SIMBAD references

In earlier papers (Roshi & Anantharamaiah 2000ApJ...535..231R, 2001ApJ...557..226R), we presented extensive surveys (angular resolution - 2°x2° and 2°x6') of radio recombination lines (RRLs) near 327MHz in the longitude range l=332°->89° using the Ooty Radio Telescope. These surveys have detected carbon lines mostly between l=358°->20° and in a few positions at other longitudes. This paper presents the observed carbon line parameters in the high-resolution survey and a study of the galactic distribution and angular extent of the line emission observed in the surveys. The carbon lines detected in the surveys arise in ``diffuse'' CII regions. The l-v diagram and radial distribution constructed from our carbon line data shows similarity with that obtained from hydrogen recombination lines at 3 cm from HII regions indicating that the distribution of the diffuse CII regions in the inner Galaxy resembles the distribution of the star-forming regions. We estimated the [CII] 158µm emission from diffuse CII regions and find that upto 95% of the total observed [CII] 158µm emission can arise in diffuse CII regions if the temperature of the latter ∼80K. Our high-resolution survey data shows that the carbon line emitting regions have structures on angular scale ∼6'. Analysis of the dual-resolution observations toward a 2° wide field centered at l=13.9° and toward the longitude range l=1.75° to 6.75° shows the presence of narrow (ΔV≤15km/s) carbon line emitting regions extending over several degrees in l and b. The physical size perpendicular to the line-of-sight of an individual diffuse CII region in these directions is >200pc.