Physical structure and water line spectrum predictions of the intermediate mass protostar OMC2-FIR4

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Volume 506 / No 3 (November II 2009)

A&A, 506 3 (2009) 1229-1241

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Table 6:

The brightest lines predicted by models 1 and 6 (the model with the largest water abundance) compared with the upper limits derived by the ISO observations.)
		Model 1	Model 6	ISO
Wavelength	Transition	Intensity	Intensity	Instrument	Upper limit (3 $\sigma$ )
( $\mu$ m)	$J_{K_- K_+} \rightarrow$ J'_{K'_- K'₊}	(erg s^-1 cm^-2)	(erg s^-1 cm^-2)		(erg s^-1 cm^-2)
ortho
75.4957	8 $_{5 4} \rightarrow$ 8_{4 5}	2.6E-20	1.9E-19	LWS04	9.78e-12
108.073	2 $_{ 2 1} \rightarrow$ 1_{1 0}	1.3E-12	1.5E-12	LWS04	2.21e-12
179.527	2 $_{ 1 2} \rightarrow$ 1_{0 1}	1.2E-12	7.0E-12	LWS04	2.56e-11
113.538	4 $_{ 1 4} \rightarrow$ 3_{0 3}	8.3E-13	8.7E-13	LWS01	1.2e-11
para
100.983	2 $_{ 2 0} \rightarrow$ 1_{1 1}	7.3E-13	9.1E-13	LWS01	8.37e-12
138.527	3 $_{ 1 3} \rightarrow$ 2_{0 2}	7.3E-13	7.3E-13	LWS01	4.14e-12
156.197	3 $_{2 2} \rightarrow$ 3_{1 3}	2.2E-13	3.4E-13	LWS01	1.60e-12

Source LaTeX | All tables | In the text

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