| AraOB1 Background Info Page Some notes on the AraOB1 region, references to previous studies etc. | ||
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On this page: MSX maps 13CO maps 13CO spectra Arnal et al (12CO) comparison Yamaguchi et al (13CO) comparison General Comments Literature Miscellaneous
MSX A (8um) map ![]() MSX E (21um) map - same FoV as previous image. The two MSX E sources of interest are the point sources at (336.55,-1.81) and (336.53,-1.74) (i.e. below the bright red blob). ![]() Integrated 13CO map, overlaid with MSX A contours (red) ![]() Integrated 13CO map, overlaid with MSX E contours (red) ![]() Close-up integrated 13CO map, overlaid with MSX A (red) + E (black) contours ![]() Integrated 13CO - profile positions (see below) ![]() 13CO spectra - cuts 1 to 9 ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() 13CO spectra coincident with 2 MSX E sources a) southern source b) northern source ![]() ![]() Integrated 13CO + Arnal's 12CO Peaks (green crosses) ![]() Integrated 13CO + Arnal's IRAS YSO candidates (green crosses) IRAS point sources that fulfil Arnal et al's YSO criteria and are spatially coincident with their molecular clouds. ![]() Integrated 13CO + Yamaguchi's 13CO Peaks (green crosses) ![]() Integrated 13CO + Yamaguchi's IRAS YSO candidates (green crosses) IRAS point sources that fulfil Yamaghuchi et al's YSO criteria and are spatially coincident with their molecular clouds. ![]() General Comments
Most previous studies have focussed on the star-forming activity
in i) RCW108/NGC6193 or ii) the embedded cluster
SFO79/RCW108-IR/IRAS16362-4845. With the exception of Arnal et al. (2003, 1987)
and Rizzo and Bajaja (1994), there has been little discussion of the
extended molecular gas distribution in Ara, or about the relationship between
the molecular/atomic/ionized gas phases in this region. A bibliographic reference and
one-line summary of previous observational studies is listed below (in
chronological order).
No masers.
CO emission confined to velocity range [-23,-13] km/s. There is a general
velocity gradient across the cloud: the SW is at more positive velocities than
the NE. But there is significant emission across this whole velocity range in the NE region. Literature
Misc Surveys, Online data etc.
Last modified 10 July 2006 |