area
*
1
Observatoire de Marseille, 2 Place Le Verrier, F-13248 Marseille Cedex 04, France
2
Observatorio Astronómico de Córdoba, Laprida 854, 5000 Córdoba, Argentina
3
Observatoire de Grenoble BP. 53X Grenoble Cedex, France
Send offprint request to: Y.M. Georgelin
Received:
9
February
1996
Accepted:
5
April
1996
The Galactic plane has been observed between l =
337 and l = 342 in the frame of an Hα
Survey of the Southern Milky Way. This area is known to be rich
in radio sources but poor in Hα emission. The analysis
of high resolution profiles of the Hα emission observed
in this direction nevertheless enabled to distinguish 6
different velocity components: 2 faint layers of diffuse ionized
hydrogen at 0 and -12 km (VLSR), 2 brighter
layers at -28 and -39 km
including individual HII
regions, a faint patch at -50 km
and two isolated
bright HII regions at -61 km
. Combining these
Hα observations with stellar and radio data we conclude
about the most probable distances for the different components.
Key words: interstellar medium: HII regions / Galaxy: structure
© European Southern Observatory (ESO), 1996