Probing the CO and methanol snow lines in young protostars - Results from the CALYPSO IRAM-PdBI survey

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Volume 591 (July 2016)

A&A, 591 (2016) A3

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Table 4

Results of elliptical and circular Gaussian fits in the uv plane to the CH₃OH emission integrated over ±3 km s^-1, performed with task uv_fit in MAPPING.

Source	PA	Elliptical fit		Circular fit	Elliptical fit with fixed PA along outflow

		major × minor^a (PA)	Errors	FWHM	Perp. axis	Radius^b	T_dust(r)^c
	(°)	(′′×′′ (°))	(′′×′′ (°))	(′′)	(′′)	(au)	(K)

IRAS4A	0	1.61 × 1.15 (19.9)	0.09 × 0.06 (5.8)	1.30 ± 0.05	1.20 ± 0.06	141 ± 7	70
L1448C	160	0.54 × 0.34 (–38.3)	0.12 × 0.15 ( 26.9)	0.47 ± 0.08	0.37 ± 0.13	47 ± 15	110
IRAS4B^d	0	10.68 × 1.21 (2.4)	0.92 × 0.11 (0.9)	1.77 ± 0.11	1.43 ± 0.13	168 ± 15	40

Notes. The centroid of all fits was fixed to the position of the dust continuum peak.

^(a)

Major and minor axes of the elliptical fits correspond to the respective FWHM.

^(b)

The radius perpendicular to the outflow as derived from the HWHM of the fit with fixed PA along the outflow.

^(c)

The dust temperature at the radius perpendicular to the outflow was determined using the profiles calculated by Kristensen et al. (2012).

^(d)

The uv fits for IRAS4B are strongly affected by outflow contamination and therefore do not reliably trace the central compact methanol emission.

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