Table 8
Comparison between observational results and model predictions.
| Source | Size of | Aver. T | Nc | Trot | Nc | Tex | Nc |
|---|---|---|---|---|---|---|---|
| emission | (model)(*) | model | (obs) | (obs)(**) | (myXClass) | (myXClass) | |
| region | prediction(*) | ||||||
| (model) | |||||||
| [′′] | [K] | [cm−2] | [K] | [cm−2] | [K] | [cm−2] | |
| H2CO | |||||||
| R CrA-IRS 5A | 64.5 | 18(1) | 4(3) × 1013 | 28.1(29) | 4.9(20) × 1013 | 27(7) | 4.2(6) × 1013 |
| NGC 1333-IRAS 2A-1 | 66.6 | 19(1) | 2(1) × 1014 | [132(102) | 2.57(3) × 1013](a) | 69.0(1) | 1.64(1) × 1013 |
| L1551-IRS 5 | 91.8 | 19(1) | 5(3) × 1013 | 19.0(1) | 2.1(2) × 1012 | 17.1(3) | 2.3(3) × 1012 |
| L1544 | 114.3 | 12.5(b) | 5(2) × 1013 | 13.1(1) | 1.8(3) × 1012 | 12(2) | 1.6(3) × 1012 |
| CH3OH | |||||||
| R CrA-IRS 5A | 64.5 | 18(1) | 3(2) × 1013 | 15.7(6) | 6.5(6) × 1013 | 18fixed | 4.6(2) × 1013 |
| NGC 1333-IRAS 2A-1 | 66.6 | 18(1) | 5(1) × 1014 | 69(44) | 8.8(53) × 1013 | 18fixed,(c) | 3.7(1) × 1013 |
| L1551-IRS 5 | 91.8 | 18(1) | 3(2) × 1013 | 3.6(7)(b) | 1.1(10) × 1013(d) | 6.7(1) | 6.1(1) × 1012 |
| L1544 | 114.3 | 12.5(b) | 2(2) × 1013 | 6.5(16) | 2.9(18) × 1013 | 6.5(3) | 2.6(2) × 1013 |
Notes. (*) Recommended model values. The indicated uncertainties are due to age uncertainties of the sources, boundary conditions of the chosen integration limits (rstart and rend), and temperature and density uncertainties of the initial parameters. (**) Column densities are obtained by applying the rotational diagram technique. (a) The rotational diagram made use of the v = 7.34 km s−1 component of the 218.222 GHz line and the 7.5 km s−1 component of the 218.475 and 218.760 GHz lines of H2CO. (b) Value taken from Tafalla et al. (1998). (c)Higher temperatures lead to incorrect results in the 318 GHz spectral range. (d) Two observed lines at 145.097 and 145.103 GHz are used for the rotational diagram analysis, as well as the three non-detected lines (integrated rms level) at 143.865, 145.093, and 146.368 GHz.
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