Chemical study of intermediate-mass (IM) Class 0 protostars - CO depletion and N2H+ deuteration

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Volume 518 (July-August 2010)

A&A, 518 (2010) A52

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Table 6:

Model results.
Source	Model	CO Binding energy	$\chi$ $_{\rm C^{18}O}$ ^a	$\chi$ $_{\rm N_2H^+}$	$\chi$ $_{\rm N_2D^+}$
Serpens-FIRS 1	Model 3	1100	4.37	3.89	4.52	only 10% of CO evaporated
	Model 4	1100	2.55	3.77	4.46	only 10% survives for T>100 K
Cep E-mm	Model 1	1100	1.48	4.12	0.71
	Model 2	5000	1.51	0.86	0.45
	Model 3	1100	0.91	2.26	1.19	only 10% of CO evaporated
	Model 4	1100	1.42	2.19	1.12	only 10% survives for T>100 K
IC 1396 N	Model 3	1100	2.95	4.45	>4.3	only 10% of CO evaporated
	Model 4	1100	1.79	4.35	>4.0	only 10% survives for T>100 K
CB3	Model 3	1100	1.63	0.76	0.31	only 10% of CO evaporated
	Model 4	1100	1.24	0.86	0.51	only 10% survives for T>100 K
NGC 7129-FIRS 2	Model 3	1100	0.97	1.29	2.05	only 10% of CO evaporated
	Model 4	1100	1.39	1.48	1.73	only 10% survives for T>100 K

Notes. ^(a) $\chi$ is defined as $\chi = \sqrt[]{[\Sigma (I_{\rm model}-I_{\rm obs})^2]/N}$ . Note that this is an absolute error and the comparison among values in different sources is not
straightforward. See Figs. 11 to 18.

Source LaTeX | All tables | In the text

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