3D physico-chemical model of a pre-stellar core - I. Environmental and structural impact on the distribution of CH3OH and c-C3H2

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Table 4

Overview of the modeled spectra for c-C₃H₂ and CH₃OH shown in Figs. 11 and 12.

		c-C₃H₂			CH₃OH
Model	T_peak (K)	dv (km s⁻¹)	W (K km⁻¹)	T_peak (K)	dv (km s⁻¹)	W (K km^−l)
L1544	0.21	0.47	0.10	0.84	0.33	0.30
I0.0_Ml.0_standard	0.57	0.39	0.23	0.09	0.45	0.04
I0.0_M0.5_standard	1.16	0.44	0.55	0.33	0.44	0.15
I0.5_M0.2_standard	1.16	0.44	0.55	0.33	0.42	0.15
I0.5_M0.5_standard	1.26	0.41	0.56	0.13	0.48	0.07
Il.0_M0.l_standard	0.14	0.39	0.06	2.4	0.41	1.06
I0.0_M1.0_κ × 0.2	0.20	0.40	0.08	0.02	0.38	0.01
I0.0_Ml.0_Gnotl00	0.05	0.43	0.02	–	–	–
I0.0_Ml.0_CRl0	0.36	0.41	0.16	1.16	0.40	0.49
I0.0_Ml.0_extAv0	0.45	0.38	0.18	0.05	0.45	0.03

Notes. The columns list the peak brightness, the FWHM, and the area of the emission lines. All spectra are extracted toward the dust peak and fitted with Gaussian profiles. Parameters for a Gaussian fit to the observed spectra toward L1544 are included in the top row.

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