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instruments. Together, radiative transfer modelling, these data sets
and future interferometric
observations with ALMA will be able to fully characterize the physical
and chemical structure of the earliest, deeply embedded stages of star
formation.
| Source | Ratiob |
 (Blue)
|
Ratiob |
(Red)
|
| K | K | |||
| RCrA IRS 7 | 1 | >200 | 2.5 | 160 |
| NGC 1333 IRAS 2 | - | - | - | - |
| L 1551 IRS 5c | >8 | <50 | 9 | 40 |
| TMR 1d | 1.5 | 180 | >4 | 120 |
| IRAS 12496-7650 | >8 | <65 | - | - |
| HH 46e | 6 | 100 | 3 | 140 |
| BHR 71 | - | - | - | - |
| Ced 110 IRS 4 | 3 | 140 | >7 | <80 |
a Estimated with an ambient density of 104 cm-3. b CO 3-2/6-5 line wing ratio. Ratios are averaged over velocity and distance from the source. See van Kempen et al. (2009) for more discussion. c CO 4-3/6-5 ratio. d Optical depth of 8 inferred for 12CO 3-2 wings (Hogerheijde et al. 1998). e See van Kempen et al. (2009).
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